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^
THE NEWYORK
PUBLIC UBRARY
A8T0R, LENOX AND
TILDE N FOUNDATIONS.
PHOTOGRAPH OF THE SOLAR SURFACE
Lick Observatory, October 19, 1896.
Sun's diameter about 44 Inches.
1M;'W.M .\ r;
M \ / I ' ' I ■' ' ^ !
VJ,;
J !
i i
r^P -. ">: AH i^'jr;r.;.CE
PUBLICATIONS
OF THE
ASTRONOMICAL SOCIETY
OF THE PACIFIC.
VOLUME IX.
1897.
SAN FRANCISCO
PRINTED FOR THE SOCIETY.
1897.
THENEW YORK
PUBLIC LIBRARY
A6TOR, LENOX AND
TILDEN FOUNDATIONS.
R 1901 L.
TABLE OF CONTENTS.*
Publications No. 54, February i, 1897.
Page
Photograph of the Solar Surface Frontispiece
List of Members of the Society, January I, 1897 . » i
List of Corresponding Institutions 12
Exchanges 13
For Review 14
On the Influence of Carbonic Acid in the Air upon the Temperature
of the Earth, by Professor S. Arrehnxus; abstract by Dr,
Edward S. Holden 14
Planetary Phenomena for March and April, 1897, by Professor Mal-
colm McNeill 24
Abjuratio Galilei 30
The Washburn Observatory, by George C. Comstock, Director 31
Some Luminous Appearances in the Sky, by W. H. S. Monck . • 33
Twenty-sixth Award of the Donohoe Comet-Medal to Mr. C. D.
Perrinb 36
Elements and Ephemeris of Comet g^ 1896, by F. H. Seares and
R. T. Crawford . 36
List of Earthquakes in California for the year 1896, by C. D. Perrine 37
Twenty-seventh Award of the Donohoe Comet-Medal to Mr. C. D.
Perrine 38
Notices from the Lick Observatory 39
Photograph of the Solar Surface made at the Lick Observatory.
E. S. H 39
Discovery of Comet ^, 1896 (Perrine). C. D. P 39
Astronomische Geselischaft Zone — 9° ^c/ to — 14** 10^. A. S. 40
Relief-Map of the Lick Observatory Reservation. E. S. H. . 40
Meteors (November 15, 1896). Letter of Mrs. F. K. Upham . 41
Observation of the Leonid Meteors. Letter of Mr. William
Yates 41
Notice to Members of the Society. E. S. H 41
The Great Sun-Spot of January, 1897 . , , , cuts to face page 42
The Great Sun-Spot of January, 1897. A. L. C 42
The Great Sun-Spot of January, 1897. R. G. A 43
The Heliocentric Theory and the University of Cambridge in
1669. (Extract.) 43
Honor Conferred on Professor Barnard 44
Prices of Reflecting Telescopes 44
A Brilliant Meteor. (Extract. Wm. S. Moses.) 44
* To the Binder; this should precede page i, Volume IX.
iv Publications of the
Page
List of American Foreign Associates of the Royal Astronom-
ical Society 45
List of Americans who have received the Medal of The Royal
Astronomical Society 45
Earthquake at Oakland, January 17, 1897. A. H. B. 45
Elliptic Elements of Comet g, 1896 (Perrine). W. J. H. and
C. D. P 46
Observations of the Companion to Procyon, and of the Com-
panion to Sirius, J. M. S 46
Honor Conferred on Dr. Lewis Swift 47
The Ladd Observatory (Providence, R. L) 47
Measures of the Companion to Ptocyon. R. G. A 47
Erratum in PubHcations A. S. P., No. 53. C. A. Y 47
Astronomical Telegrams. Discovery of Comet ^, 1896 .. . 47
Astronomical Telegram. Observation of Same, December,
9. 1896 47
Astronomical Telegram. Observation of Same, December,
10, 1896 48
Astronomical Telegram. Elements of Same, December 11.
1896 48
Astronomical Telegram. Lowell. Martian North Polar Cap 48
Astronomical Telegram. Elements of Comet g, 1896 .... 48
Astronomical Telegram. Chandler. Comet g, 1896 ... 48
Minutes of the Meeting of the Directors^ January 30, i8gy .... 49
Minutes of the Meeting of the Society^ January 30, iSgy 50
Officers of the Society, etc 51
Publications No. 55, April i, 1897.
Astronomy and Astronomers in Their Relations to the Public.
Address of the Retiring President, by W. J. Hussev 53
Astronomical Observations in 1896, by Torvald Kohl . .... 65
Planetary Phenomena for May and June, 1897, by Professor Mal-
colm McNeill 70
Ephemeris for Physical Observations of the Moon for Certain Dates
between 1890 and 1896, by Dr. A. Marth, F. R. A. S. . , . . . 76
Review of Solar Observations, 1895 (August-December) and 1896,
by David E. Haddbn 77
Predictions for the Solar Eclipse of July 29, 1897, Lick Observatory
and San Francisco, by C. D. Perrine 85
Maximum of o Ceti (Mira), 1896-97, by Miss O'Halloran .... 86
Portrait of W. C. Bond to face page 89
Notices from the Lick Obserx'aiory 89
Photographs of Donati's Comet in September, 1858. E. S. H. 89
Search for Comets Reported by Dr. Swift, September 20th.
W. J. H 89
Bright Fireball, January 26, 1897 (Mt. Hamilton). C. D. P. . 90
The Metric System 90
Erratum in No. 53 of the Publications A. S. P 90
Astronomical Society of the Pacific. v
?AGE
HoSn6 Wronski. E. S. H 90
Portrait of William Cranch Bond. E. S. H 91
Meteor of January 24. 1897 (Los Angeles). Letter of S. J. Reese 91
Mr. Lowell's Observations of Mercury and Ventts, E. S. H. 92
Measures of ^ Delphini, ^ 151. R. G. A 93
First Results from the Bruce Photographic Telescope at
Arequipa. E. S. H 93
Elements of Descriptive Astronomy: a Text-book. By Dr.
Herbert A. Howe. Review by E. S. H 94
Portraits of Astronomers and Others Belonging to the Lick
Observatory. E. S. H 95
Light Absorption as a Determining Factor in the Selection
of the Size of the Objective of the Potsdam Observatory.
R. G. A 98
Awards of the Comet-Medal of the Astronomical Society of
the Pacific 99
Memorials of William Cranch Bond, and of His Son, George
Phillips Bond, by Edward S. Holden. E. S. H 100
The Reversing-Layer of the Sun's Corona (Total Solar Eclipse
of 1896. August 9). E. S. H 100
Gift of Miss Bruce to the Observatory of Prague 10 1
Measures of Sirius, R. G. A loi
Latitude of the Lick Observatory. R. H. T loi
The International Astrographic Charts 102
Weather at Mt. Hamilton in the Winter of 1896-97. R. G. A. 103
The Companion of Sirius, Observed at Glasgow, Mo., with a
Twelve-inch Telescope. (Extract of a Letter from H. S. P.) 104
The Bruce Medal of the Astronomical Society of the Pacific , 104
Return of the Lowell Observatory to Arizona 105
The Cape Photographic Durchmusterung 105
International Catalogue of Fundamental Stars 106
Probable Error of a Single Observed Position in Some Fre-
quently Used Catalogues and Collections of Stars. E. S. H. 107
Addendum to Dr. Marth's Article on Page 76 ...... . 108
Notice to Members. The Committee on Publication 108
Recent Observations of the Spectrum of Mars, by W.W. Camp-
bell. Abstract from S. F. Chronicle 109
Minutes of the Meeting of the Directors, March 27, iSgj . ... 113
Report of the Library Committee 113
Minutes of the Annual Meeting^ of the Society, March 27, iSgj . 114
Report of the Committee on the Comet-Medal, March 27, 1897 1 15
Report of the Treasurer, March 27, 1897 116
Minutes of the Meeting of the Directors, March 27, 1897 • • . . 118
Officers of the Society, etc 119
vi Publications of the
Publications No. 56, June i, August i, 1897.
Pack
A New Observatory (Valkenburg, Holland), by Rev. John G.
Hagen, S. J 121
The Spectra and Proper Motion of Stars, by W. H. S. Monck,
F. R. A. S 123
Supplemental Note to the Same, by W. H. S. Monck .... 128
The Sayre Observatory, South Bethlehem, Penn., by C. L. Doo-
LiTTLE 130
Total Solar Eclipse, January 22, 1898. English Preparations, by
Edward W. Maunder, F. R. A. S 131
Earthquake of June 20, 1897 (Oakland), by Allen H. Babcock . 135
Earthquake of June 20, 1897 (Fresno County), by S. C. Lillis. . 135
Planetary Phenomena for July and August, 1897. By Professor
Malcolm McNeill 136
Double Star Measures, by D. A. Lehman 141
Photograph of the Moon, Paris Observatory, March 14, 1894
cut to face page 145
Notices from the Lick Observatory 145
A New Celestial Atlas. Notice by E. S. H. . . 145
Meteor Seen at Mt. Hamilton (May 5, 1897). J. M. S 146
Photographic Equatorial of the Moscow Observatory ....
cut to face page 147
Stability of the Great Equatorial. E. S. H 147
Measures of Procyon. W. J. H . 147
Reflector and Portrait Lens in Celestial Photography. Abstract
of an Article by Professor Max Wolf. E. S. H 147
Dedication of the Flower Observatory, University of Penn-
sylvania 148
• Record of Experiments with the Moving Floor of the 75-foot
Dome of the Lick Observatory. E. S. H 148
Eye-End of the 30-inch Equatorial of the Pulkowa Observatory
cut to face page 149
Statistics of the Library of the Lick Observatory. R. G. A. . 150
Apparatus for Measuring Photographic Plates (Repsold)
cut to face page 151
Post-office at Mt. Hamilton. E. S. H 151
Appointment of Professor Robert G. Aitken as Assistant
Astronomer at the Lick Observatory. E. S. H 151
Graduate Students in Astronomy at the Lick Observatory
(1897) 151
Instruments Making in Allegheny 151
Death of Alvan G. Clark. E. S. H 152
Royal Observatory, Greenwich, 1896-97. Extract from the
London Times^ June 7, 1897 152
Expedition from the Lick Observatory to Observe the Eclipse
of January, 1898, in India. E. S. H 155
Astronomical Telegram. Discovery of D' Arrest's Comet . 155
Photographic Atlas of the Moon. (Extracts from a Circular.)
By Dr. L. Weinek 156
Astronomical Society of the Pacific. vii
Page
Trial of the Crossley Reflector. E. S. H 159
Death of Hon. Charles Frederick Crocker. £. S. H. . . 160
Small Telescope for Sale. E. S. H 160
Appointments in the Lick Observatory. E. S. H 160
Meeting of the Directors and of the Society, June 12, iSgy . . . 160
Officers of the Society, etc 161
Publications No. 57, September i, 1897.
By-Laws of the Astronomical Society of the Pacific 163
Statutes for the Bestowal of the Bruce Medal of the Astronomical
the Society of the Pacific • 165
Rules Relating to the Comet-Medal of the Astronomical Society of
the Pacific 170
Officers of the Society 171
Publications No. 58, October i, 1897.
Photographs of Jupiter (taken with the Schaebbrle Reflector)
to face page 173
Photographs of yi//«/^, by J. M. Schaeberle 173
Planetary Phenomena for September, October, November, and
December, 1897, by Professor Malcolm McNeill 174
The Bruce Photometers of the Lick Observatory, by R. G. Aitken 184
Catalogue No. II, of Nebulae Discovered at the Lows Observatory,
Echo Mountain, Cal., by Lewis Swift 186
Eclipse of the Sun, July 29. 1897, by David E. Hadden 188
Notes on the Total Eclipse of the Sun, January 21-22, 1898, in
India, by Colonel A. Burton-Brown. R. A., F. R. A. S 189
The Cause of Gravitation, by V. Wellman 190
Notices from the Lick Observatory 195
Observation of the Partial Solar Eclipse, July 29, 1897. R. G. A. 195
Unusual Lunar Halo, August 5, 1897. (Extract.) Kate Ames 195
The Work of the Lick Observatory. E. S. H 196
Inventory, etc., of Lick Observatory Buildings and Equipment,
June 30, 1897. E. S. H 201
Cost of the Library of the Lick Observatory, 1875-1897.
E. S. H 201
Lick Observatory Moon- Atlas. E. S. H 202
Albert Marth; bom 1828; died 1897. E. S. H 202
Resignation oC Mr. Colton. E. S. H 203
A New Celestial Atlas. E. S. H 203
Portraits of Astronomers and Others Belonging to the Lick
Observatory. (Addenda.) 204
Minutes of a Special Meeting of the DirectorSy August 14^ i8gj 205
Minutes of the Meeting of the Directors and of the Society , Septetnber
4, 18^ 206
Minutes of a Special Meeting of the Directors, September 18, 1897 207
Officers of the Society, etc • 208
viii Publications of the Astronomical Society dfc.
Publications No. 59, December i, 1897.
Page
The Yerkes Observatory Frontispiece
The Yerkes Observatoty, by W. J. Hussey 209
Catalogues Nos. Ill and IV, of Nebulae Discovered at the Lowe
Observatory, Echo Mountain, Cal., by Lewis Swift 223
Planetary Phenomena for January and February, 1898, by Professor
Malcolm McNeill 226
Comet b, 1897, by C. D. Perrine 232
Comet b^ 1897, by R. Tracy Crawford 234
Notices from the Lick Observatory 235
Letter of Resignation of Professor Holden as Director of the
Lick Observatory. E. S. Holden 235
List of Recorded Earthquakes on the Pacific Coast, 1 769-1897,
by Edward S. Holden. E. S. H 238
Measures of the Companion of Sirius, and of ^ 883.
R. G. AiTKEN 238
The Leonids in 1897. C. D. P 239
Comets Due to Return in 1898. C. D. P 239
Photograph of the Spectrum of a Meteor. R. G. A 240
Dimensions of the Planets and Satellites. R. G. A 241
Changes in the U. S. Coast and Geodetic Survey 241
The Telegraphic Longitude Net of the United States .... 242
Observations of the Companion to Procyon, J. M. S 244
Lick Observatory Eclipse Expedition. C. D. P 244
The Chabot Observatory Eclipse Expedition. A. H. B. . . . 245
Elements of Comet b, 1897. W. J. H. and R. G. A. . . . . 246
Astronomical Telegrams on Comet ^, 1897 246
Minutes of the Meeting of the Directors^ November ^7, iSgj . . . 248
Minutes of the Meeting of the Society, November 27, iSgy 249
Officers of the Society, etc 250
General Index 251
ABTORi LENCX AND
TlLDEN FOUNPATlONd,
PUBLICATIONS
OF THE
Astronomical Society of the Pacific.
Vol. IX. San Francisco, California, February i, 1897. No. 54.
LIST OF MEMBERS
OF THE
ASTROiNOMICAL SOCIETY OF THE PACIFIC.
January i, 1897.
OFFICERS OF THE SOCIETY.
W. J. HussKY (Lick Observatory), President
E. J. MoLBRA (606 Clay Street. S. F.) »
E. S. HoLDBN (Lick Observatory), [ Vice-Presidents
O. VON Gbldrrn (819 Market Street, S. F.) )
C. D. Pbkrinb (Lick Observatory!. Secretary
F. R. ZiKL (410 California Street. S. F.). Secretary and Treasurer
Board 0/ Directors — .Messrs. Edwards. Holden. Hussev, Moleka, Miss O'Hallokan.
Messrs. Pardee, Perrinb, Pibrsun, Stringham, von Gbluekn, Ziel.
Finance Committee — .Messrs. von Gbldbrn, Pibrson, Stringham.
ComMittee on Publication — Messrs. Holdbn, Babcock, Aitken.
Library Committee— yi\%% 0*Hallx>ran, Messrs. Molera, Burckhalter.
Committee OH the Comet-Afeda/^Mcisrs. Holden (ex-o^cio), Schaeberle, Campbell.
OFFICERS OF THE CHICAGO SECTION.
Executive Committee — Mr. Ruthvbn W. Pike.
OFFICERS OF THE MEXICAN SECTION.
Executive Committee— }At»tTS* Camilo Gonzalez, Francisco Rodriguez Rev.
LIST OF MEMBERS.*
Mr. Carl H. Abbott 118 nth St., Oakland, Cal.
Mr. Charles L. Ackerman 426 California St., S. F., Cal.
Prof. R. G. Aitken { ^'['on °Ca™""^'' '^''' "^""'"
Mr. J. H. Albert Salem, Oregon.
Prof. W. Steadman Alois* { "^nd.^' Abckland, New Zea-
Prof. VV. D. Alexander Honolulu, Hawaiian Islands.
Mr. Richard H. Allen* Chatham, Morris Co., N. J.
♦A star si^ifies Life-Membership. Total membership, 570 (67 life-members).
2 Publications qf the
Mr. Charles Altschul { ^^BaliT' S^^^^^ American
Hon. Henry B. Alvord* San [os^, Cal.
Hon. William Alvord* 2200 Broadway, S. F., Cal.
Mrs. William Alvord* 2200 Broadway, S. F., Cal.
Mr. W. S. Andrews Schenectady, N. Y.
Mr. F. S. Archenhold \ Obseryatorium,Grunewald.bei
\ Berlin, Germany.
Mrs. Wm. Ashburner 1014 Pine St., S. F., Cal.
Mr. J. J. Aubertin* jas Duke St St James, S. W.,
-' -' \ London, England.
Mr. Allen H. Babcock i2i4WebsterSt., Oakland,CaI.
Mr. N. A. Baldwin New Haven, Conn.
Mr. T. R. Bannerman 2407 Howard St.. S. F., Cal.
Dr. G. Barroeta San Luis Potosi, Mexico.
Mr. J. Bassett / 82 High St Stoke Newingion,
^ I N., England.
Dr. Henry H. Bates \^^^ ^Portland, Washington,
Miss Frances L. Beans 489 N. First St., San Jos^, Cal.
Mr. Henry Berger | Observatory Hill, Allegheny,
Mr. E. F. BiGELow i 5 Waverly Avenue, Portland,
{ Conn.
Prof. Frank H. Bigelow | U, S Weather Bureau. Wash-
t mgton, U. L.
Mr. WiLBERT M. BiRGE Davenport, Neb.
Mr. R. L. BiscHOFFSHEiM* 3 Rue Taitbout, Paris, France.
Mr. Anson Stiles Blake Berkeley, Cal.
Mr. Charles T. Blake Berkeley, Cal.
Mr. Henry Lord Boulton, Jr.* . . . i ^^J^^^'w ^T^"A v ^"""^
* •' t 2015, New York, N. Y.
Dr 1 T Boyd -^ ^6 E. Ohio St., Indianapolis,
■ -'* * i Ind.
Colonel E. D. Boyle Gold Hill, Storey Co., Nev.
Mr. J. A. Brashear Allegheny City, Pa.
Rev. M. S. Brennan { ^oufs"^ Mo?^'^ ^^"'"''*'' ^^*
Rev. A. L. Brewer San Mateo, Cal.
Mr. Edward M. Brewer 27 Kilby St., Boston, Mass.
{Hope Bank, Nelson St.. Wool-
lahra,via Sydney, New South
Wales.
Co..A.HX.Bu.xo..B«ow..R.A..P.R.A.s.|St^Oeo^.e-s^a^^
Miss E. Brown* {^England*"'"'' ^''■^"''^'^'■•
Dr. William Andrews Browne . . . Newton, Mass.
Dr. J. D. Brownlee 754 S. 3d St., San Jos^, Cal.
Miss C. W. Bruce* 810 5th Ave., New York, N. Y.
Mr. Charles Burckhalter, f. r. a.s. {C™'^^,^^''^^^^^*"''^' O*"^"
Astronomical Society of the Pcuific. 3
Miss MAKV E. BVRO {'^^V^&Trpfon.'Ma^s^;-
Dr. J. Callandrkau* 1 114 ^Montgomery St., S. F..
Prof. W. W. Campbell J Lick Observatory. Mt. Hatnil-
( ton. ual.
Mr. Andrew Carnegie* 5 WestsistSt.NewYork.N.Y.
Mr. J. C. Cebrian* {^'cfal^"'' ^"^^'^ ^^" ^' ^"
Dr. V. Cerulli | Observatorio Privato, Teramo.
Mrs. EMBUE M. Chabot { ^'SakYa'd'cal.'^''""" ^'"•
Miss JOS.H Chabot { '^'SakValld.'^l.''''"''" ^''•'
Rev. E. Bentley Church 1036 Valencia St., S. F., Cal.
Mr. B. G. Clapp The Academy, Fulton, N. Y.
Dr. E. S. Clark 16 Geary St., S. F., Cal.
Mis-s Isabella D. Clark San Jos^, Cal.
Mr. Mateo Clark* j '^En?S.'^ ^^^^' ^''"'^''"'
Miss Agnes M. Clerke j ^£^^2^ ^"^'^' ^^"^°"'
Mr. Ernest A. Cleveland Vancouver, B. C.
Mr. C. H. CoLBURN Virginia City, Nevada.
Mr. Arthur T. Collins Swarthmore, Delaware Co., Pa.
Mr. A. I. Colton* ] H^^^ ^r^!f '^^^^'y* ^^^' "^'""-
{ ton, Cal.
Mr. J. Costa { ' M _^Montgomery St., S. F.,
Mr. Henry Cowell* 413 Hyde St., S. F., Cal.
Mr. Hugh Craig 312 California St., S. F., Cal.
Mr. Walter Cramp { '"llE Pa^'°^'' ^^" ''''"^"
Hon. C. F. Crocker* {^fT'cIl'' ^"'^ ^'"^ ^"■'
Mr. Henry J. Crocker 508 California St., S. F.. Cal.
Mr. Edward Crosslev,* f.r.a.s.. . { ^^f^^gSa^d*^'"*''"'''* "^'''
Miss S. J. Cunningham | Swarthmore College, Delaware
Mr. Chas. S. Cushing 813 12th St., Oakland, Cal.
Mr. J. EWEN Davidson* ...:..{ Alexandra Plantation, Brans-
■" I combe, Mackay,Queensland.
Mr. Joseph E. Davis 154 Beacon St., Boston, Mass.
Mr. William T. Dawson Etna, Siskiyou Co., Cal.
Mr. C. W. Dearborn j ^ Oakland "ca?^"''"'^^^'''"^'
Dr.J. H. DeMeritt 1 1335 Vermont Ave., Washing-
Mr. A. B. Depuy 1 541^ Washington St.,Camden,
Mrs. John H. Devereux j ^^hb"*'"'' ^^^" ^'^^^'''"'''
4 Publications of the
Mr. W. H. Devine* Nagasaki, Japan.
Miss Grace H. Dodge' j '%oK'°Y. ^''^""^' ^^^^
Mr. John Dolbeer lo California St., S. F., Cal.
Mr. W. E. Downs • . . . . Sutter Creek, Amador Co., Cal.
Mrs. Anna Palmer Draper* . . . . -j 27i^Madison Ave.. New York,
Rev. W. Arthur Duckworth, j. p. . . Frome. Somerset, England.
Mr. Francis G. Du Pont Wilmington. Del.
Mr. Earnest I. Dyer 1383 Alice St., Oakland, Cal.
Miss S. J. Eastman Ogontz School, Pa.
Mr. Geo. W. Edwardes j ^33 South Orange St., Media,
Prof. George C. Edwards Berkeley, Cal.
Capt. Oliver Eldi<idge 615 Sutter St., S. F., Cal.
Mr. THOMAS GwvNE.aHK { ^^d^Sf ^.3.^^"
Mr.R.L.J.E.UK.v,c.M.G.. . . -. . {''''^^t^^^:^^^^^''^^
Mr. John Everding, Jr 48 Clay St., S. F., Cal.
{Puisne Judge, Supreme Court,
Pielermaritzburg, Natal,
South Africa.
Mr. S. Wilson Fisher 1502 Pine St., Philadelphia, Pa.
Miss Katharine Flavan 2014 Van Ness Ave., S.F., Cal.
Mr. Andrew B. Forbes* 401 California St., S. F., Cal.
Mr.GHO.STUAaTFoRBKS {^Yn'dS;nSl';°y;in^^l!
Mr. Arthur W. Foster* 322 Pine St., S. F., Cal.
Mr. C. L. Foster 601 Polk St., S. F., Cal.
Mr. H. C. Frick* 42 5th Ave., Pittsburgh, Pa.
Prof. Chas. W. Friend Observatory, Carson, Nev.
Mr. Robert D. Fry* 1812 Jackson St., S. F., Cal.
Mr. Walter F. Gale, f. r. a. s Paddington, Sydney, N. S. W.
Mr. Jos. F. Gassmann 318 Montgomery St., S.F., Cal.
Mr. Otto VON Geldern | Room 56. 819 Market St.. S.F..
Mr. Louis Gex Santos, Brazil.
Hr HAvinnifr r n f Royal Astronomer, Cape of
Dr. David Gill, c. b ^ ^^^^ ^^p^^ ^^^.j^^
Mr. Allen F. Gillihan 2420 Fulton St., Berkeley, Cal.
\f.. r-T«^r>^w^ /-,^.o^i.T /South Pasadena, Los Angeles
Mr. George Gleason s ^ pi ' ^
Mr rAXfirr. ri^M7Aii7Q (National Observatory, Tacu-
Mr. Camilo Gonzales | ^^^^^ Mexico.
^ ^ r-«A«rT.o r-rx^T^*r ,* I S. E. cor. McAlHster aud Plercc
Capt. Charles LjOodall* < q^ q P p .
Mr. H. M. Gorham
Mr. Adam Grant*
Mr. H. M. Gorham Gold Hill, Nevada.
f N. E. cor. Bush and Sansome
\ Sts., S. F., Cal.
TV* T^^r^r,., T^ r-r»AVTa<* i ^- E. cor. Bush and Sansome
Mr. Joseph D. Grant* • | g^^^ 5 p^ ^^,
Astronomical Society of the Pacific. 5
Rev. Charles Graves {^Towa^ C\iyxx<:\ Anamosa.
Tu.. T x> nr*».xr f Dunstable St., Ampthill, Bed-
Mr. 1. r. LrRAV I fordshire, England.
Mr. Andrew Greig* Belle Vue, Tayport, Scotland.
Sir George Grey,* k. c. b Auckland, New Zealand.
Mr. P. HHNRV GK,K..M {^°,^^^of St'EngTafd"""'
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' ^ \ burgh, Pa.
Astronomical Society of the Pacific. 9
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«» c- „,- u. ur... „ ( State Normal School, Valley
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12 Publications of the
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LIST OF CORRESPONDING INSTITUTIONS.
Albany, New York, Dudley Observatory.
Allegheny, Pennsylvania, Allegheny Observatory.
Armagh, Ireland, Armagh Observatory.
Berlin, Germany, Redaction des Berliner Jahrbuchs.
Berlin, Germany, Royal Observatory.
Cambridge, England, University Observatory.
Cape Town, Africa, Royal Observatory.
Christiania, Norway, University Observatory.
Cincinnati, Ohio. University Observatory.
Cordoba, Argentine Republic, National Observatory.
Dorpat, Russia, University Observatory.
Dublin, Ireland, Dunsink Observatory.
Dublin, Ireland, Royal Dublin Society.
Edinburgh, Scotland, Royal Observatory.
Geneva, Switzerland, Observatory.
Glasgow, Scotland, Univeisity Observatory.
Gotha, Germany, Ducal Observatory.
Goeitingen, Germany, Royal Observatory.
Greenwich, England, Royal Observatory.
Hamburg, Germany, Observatory.
Helsingfors, Russia, University Observatory.
Kasan, Russia, University Observatory.
Kiel, Germany, University Observatory.
Koenigsberg, Germany, University Observatory.
La Plata, Argentine Republic, Observatory.
Leipzig, Germany, University Observatory.
Leyden, Holland, University Observatory.
Lisbon (Tapada), Portugal, Royal Observatory.
London, England, 26 Martin's Lane, British Astronomical Association.
London, England, British Museum.
London, England, Royal Astronomical Society.
London, England, 3 Verulam Bldgs., Gray's Inn, The Nautical Almanac.
Lund, Sweden, University Observatory.
Madison, Wisconsin, Washburn Observatory.
Madras, India, Observatory.
Madrid, Spain, Royal Observatory.
Marseilles, France, Observatory.
Melbourne, Victoria, Observatory.
Mexico, Mexico, Sociedad Cientifica "Antonio Alzate.'*
Milan, Italy, Royal Observatory.
Astronomical Society of the Pacific. 13
Moscow, Russia, University Observatory.
Munich, Germany, Royal Observatory.
Naples, Italy, Royal Observatory.
New Haven, Connecticut, Yale University Observatory.
New York, New York, American Mathematical Society.
New York, New York, Columbia University Observatory.
Nice, France, Observatory.
Northfield, Minnesota, Carleton College Observatory.
Oxford, England, Radcliffe Observatory.
Oxford, England, University Observatory.
Paris, France, Bureau of Longitudes.
Paris, France, National Observatory.
Potsdam, Germany, Astrophysical Observatory.
Prague, Austro-Hungary, University Observatory.
Pulkowa, Russia, Imperial Observatory.
Rio de Janeiro, Brazil, Observatory.
Rome, Italy, Observatory of the Roman College.
Rome, Italy, Italian Spectroscopic Society.
Rome, Italy, Specula Vaticana.
San Francisco, California, California Academy of Sciences.
San Francisco, California, Technical Society of the Pacific Coast.
Stockholm, Sweden, University Observatory.
Strassburg, Germany, University Observatory.
Sydney, New South W>«les, Observatory.
Tacubaya, Mexico, National Observatory.
Tokio, Japan, University Observatory.
Toronto, Canada, Astronomical and Physical Society of Toronto.
Toulouse, France, Observatory.
Turin, Italy, Observatory.
University Park, Colorado, Chamberlin Observatory.
University of Virginia, Virginia, McCormick Observatory.
Upsala, Sweden, University Observatory.
Vienna, Austria, Imperial Observatory.
Vienna (Ottakring), Austria, Von Kuffner's Observatory.
Washington, District of Columbia, Library of Congress.
Washington, District of Columbia, National Academy of Sciences.
Washington, District of Columbia, Naval Observatory.
Washington, District of Columbia, Smithsonian Institution.
Washington, District of Columbia, The American Ephemeris.
Washington, District of Columbia, U. S. Coast and Geodetic Survey.
William's Bay, Wisconsin, Yerkes Observatory.
Zurich, Switzerland, Observatory.
EXCHANGES.
Astrophysical Journals Chicai^o, Illinois.
Sirius, Cologne, Germany.
The Observatory^ Greenwich, England.
14 Publications of the
FOR REVIEW.
[See Publications A. S. P., Vol. VIII, p. loi.J
The Caily San Francisco, California.
The Chronicle, San Francisco, California.
The Examiner, San Francisco, California.
The Mercury^ San Jos6, California.
The Overland Monthly, San Francisco, California.
The Record' Union^ Sacramento, California.
The Times, Los Angeles, California.
The Tribune, Oakland, California.
ON THE INFLUENCE OF CARBONIC ACID IN THE
AIR UPON THE TEMPERATURE OF THE EARTH.
By Professor S. Arrhenius.
[Abstract by Edward S. Holdkn.]
[Note. — The following very brief and inadequate notice of an important paper pre-
sented to the Royal Swedish Academy of Sciences in December, 1895, and printed in the
Philosophical Magazine, Volume XLI, pages 237-276, is given here chiefly for the pur-
pose of directing attention to an entirely novel and simple explanation of the vexed
questions relating to the Earth's temperature in past times and to the cause of the
Glacial Epoch. It is impossible in the present place to give more than the shortest
abstract.— E. S. H.]
7. Introduction: Observations of Lang ley on Atmospheric
Absorption,
**A great deal has been written on the influence of the
absorption of the atmosphere upon the climate. Tyndall,* in
particular, has pointed out the enormous importance of this
question. To him it was chiefly the diurnal and annual varia-
tions of the temperature that were lessened by this circumstance.
Another side of the question, that has long attracted the attention
of physicists, is this: Is the mean temperature of the ground in
any way influenced by the presence of heat-absorbing gases in the
atmosphere? Fourier maintained that the atmosphere acts like
the glass of a hot-house, because it lets through the light-rays of
the Sun, but retains the dark-rays from the ground. This idea
was elaborated by Pouillet; and Langley was by some of his
researches led to the view that ** the temperature of the Earth
under direct sunshine, even though our atmosphere were present,
as now, would probably fall to —200° C, if that atmosphere did
• The author's references to the original authorities are, in general, omitted here. —
E. S. H.
Astronomical Society of the Pacific. 15
not possess the quality of selective absorption." This view,
which was founded on too wide a use of Newton's law of cooling,
must be abandoned, as Langley himself in a later memoir
showed that the full Moon, which certainly does not possess any
sensible heat-absorbing atmosphere, has a ** mean effective tem-
perature'* of about 45° C.
The air retains heat (light or dark) in two different ways. On
the one hand, the heat suffers a selective diffusion on its passage
through the air; on the other hand, some of the atmospheric
gases absorb considerable quantities of heat. These two actions
are very different. The selective diffusion is extraordinarily great
for the ultra-violet rays, and diminishes continuously with in-
creasing wave-length of the light, so that it is insensible for the
rays that form the chief part of the radiation from a body of the
mean temperature of the Earth.
The selective absorption of the atmosphere is * * * of a
wholly different kind. It is not exerted by the chief mass of the
air, but in a high degree by aqueous vapor and carbonic acid,
which are present in the air in small quantities. * * * The
influence of this absorption is comparatively small on the heat
from the Sun, but must be of great importance in the transmission
of rays from the Earth. * * *
// The Total Absorption by Atmospheres of Varying Composition,
I J I. Thermal Equilibrium on the Surface and in the Atmosphere
of the Earth.
IV. Calculation of the Variation of Temperature that would
ensue in consequence of a given variation of the
Carbonic Acid in the Air,
If the quantity of carbonic acid increases in geometric pro-
gression, the augmentation of the temperature will increase nearly
in arithmetical progression. This rule — which naturally holds
good only in the part investigated — will be useful for the follow-
ing summary estimations.
V, Geological Consequences,
I should certainly not have undertaken these tedious calcula-
tions if an extraordinary interest had not been connected with
1 6 Publications of the
them. In the Physical Society of Stockholm there have been
occasionally very lively discussions on the probable causes of the
ice age; and these discussions have, in my opinion, led to the
conclusion that there exists as yet no satisfactory hypothesis
that could explain how the climatic conditions for an ice age
could be realized in so short a time as that which has elapsed
from the days of the glacial epoch. The common view hitherto
has been that the Earth has cooled in the lapse of time; and if
one did not know that the reverse has been the case, one would
certainly assert that this cooling must go on continuously.
Conversations with my friend and colleague, Professor Hogbom,
together with the discussions above referred to, led me to make a
preliminary estimate of the probable effect of a variation of the
atmospheric carbonic acid on the temperature of the Earth.
As this estimation led to the belief that one might in this
way probably find an explanation for temperature variations of
5° - io° C. , I worked out the calculation more in detail, and lay
it now before the public and the critics.
From geological researches the fact is well established that in
tertiary times there existed a vegetation and an animal life in the
temperate and arctic zones that must have been conditioned by a
much higher temperature than the present in the same regions.*
The temperature in the arctic zones appears to have exceeded the
present temperature by about eight or nine degrees. To this
genial time the ice age succeeded, and this was one or more times
interrupted by interglacial periods with a climate of about the
same character as the present, sometimes even milder. When
the ice age had its greatest extent, the countries that now
enjoy the highest civilization were covered with ice. This was
the case with Ireland, Britain (except a small part in the south),
Holland, Denmark, Sweden and Norway, Russia (to Kiev,
Orel, and Nijni Novgorod), Germany and Austria (to the Harz,
Erz-Gebirge, Dresden, and Cracow). At the same time an ice-
cap from the Alps covered Switzerland, parts of France, Bavaria
(south of the Danube), the Tyrol, Styria, and other Austrian
countries, and descended into the northern part of Italy. Simul-
taneously, too, North America was covered with ice on the west
coast to the forty- seventh parallel, on the east coast to the fortieth,
• For details cf. Neumayr, Erdgeschichte, Bd. 2, Leipzig, 1887; and Gbikib, "The
Great Ice-Age," 3d ed., London, 1894. ^kihok^i ^ Jordens Historia, p. 989, Stockholm,
1894. '
Astronomical Society of the Pacific, 17
and in the central part to the thirty-seventh (confluence of the
Mississippi and Ohio Rivers). In the most different parts of the
world, too, we have found traces of a great ice age, as in the Cauca-
sus, Asia Minor, Syria, the Himalayas, India, Thian Shan, Altai,
Atlas, on Mount Kenia and Kilimandjaro (both very near to the
equator), in South Africa, Australia, New Zealand, Kerguelen,
Falkland Islands, Patagonia, and other parts of South America.
The geologists in general are inclined to think that these glacia-
tions were simultaneous on the whole Earth;* and this most
natural view would probably have been generally accepted, if the
theory of Croll, which demands a genial age on the Southern
hemisphere at the same time as an ice age on the Northern, and
vice versa, had not influenced opinion. By measurements of the
displacement of the snow-line we arrive at the result — and this
is very concordant for different places — that the temperature at
that time must have been 4°- 5° C. lower than at present. The
last glaciation must have taken place in rather recent times,
geologfically speaking; so that the human race certainly had
appeared at that period. Certain American geologists hold the
opinion that since the close of the ice age only some 7000 to
10,000 years have elapsed, but this most probably is greatly
underestimated.
One may now ask, How much must the carbonic acid vary,
according to our figures, in order that the temperature should
attain the same values as in the tertiary and ice ages, respectively ?
A simple calculation shows that the temperature in the arctic
regions would rise about 8° to 9° C, if the carbonic acid increased
to 2.5 or 3 times its present value. In order to get the tempera-
ture of the ice age between the fortieth and fiftieth parallels, the
carbonic acid in the air should sink to 0.62-0.55 of its present
value (lowering of temperature 4^-5° C). The demands of the
geologists, that at the genial epochs the climate should be more
uniform than now, accords very well with our theory. The
geographical annual and diurnal ranges of temperature would be
partly smoothed away, if the quantity of carbonic acid was
augmented. The reverse would be the case (at least to a latitude
of fifty degrees from the equator), if the carbonic acid diminished
in amount. But in both these cases, I incline to think that the
secondary action due to the regress or the progress of the snow-
covering would play the most important r61e. The theory
•Neumayr, Erdgeschichte, p. 648; Nathorst, /. c. p. 992.
1 8 Publications of the
demands also that, roughly speaking, the whole Earth should
have undergone about the same variations of temperature;
so that, according to it, genial or glacial epochs must have occurred
simultaneously on the whole Earth. Because of the greater
nebulosity [cloudiness] of the Southern hemisphere, the variations
must there have been a little less (about fifteen per cent.) than
in the Northern hemisphere. The ocean currents, too, must
there, as at the present time, have effaced the differences in
temperature at different latitudes to a greater extent than in the
Northern hemisphere. This effect also results from the greater
nebulosity in the arctic zones than in the neighborhood of the
equator.
There is now an important question which should be answered,
namely: — Is it probable that such great variations in the quantity
of carbonic acid as our theory requires have occurred in relatively
short geological times ? The answer to this question is given by
Professor Hogbom. As his memoir on this question may not be
accessible to most readers of these pages, I have summed up and
translated his utterances which are of most importance to our
subject: *
"Although it is not possible to obtain exact quantitative
expressions for the reactions in nature by which carbonic acid is
developed or consumed, nevertheless there are some factors, of
which one may get an approximately true estimate, and from which
certain conclusions that throw light on the question may be
drawn. In the first place, it seems to be of importance to com-
pare the quantity of carbonic acid now present in the air with the
quantities that are being transformed. If the former is insignifi-
cant in comparison with the latter, then the probability for varia-
tions is wholly other than in the opposite case.
** On the supposition that the mean quantity of carbonic acid
in the air reaches 0.03 vol. per cent., this number represents
0.045 per cent, by weight, or 0.342 millim. partial pressure, or
0.466 gramme of carbonic acid for every cm.* of the Earth's
surface. Reduced to carbon, this quantity would give a layer of
about one millim. thickness over the Earth's surface. The
quantity of carbon that is fixed in the living organic worl^ can
certainly not be estimated with the same degree of exactness ; but
it is evident that the numbers that might express this quantity
ought to be of the same order of magnitude, so that the carbon
* HC>GBOM, Svensk kemisk Tidskri/t, Bd. vi, p. 169 (1S94).
Astronomical Society of the Pacific. 19
in the air can neither be conceived of as very great, nor as very
little, in comparison with the quantity of carbon occurring in
organisms. With regard to the great rapidity with which the
transformation in organic nature proceeds, the disposable quantity
of carbonic acid is not so excessive that changes caused by
climatological or other reasons in the velocity and value of that
transformation might not be able to cause displacements of the
equilibrium.
* * The following calculation is also very instructive for the ap-
preciation of the relation between the quantity of carbonic acid
in the air and the quantities that are transformed. The world's
present production of coal reaches, in round numbers, 500 millions
of tons per annum, or one ton per km.' of the Earth's surface.
Transformed into carbonic acid, this quantity would correspond
to about a thousandth part of the carbonic acid in the atmosphere.
It represents a layer of limestone of 0.003 n^iHifn. thickness over
the whole globe, or 1.5 km.^ in cubic measure. This quantity
of carbonic acid, which is supplied to the atmosphere chiefly by
modern industry, may be regarded as completely compensating
the quantity of carbonic acid that is consumed in the formation
of limestone (or other mineral carbonates) by the weathering or
decomposition of silicates. From the determination of the
amounts of dissolved substances, especially carbonates, in a
number of rivers in different countries and climates, and of the
quantity of water flowing in these rivers, and of their drainage-
surface compared with the land-surface of the globe, it is esti-
mated that the quantities of dissolved carbonates that are supplied
to the ocean in the course of a year reach at most the bulk of 3
km.' As it is also proved that the rivers the drainage regions of
which consist of silicates convey very unimportant quantities of
carbonates compared with those that flow through limestone
regions, it is permissible to draw the conclusion, which is also
strengthened by other reasons, that only an insignificant part of
these 3 km.' of carbonates is formed directly by decomposition of
silicates. In other words, only an unimportant part of this
quantity of carbonate of lime can be derived from the process of
weathering in a year. Even though the number given were, on
account of inexact or uncertain assumptions, erroneous to the
extent of fifty per cent, or more, the comparison instituted is of
very great interest, as it proves that the most important of all
the processes by means of which carbonic acid has been removed
20 Publications of the
from the atmosphere in all times — namely, the chemical weather-
ing of siliceous minerals, — is of the same order of magnitude as a
process of contrary effect, which is caused by the industrial de-
velopment of our time, and which must be conceived of as being
of a temporary nature.
** In comparison with the quantity of carbonic acid which is
fixed in limestone (and other carbonates), the carbonic acid of
the air vanishes. With regard to the thickness of sedimentary
formations and the great part of them that is formed by limestone
and other carbonates, it seems not improbable that the total
quantity of carbonates would cover the whole Earth's surface to
a height of hundreds of metres. If we assume loo metres — a
number that may be inexact in a high degree, but probably is
underestimated, — we find that about 25,000 times as much car-
bonic acid is fixed to lime in the sedimentary formations as exists
free in the air. Every molecule of carbonic acid in this mass of
limestone has, however, existed in and passed through the atmo-
sphere in the course of time. Although we neglect all other
factors which may have influenced the quantity of carbonic acid in
the air, this number lends but very slight probability to the hy-
pothesis, that this quantity should in former geological epochs have
changed within limits which do not differ much from the present
amount. As the process of weathering has consumed quantities
of carbonic acid many thousand times greater than the amount
now disposable in the air, and as this process from diflferent geo-
graphical, climatological, and other causes has in all likelihood
proceeded with very different intensity at difl*erent epochs, the
probability of important variations in the quantity of carbonic acid
seems to be very great, even if we take into account the compen-
sating processes which, as we shall see in what follows, are called
forth as soon as, for one reason or another, the production or
consumption of carbonic acid tends to displace the equilibrium to
any considerable degree. One often hears the opinion expressed,
that the quantity of carbonic acid in the air ought to have been
very much greater formerly than now, and that the diminution
should arise from the circumstance that carbonic acid has been
taken from the air and stored in the Earth's crust in the form of
coal and carbonates. In many cases this hypothetical diminution
is ascribed only to the formation of coal, whilst the much more
important formation of carbonates is wholly overlooked. This
whole method of reasoning on a continuous diminution of the
Astronomical Society of tlie Pacific. 21
carbonic acid in the air loses all foundation in fact, notwithstand-
ing that enormous quantities of carbonic acid, in the course of
time, have been fixed in carbonates, if we consider more closely
the processes by means of which carbonic acid has in all times
been supplied to the atmosphere. From these we may well
conclude that enormous variations have occurred, but not that
the variation has always proceeded in the same direction.
** Carbonic acid is supplied to the atmosphere by the follow-
ing processes: — (i) volcanic exhalations, and geological phe-
nomena connected therewith; (2) combustion of carbonaceous
meteorites in the higher regions of the atmosphere; (3) com-
bustion and decay of organic bodies; (4) decomposition of car-
bonates; (5) liberation of carbonic acid mechanically inclosed in
minerals on their fracture or decomposition. The carbonic acid
of the air is consumed chiefly by the following processes:
(6) formation of carbonates from silicates on weathering; and (7)
the consumption of carbonic acid by vegetative processes. The
ocean, too, plays an important r61e as a regulator of the quantity
of carbonic acid in the air by means of the absorptive power of
its water, which gives off* carbonic acid as its temperature rises,
and absorbs it as it cools. The processes named under (4) and
(5) are of little significance, so that they may be omitted. So too
the processes (3) and (7); for the circulation of matter in the
organic world goes on so rapidly that their variations cannot
have any sensible influence. From this we must except periods
in which great quantities of organisms were stored up in sedimen-
tary formations and thus subtracted from the circulation, or in
which such stored-up products were, as now, introduced anew
into the circulation. The source of carbonic acid named in (2)
is wholly incalculable.
*' Thus the processes (i), (2), and (6) chiefly remain as bal-
ancing each other. As the enormous quantities of carbonic acid
(representing a pressure of many atmospheres) that are now fixed
in the limestone of the Earth's crust cannot be conceived to have
existed in the air but as an insignificant fraction of the whole at
any one time since organic life appeared on the globe, and since
therefore the consumption through weathering and formation of
carbonates must have been compensated by means of continuous
supply, we must regard volcanic exhalations as the chief source
of carbonic acid for the atmosphere.
*' But this source has not flowed regularly and uniformly.
22 Publications of the
Just as single volcanoes have their periods of variation with
alternating relative rest and intense activity, in the same manner
the globe as a whole seems in certain geological epochs to have
exhibited a more violent and general volcanic activity, whilst
other epochs have been marked by a comparative quiescence of
the volcanic forces. It seems therefore probable that the quantity
of carbonic acid in the air has undergone nearly simultaneous
variations, or at least that this factor has had an important
influence. >
**If we pass the above-mentioned processes for consuming
and producing carbonic acid under review, we find that they
evidently do not stand in such a relation to or dependence on
one another that any probability exists for the permanence
of an equilibrium of the carbonic acid in the atmosphere.
An increase or decrease of the supply continued during geological
periods must, although it may not be important, conduce to
remarkable alterations of the quantity of carbonic acid in the air,
and there is no conceivable hindrance to imagining that this
might in a certain geological period have been several times
greater, or, on the other hand, considerable less, than now.'*
As the question of the probability of quantitative variation of
the carbonic acid in the atmosphere is in the most decided
manner answered by Professor Hogbom, there remains only one
other point to which I wish to draw attention in a few words,
namely: Has no one hitherto proposed any acceptable ex-
planation for the occurrence of genial and glacial periods?
Fortunately, during the progress of the foregoing calculations,
a memoir was published by the distinguished Italian meteoro-
logist, L. De Marchi, which relieves me from answering the
last question.* He examined in detail the different theories
hitherto proposed — astronomical, physical, or geographical, and
of these I here give a short rhuniL These theories assert that
the occurrence of genial or glacial epochs should depend on one
or other change in the following circumstances:
(i) The temperature of the Earth's place in space.
(2) The Sun's radiation to the Earth (solar constant).
(3) The obliquity of the Earth's axis to the ecliptic.
(4) The position of the poles on the Earth's surface.
•LuiGi Dk Marchi: Lf Cause deir Era Glaciate, \>x^m\2\o dal R. Instituto Lom-
bardo, Pavia, 1895.
Astronomical Society of the Pacific, 23
(5) The form of the Earth's orbit, especially its eccentricity
(Croll).
(6) The shape and extension of continents and oceans.
(7) The covering of the Earth's surface (vegetation).
(8) The direction of the oceanic and aerial currents.
(9) The position of the equinoxes.
De March I arrives at the conclusion that all these hypotheses
must be rejected. On the other hand, he is of the opinion that
a change in the transparency of the atmosphere would possibly
give the desired effect. According to his calculations, * * a lower-
ing of this transparency would effect a lowering of the temperature
on the whole Earth, slight in the equatorial regions, and increasing
with the latitude into the seventieth parallel; nearer the poles
again a little less. Further, this lowering would, in non-tropical
rejjions, be less on the continents than on the ocean, and would
diminish the annual variations of the temperature. This diminu-
tion of the air's transparency ought chiefly to be attributed to a
greater quantity of aqueous vapor in the air, which would cause
not only a direct cooling, but also copious precipitation of water
and snow on the continents. The origin of this greater quantity
of water- vapor is not easy to explain." De Marchi has arrived
at wholly other results than myself, because he has not sufficiently
considered the important quality of selective absorption which is
possessed by aqueous vapor. And further, he has forgotten that
if aqueous vapor is supplied to the atmosphere, it will be con-
densed till the former condition is reached, if no other change
has taken place. As we have seen, the mean relative humidity
between the fortieth and sixtieth parallels on the Northern hemi-
sphere is seventy-six per cent. If, then, the mean temperature
sank from its actual value-}- 5-3 by 4° -5° C, /. <f., to -)- 1.3
or -{-0.3, and the aqueous vapor remained in the air, the relative
humidity would increase to loi or 105 per cent. This is, of
course, impossible; for the relative humidity cannot exceed 100
per cent, in the free air. A fortiori, it is impossible to assume
that the absolute humidity could have been greater than now in
the glacial epoch.
As the hypothesis of Croll still seems to enjoy a certain
favor with the English geologists, it may not be without interest
to cite the utterance of De Marchi on this theory, which he, in
accordance with its importance, has examined more in detail
than the others. He says, and I entirely agree with him on this
24 Publications of the
point: **Now, I think I may conclude that from the point of view
of climatology or meteorology, in the present state of these
sciences, the hypothesis of Croll seems to be wholly untenable,
as well in its principles as in its consequences,*' *
It seems that the great advantage which C roll's hypothesis
promised to geologists, viz: of giving them a natural chronology,
predisposed them in favor of its acceptance. But this circum-
stance, which at first appeared advantageous, seems with the
advance of investigation rather to militate against the theory,
because it becomes more and more impossible to reconcile the
chronology demanded by Croll's hypothesis with the facts of
observation.
I trust that after what has been said the theory proposed in the
foregoing pages will prove useful in explaining some points in
geological climatology which have hitherto proved most difficult
to interpret.
PLANETARY PHENOMENA FOR MARCH AND
APRIL, 1897.
Bv Professor Malcolm McNeill.
March.
The Sun '* crosses the line** and spring begins just after mid-
night, March 19-20 P. S. T.
Mercury is a morning star, having passed greatest west elonga-
tion on February 15th. At the beginning of the month it rises not
quite an hour before sunrise, and may possibly be seen if the
weather conditions are very favorable, but its distance from the
Sun grows less throughout the month, and it comes to superior
conjunction on April ist.
Venus is an evening star, having passed its greatest east
elongation in February. During the month it draws a little
nearer the Sun, but sets more than three hours after sunset at
the end of the month. On March 21st it comes to its maximum
brilliancy, and all through the month it will be visible to the
naked eye in full daylight, if the sky is clear and free from haze.
Mars is still a prominent object in the western sky in the
evening, and does not set until after midnight. During the
• Dk Marchi, /. c. p. 166.
Astronomical Society of the Pacific. 25
month it moves about fifteen degrees eastward from the con-
stellation Taurus into Gemini, On March ist it is about three
degrees south of the second magnitude star /3 Tauri, The
planet has lost very much in brightness, but is still conspicuous.
At the end of the month its distance from us is about 130,000,000
miles, two and and one-half times as far away as it was at
opposition in December.
Jupiter passed opposition on February 23d, and is above the
horizon practically the whole night throughout March. It is
retrograding, moving westward and northward about three
degrees during the month toward the first magnitude star Reguius
(a Leonis), and at the close of the month is about three degrees
east of the star.
Saturn rises two hours earlier than during the corresponding
period in February, and toward the close of the month is well
above the horizon before midnight. It is in the constellation
Scorpio and moves slowly eastward and then begins to move
westward, but the total change of position is only a fraction of a
degree. It is about one degree north of fi Scorpii, The rings
are in good position for observation, being well out toward their
maximum opening.
Uranus is near Saturn about two degrees west and one degree
thirty minutes south, and moves in about the same way but not
as fast.
Neptune is in Taurus and sets at about midnight.
April.
Mercury passes superior conjunction on April ist, and through
the rest of the month is an evening star reaching greatest east
elongation on the morning of April 28th. From the middle of
the month it sets more than an hour after the Sun, and at the
end of the month it sets nearly two hours later. This is the best
time of the year for seeing the planet as an evening star.
Venus sets about three hours later than the Sun on April ist;
but it rapidly approaches the Sun and passes inferior conjunction
on the morning of April 28th. It will not be easy to see after
April 20th. Venus and Mercury are in conjunction on the
morning of April 17th, Mercury being five degrees south.
Afars still sets after midnight. During the month it moves
about seventeen degrees eastward in the constellation Gemi7ii,
and at the close is south of Castor and Pollux (a and P Gcmin-
26 Publications of the
orum), the distance from the nearer star not being greatly dif-
ferent from their distance apart. The planet makes a very near
approach to the third magnitude star c Geminorum on the
morning of April 8th. The least distance is only two minutes,
and to the naked eye the star will be lost in the glare of the
planet, but the phenomenon will occur while they are below our
horizon.
Jupiter is above the horizon until long after midnight. It is
in the constellation Leo, and moves slowly westward about one
degree toward the first magnitude star Regulus, until it stops and
begins to move eastward on April 26th. It is about two degrees
east of Regulus at the end of the month.
Sahirji rises at a little after 8 p.m. at the end of the month. It
is in the constellation Scorpio^ and moves about two degrees west-
ward during April away from the second magnitude star fi Scorpii,
which is a little east and south of the planet.
Uranus is about two degrees west and the same amount south
of Saturn. The distance west diminishes slightly, and the dis-
tance south increases slightly during the month.
Neptwie is in the constellation Taurus and sets before mid-
night.
Occullations, The Moon occults the Pleiades group on the
evening of April 5th. The Moon is then about four days old,
and it will be a fine opportunity for seeing the disappearance of
the stars at the dark limb. The times vary so for different parts
of the country that it is not worth while to try to give any here.
Explanation of the Tables.
The phases of the Moon are given in Pacific Standard time.
In the tables for Sun and planets, the second and third columns
give the Right Ascension and Declination for Greenwich noon.
The fifth column gives the local mean time for transit over the
Greenwich meridian. To find the local mean time of transit for
any other meridian, the time given in the table must be corrected
by adding or subtracting the change per day, multiplied by
the fraction whose numerator is the longitude from Greenwich
in hours, and whose denominator is 24. This correction is
seldom much more than i°*. To find the standard time for the
phenomenon, correct the local mean time by adding the differ-
ence betw^een standard and local time if the place is west of the
standard meridian, and subiradifig if east. The same rules apply
Astronomical Society of the Pacific, 27
to the fourth and sixth columns, which give the local mean times
of rising and setting for the meridian of Greenwich. They are
roughly computed for Lat. 40°, with the noon Declination and
time of meridian transit, and are intended as only a rough guide.
They may be in error by a minute or two for the given latitude,
and for latitudes differing much from 40° they may be several
minutes out.
Phases (
OF
THE Moon,
P. S. T.
New
Moon,
Mar. 3,
H. M.
3 56 A. M.
First
: Quarter,
Mar. 1 1 ,
7 28 A. M.
Full
Moon,
Mar. 18,
I 28 P. M.
Last
Quarter,
Mar. 25,
4 A. M.
The Sun.
R. A.
Declination.
Rises.
Transits.
Sets.
1897.
H. M.
'
H. M.
H. M.
H.
M.
Mar. I.
22 51
- 7
22
6 37 A.M
[. 12 12 P.M.
5 47 P.M.
II.
23 27
- 3
29
6 21
12 10
5
59
21.
4
4-
27
6 6
12 7
6
8
31-
41
+ 4
22
5 49
12 4
6
19
Mercury.
Mar. I.
21 23
— 16
58
5 44A.M
. ID 45 A.M.
3
46 P.M.
II.
22 23
— 12
28
5 48
II 5
4
22
21.
23 27
- 5
53
5 50
II 30
5
10
31-
36
+ 2
33
5 51
Venus,
II 59
6
9
Mar. I.
I 36
+ 13
17
8 12 A.M
2 58 P.M.
9
44 p. M.
II.
2 6
+ 17
16
7 48
2 48
9
48
21.
2 31
+ 20
27
7 21
2 34
9 47
31-
2 46
+ 22
37
6 48
Mars,
2 9
9
30
Mar. I.
5 21
4 25 39
II 7 A.M.
6 42 P.M.
2
I7A.M.
II.
5 39
+ 25 44
10 46'
6 21
I
56
21.
5 59
+ 25 41
10 26
6 I
I
36
31-
6 20
+ 25 29
10 9
5 43
I
17
Jupiter,
Mar. I.
10 27
+ 11
7
5 9 P.M.
11 47 P.M.
6
25A.M.
II.
10 23
+ 11
34
4 23
11 3
5
43
21.
10 18
+ 11
58
3 38
10 19
5
31.
10 15
+ 12
16
2 55
Sa turn.
9 37
4
19
Mar. I.
15 56
- 18 1
[2
12 23 A.M.
5 19 A. M.
10
15 P.M.
II.
15 56
— 18
II
II 43 P.M.
4 40
9
37
21.
15 56
- 18
8
II 3
4
8
57
31-
15 55
- 18
3
10 23
3 20
8
17
28
Publications of the
Uranus,
1897.
R. A.
Declination.
Rises.
Transits.
Sets.
H. M.
H. M.
H. M.
H. M.
lar. I.
15 47
- 19 44
12 20 A.M.
5 lOA.M.
10 P.M
II.
15 47
- 19 43
II 41
4 31
9 21
21.
15 47
- 19 42
II 2
3 52
8 42
31-
15 46
- 19 39
10 21
3 II
8 I
Neptune.
Mar. I. 56 + 21 29 II 10 A.M.
II. 5 6 + 21 29 10 31
21. 5 7 -4-2[ 31 9 52
31. 58 +21 32 9 13
6 27 P.M. I 44 A.M.
5 48 15
59 12 26
4 30 II 47 P.M.
Eclipses of Jupiter* s Satellites, P. S.
(Off right-hand limb as seen in an inverting telescope.)
H. M.
T.
I. R,
Mar. 3.
3 A. M.
IV, R, Mar. 14.
4 28 P. M.
I, R.
4-
9 30 p. M.
I, R.
19.
I 18 A.M.
Ill, R,
5-
6 27 P. M.
Ill, R.
20.
2 24 A. M.
I, R,
6.
3 58 P- M.
I, R,
20.
7 46 P. M.
II, R,
6.
II 25 p. M.
II, R,
21.
4 37 A. M.
I, R,
10.
4 55 A. M.
II, R,
24.
3 55 P. M.
I, R,
II.
II 23 P. M.
I, R,
26.
3 12 A.M.
III, R,
12.
10 25 P. M.
I, R,
27.
9 41 p. M.
I, R,
13.
5 52 P. M.
I, R,
29.
4 9 p. M.
II, R,
14.
2 I A. M.
II, R,
31.
8 31 P.M.
Minima of Algol, R S. T.
H. M.
H. M.
Mar. 2.
12 33 p. M.
Mar. 19.
5 27 p. M.
5.
9 22 A. M.
22.
2 16 p. M.
8.
6 1 1 A. M.
25-
II 5 A. M.
II.
3 A. M.
28.
7 54 A. M.
13.
II 49 p. M.
31-
4 43 A. M.
16.
8 38 P. M.
Phases of the
Moon, P. S.
T.
New
Moon, Apr
H. M.
I, 8 24
p. M.
First
Quarter, Apr
10, 12 27
A. M.
Full
Moon, Apr.
16, 10 25
P. M.
Last
Quarter, Apr
23. I 48
P. M.
The Sun.
1897.
R. a.
Declination. Rises. Transits.
Sets.
H. M.
•^ ' H.
M. H.
M.
H. M.
Apr. I.
44
+ 4 45 5
47 A.M. 12
3 P.M
. 6 19 P.M
II.
I 21
+ 8 31 5
32 12
I
6 30
21.
I 58
+ 12 3 5
18 II
59 A. M
. 6 40
May I.
2 36
+ 15 15 5
4 II
57
6 50
Astronomical Society of the Pcuific.
29
Mercury,
R. A.
Declination.
Rises.
Transits.
Sets.
1897.
H. M.
H. M.
M. M.
H. M.
Apr. I.
43
+ 3 28
5 52 A.M.
12 3 P.M.
6 14 P.M.
II.
I 59
+ 12 45
5 55
12 39
7 23
21.
3 8
+ 19 56
5 58
I 9
8 20
May I .
3 55
+ 23 5
5 54
Venus.
I 17
8 40
Apr. I.
2 47
+ 22 45
6 44 A.M.
2 6 P.M.
9 28 P.M.
II.
2 48
+ 23 17
6 4
I 28
8 52
21.
2 34
+ 21 43
5 17
12 35
7 53
May I.
2 12
+ 18 12
4 29
Mars.
11 33 A.M.
6 37
Apr. I.
6 22
+ 25 28
10 7 A.M.
5 41 P.M.
I 15A.M.
II.
6 44
+ 25 4
9 51
5 24
12 57
21.
7 7
+ 24 27
9 37
5 7
12 37
May I.
7 30
+ 23 38
9 15
4 51
12 17
Jupiter.
Apr. I.
10 15
+ 12 18
2 51 P.M.
9 33P-M.
4 15A.M.
II.
10 12
+ 12 30
2 8
8 51
3 34
21.
10 II
+ 12 35
I 28
8 u
2 54
May I.
10 II
+ 12 33
12 48
5"^ TURN.
7 31
2 14
Apr. I.
15 55
-18 3
10 19 P.M.
3 16 A.M.
8 13A.M.
II.
15 53
-17 56
9 38
2 35
7 32
21.
15 51
-17 48
8 55
I 53
6 51
May I.
15 48
- 17 39
8 13
Uranus.
I II
6 9
Apr. I.
15 46
— 19 39
10 16 P.M.
3 7 A-M.
7 58 A.M.
II.
15 45
- 19 35
9 35
2 26
7 17
21.
15 43
- 19 31
8 55
I 46
6 37
May I.
15 42
— 19 26
8 14
I 5
5 56
Neptune.
Apr. I.
5 8
4-21 32
9 9 A.M.
4 26 P.M.
II 43P.M.
II.
5 8
+ 21 34
8 31
3 48
II 5
21.
5 10
+ 21 36
7 53
3 10
10 27
May I.
5 II
+ 21 37
7 15
2 32
9 49
Eclipses
> OF lupiTER-s Satellites, P. S.
T.
(Off right-band limb, as seen in an inverting telescope.)
H. M.
H. M.
I, R,
Apr. 3.
II 35 P-
M. I, R,
Apr. 19.
9 54 P- M.
I, R.
5.
6 3P.
M. I, R,
21.
4 22 P. M.
II, R,
7.
II 6 p.
M. III. D,
24.
6 57 p. M,
I, R,
II.
1 30 A.
M. Ill, R,
24.
10 17 p. M
I, R,
12.
7 59 P-
M. II, R,
25-
5 36 P- M
II, R.
15.
I 43 A.
M. I, R,
26.
II 48 P. M,
Ill, R,
17.
6 19 p.
M. I, R,
28.
6 17 P. M
30 Publications of the
Minima of Algol, P. S. T.
Apr.
H.
M.
H.
M.
3-
I
32 A. M.
Apr.
17-
9
37 A. M
5-
10
21 P. M.
20.
6
26 A. M
8.
7
10 P. M.
23.
3
15 A. M
II.
3
59 P- M.
26.
12
4A. M
14.
12
49 P. M.
28.
8
53 P. M
ABJURATIO GALILEI.
Ego, Galileus Galilei, filius quondam Vincentii Galilei,
Florentinus, aetatis meae Annorum 70, constitutus personaliter in
judicio, & genuflexus coram vobis Eminentissimis, & Reveren-
dissimis Dominis Cardinalibus universae Christianae Reipublicae
contra haereticam pravitatem generalibus Inquisitoribus, habeas
ante oculos meos sacro sancta Evangelia, quae tango propriis
manibus, juro me semper credidisse, & nunc credere, & Deo
adjuvante in posterum crediturum omne id, quod tenet, praedicat,
& docet S. Catholica, & Apostolica Romana Ecclesia. Sed
quia ab hoc S. Officio, eo quod postquam mihi cum praecepto
fuerat ab eodem juridice injunctum, ut omnino defererem falsam
opinionem, quae tenet Solem esse centrum, nee moveri, nee
possem tenere, defendere aut docere quovis modo, vel scripto
praedictam falsam doctrinam : & postquam mihi notificatum
fuerat praedictam doctrinam repugnantem esse Sacrae Scripturae;
scripsi, & typis mandavi librum, in quo eandem doctrinam jam
damnatam tracto, & adduco rationes cum magna efficacia in
favorem ipsius, non afferendo ullam solutionem; idcirco judicatus
sum vehementer suspectus de haeresi, videlicet, quod tenuerim,
& crediderim Solem esse centrum Mundi, & immobilem, &
terram non esse centrum, ac moveri.
Idcirco volens ego eximere a mentibus Eminentiarum Vestra-
rum, & cujuscunque Christiani Catholici vehementem hanc sus-
picionem adversum me jure conceptam, corde sincero, & fide
non ficta abjuro, maledico, & detestor supradictos errores, &
haereses, & generaliter quemcunque alium errorem, & sectam
contrariam supradictae S. Ecclesiae, & juro me in posterum
nunquam amplius dicturum, aut asserturum voce, aut scripto
quidquam, propter quod possit haberi de me similis suspicio;
sed si cognovero aliquem haereticum, aut suspectum de haeresi,
denuntiaturum ilium huic S. Officio, aut Inquisitori, & Ordinario
loci, in quo fuero. Juro insuper ac promitto, me impleturum,
Astronomical Society of the Pacific. zi
& observaturum integre omnes poenitentias, quae mihi impositae
sunt, aut imponentur ab hoc S. Officio. Quod si contingat me
aliquibus ex dictis meis promissionibus, protestationibus, & jura-
mends (quod Deus avertat) contraire, subjicio me omnibus
poenis, ac suppliciis, quae a Sacris Canonibus, & aliis Consti-
tudonibus generalibus, & particularibus contra hujusmodi
delinquentes statuta, & promulgata fuerunt: Sic me Deus
adjuvet, & Sancta ipsius Evangelia, quae tango propriis
manibus.
Elgo, Galileus Galilei, supradictus abjuravi, juravi, promisi,
& me obligavi ut supra, & in horum fidem mea propria manu
subscripsi praesenti chirographo meae abjurationis, & recitavi
de verbo ad verbum.
Romae in Conventu Minervae, hac die 22. Junii Anni 1633.
Ego, Galileus Galilei, abjuravi ut supra manu propria.
THE WASHBURN OBSERVATORY.
By George C. Comstock, Director.
The University of Wisconsin owes to the late Governor
C. C. Washburn the astronomical observatory which bears his
name, but the original gift has been largely supplemented by
both public and private munificence.
The observatory, as originally built in 1878, consisted of a
dome, a centre hall, and two rooms, one east, the other west of
the dome. To these were added, at the instance of the first
Director, the late Professor J. C. Watson, an east wing, connected
to the original building by a corridor. The accompanying wood-
cut shows the building as seen from the east; the west room
which contains the meridian-circle being entirely hidden. In the
foreground to the right, is the Students* Observatory containing
the six-inch Clark equatorial, aperture 152 mm, with which much
of the early double-star work of Professor S. W. Burnham was
done, and an admirable broken transit of 76 mm aperture, by
Bamberg, which is the finest instrument of its type I have ever
seen. In the extreme left of the cut is seen the roof of the
Solar Observatory, constructed at his own expense by Professor
Watson, and destined for the reception of an underground
telescope to be used in a search for intra-mercurial planets.
32 Publications of the
A thorough test of the capabilities of such a telescope havings
been made with disappointing results by Professor E. S. Holdkn
upon his accession to the directorship of the observatory, the
building has long since been relegated to humbler uses.
The topography represented in the cut is in some respects
misleading, although it very well shows the open character of the
surroundings. The observatory stands upon the crest of a hill,
which slopes gently to the west, and more rapidly to the south
and north, upon which latter side it descends to the shores of
Lake Mendota, about a hundred feet below it.
The principal instruments of the observatory are the Clark
equatorial telescope of 395 mm (sixteen inches) aperture, and the
Repsold meridian-circle of 122 mm (five inches) aperture. The
latter instrument is substantially siinilar in construction and
appearance to the one illustrated at page 86, Vol. Ill, Pud/tea-
tions of the Astronomical Society of the Pacific, and in the hands
of the successive observers who have used it, has proved capable
of furnishing results of the highest order of excellence, both in
the determination of star places and in the investigation of stellar
parallaxes.
In its optical parts the Clark equatorial has shown itself an
instrument of very superior quality, but in respect of mounting"
it lacks many of the conveniences of more recently constructed
instruments. It is provided with a filar micrometer, double-
image micrometer spectroscope, a Zoellner astro-photometer
and a very complete set of oculars.
The small equatorial in the Students' Observatory, shown
in the accompanying cut, has been provided with a modified
LoEWY prism apparatus and employed in various researches
requiring the simultaneous observation of stars situated in widely
different parts of the heavens. This has required the construc-
tion of the peculiar type of dome there shown, with revolving
semi-circular shutter. This shutter has proved in practice an
excellent device, and may be recommended for general use in
small domes.
Three astronomical clocks (employed in connection with the
railway time-service), chronometers, a chronograph, an excellent
universal instrument* and a considerable amount of subsidiary
apparatus employed in instruction, supplement the equipment
above described. To this there should be added the excellent
Woodman Astronomical Library, comprising over five thousand
Astronomical Society of the Pacific. 33
books and pamphlets, which are housed in the east wing of the
observator>'.
The scientific activity of the pbservatory has lain almost
wholly along the lines of the older astronomy of precision, and
the chief results of that activity are set forth in the ten volumes
of its Publications,
Madison, December, 1896.
SOME LUMINOUS APPEARANCES IN THE SKY.
Bv VV. H. S. MoNCK.
In Nature for March 28, 1896, appeared an account of a
luminous appearance seen in the sky by Dr. Brauner, of
Prague, on the thirteenth of that month. There were five streaks
reaching from the western horizon towards the zenith, apparently
not of very long duration. It was only about an hour after
sunset, and Dr. Brauner ascribed them to some peculiar reflec-
tion in the upper regions of the atmosphere. This explanation,
however, is not applicable to a similar phenomenon described by
Mr. Lyon Browne, of Shrewsbury, in Knowledge for April; for
it was seen at 8** 30° on the 4th of March, and therefore a consider-
able time after sunset. It disappeared in the course of ten minutes.
It also stretched from the western horizon towards the zenith.
Mr. Browne thought it might be the zodiacal light, but this
seems hardly probable; and the descriptions given do not closely
resemble the aurora.
The hypothesis of any peculiar reflection in the upper strata of
the atmosphere is more clearly excluded by the following
examples of similar phenomena seen in the east after sunset.
Captain Noble describes one seen by him on the 28th of August,
1883, at lo*" 35" P.M. **For a moment I thought I was tracing
the apparition of a new and most glorious comet." It was seen
in the east- northeast. His description appeared in Knowledge^
and it seems that Mr. W. K. Bradgate saw an appearance at
Liverpool on the same night and in nearly the same direction that
Captain Noble had seen it in Sussex, but the hour was so much
later that it could hardly have been the same object. Then followed
an account of a similar appearance seen by Mrs. Harbin at
34 Publications of the
Yeovil at ^ 30" p.m. on the 21st of September, 1883, also in the
east-northeast.
I saw a similar object myself on the 4th of September, 1885.
It was in the east or east- northeast, and it was near 11 o'clock
P.M. when I saw it. I took it for a very fine meteor-train, and
described it as such in a letter to The Observatory, But I saw
no meteor, and a comparison with the descriptions of Captain
Noble, Mr. Bradgate, and Mrs. Harbin in Knowledge led
me to conclude that what I had seen was of the same kind. As
far as these scanty data go, these appearances seem to occur in
spring and autumn, being in the west in spring and in the east
in autumn. The resemblance to the tail of a comet presented by
them has struck many observers, and I am inclined to think that
on certain occasions they have been mistaken for comets' tails.
The first of these which I shall notice occurs in The AnnucU
Register for 1761:
**July 18. At a quarter past eleven o'clock at night, a comet
was seen off the quarter of His Majesty's ship Princess Royal at
the Nore during nearly half a minute, very bright and light, but
the clouds being thick obscured it presently. It had a very long
tail and appeared to the E. S. E."
A real comet of this magnitude could not have escaped other
observers. Clouds, however, seem rather a frequent accompani-
ment of the kind of phenomenon with which I am dealing.
On the 9th of April, 1894, Mr. Edwin Holmes announced that
he had discovered a bright comet in the constellation Draco.
Mr. Holmes had discovered a comet not very long before, and
the resemblance must have been striking in order to deceive him.
Unfortunately, I have not the details of his observation at hand,
but I have doubt that he mistook one of the appearances on
which I have been commenting for a comet. The same remark
applies to the discovery of a comet, or rather comet's tail, by
Mr. Eddie at Grahamstown, in South Africa, some time pre-
viously, but I do not recollect even the dale of this announce-
ment. The failures of astronomers are apt to be speedily
forgotten. But clearly they saw something; and I believe both
Mr. Holmes and Mr. Eddie saw it with the naked eye. That
it was not the zodiacal light, or a meteor- train I am convinced;
nor do I think that these appearances are explicable as auroras,
though that solution seems, on the whole, more probable.
I have not hitherto seen any notice of this phenomenon on the
Astronomical Society of the Pacific. 35
American continent, and I hope that American observers will
keep an eye out for it in future. The great extent of the United
States might enable it, if it be an atmospheric phenomenon, to be
viewed simultaneously from all sides; while if it presented similar
features at distant stations, light would also be thrown on its
origin. Possibly, the present paper may lead to the publication
of similar observations already made in America. The subject is,
I think, worthy of the attention of astronomers. Even if the
appearances should prove to be atmospheric, the atmosphere is
the medium through which all observations must be made, and
it is highly desirable on that account to become acquainted with
all its properties. Its influence on the phenomena of lunar
eclipses ss of a very marked character, and has hardly received
adequate consideration; while the twinklings of the stars is
believed to be also an atmospheric phenomenon. It is probably
owing to this twinkling — certainly to some property of the
atmosphere — that stars are often caught by glimpses, and that
astronomers have imagined that they saw stars were there were
none. The satellites of Uranus and the stars in the trapezium
of Orion form remarkable examples of this. If we could remove
the atmosphere, our seeing would be steady.
But the occurrences in the upper portions of the atmosphere
are worthy of study on their own account, and astronomers are
the persons to study them. A pulsation or flickering, for instance,
has often been observed in the tail of a comet. It has been
pointed out that this can hardly be real; but if not so, it must
indicate the passing of a wave of a peculiar character through
the atmosphere. This wave seems to pass from the head of
the comet to the end of the tail; and as the tail is pointed
towards the Sun, the atmospheric wave must pass in the same
direction. Twinkling is perhaps a similar phenomenon which
exhibits itself among the stars successively rather than simultane-
ously — a star nearer to the Sun exhibiting any given phase
later than a star more remote from it on the sphere. The con-
dition of the upper strata of the atmosphere may also seriously
affect our results in meteoric astronomy; for no meteor can be
seen until it has traversed a sufficient quantity of air to change its
original extreme cold into intense luminosity. But does such
luminosity imply intense heat, or does the rush of the meteor
excite some such properties in the air as those which render
themselves visible in the aurora ? We have a good deal still to
3^ Publications of the
learn about our atmosphere, and it may afford a guide to us in
dealing with the atmospheres of other bodies.
(TWENTY-SIXTH) AWARD OF THE DONOHOE
COMET-MEDAL.
The Comet-Medal of the Astronomical Society of the Pacific
has been awarded to Mr. C. D. Perrine, Assistant Astronomer
in the Lick Observatory, for his discovery of an unexpected
comet on November 2, 1896.
The Committee on the Comet-Medal,
Edward S. Holden,
j. m. schaeberle,
W. W. Campbell.
1897, January 2.
ELEMENTS AND EPHEMERIS OF COMET g, 1896,
(PERRINE).
Bv F. H. Seares and R. T. Crawford.
From observations made at the Lick Observatory by Mr. C. D.
Perrine on December 8th, 9th, and loth, we have computed
the following elements and ephemeris of Comet g, 1896, (Per-
rine). The observations were telegraphed to the Students*
Observatory by Dr. Holden: —
T = 1896 Nov. 24.7839 G. M. T.
. 01 = 163° 38' 14" ) ^ ^ .
o ^ f Mean Equmox
'I '' . \ of 1896
/ =: 16 39 57 ) ^
q= 1. 15349
Representation of middle place —
(O— C) AX cos ^ = +5". 5 A^ = o".o
[The ephemeris at four-day intervals from December 13th to
25th is here omitted.] The brightness decreases from 0.91
(December 13th) to 0.59 (December 25th).
Students* Observatory,
Berkeley, December 12, 1896.
Astronomical Society of the Pacific. 37
LIST OF EARTHQUAKES IN CALIFORNIA FOR THE
YEAR 1896.
Compiled by C. D. Perrine.
The following list is a continuation of similar reports printed
in these Publications: Vol. II, p. 74; Vol. Ill, p. 247: Vol. V,
p. 127; Vol. VI, p. 41; Vol. VII, p. 99, and Vol. VIII, p. 222.
A more complete account will be published by the United States
Geological Survey as a bulletin. The dates are civil dates. The
times are Pacific Standard (120th meridian).
Roman numerals enclosed in parentheses indicate the intensity
on the Rossi- FoREL scale.
Some doubtful cases have been included, and are indicated by
an interrogation point enclosed in parenthesis.
List of Earthquake Shocks, 1896.
January 3. Esquimault (B.C.). 10:09 P.M. Reported by
E. Bavnes Reed, Esq. Victoria (B. C), 10:20 p.m.;
Port Angeles (Wash.), 10:30 p. m. The volcano of Kilauea
in the Hawaiian Islands in eruption.
January 5. Volcanoes below the Cocopah Mountains reported
in eruption.
January 8. Lake Chepala, Mexico.
January 25. Carson (Nevada), 4:45 a.m.; 4:46 a.m.; 5:02 a.m.
Reported by Professor C. W. Friend.
January 27. Carson (Nevada), 7:59 a. m. (II); 8:34 a.m. (Ill);
11:04 a.m. (Ill); 11:19 A.M. (I); 1:01 P.M. (IV); 6:32
p.m. (II), and quite a number of light tremors between.
Reported by Professor C. W. Friend.
February 5. Tauquiz Mountain (near San Jacinto). Volcanic
eruption. (?)
February 6. East Clallam (Wash.), 9:55 p. m.
February 13. Redding, io± a.m.; Weaverville, 9:55 a.m.;
Eureka, 9:55 a.m.
February 15. Los Angeles, 2:52 p.m. (another report says
2:45P.M.); Pasadena, 2:57 p.m.
March 15. Burrard Mountains (ten miles from Vancouver,
(B. C). Volcanic eruption. (?)
April 2. Portland (Oregon), 3:20^1 a. m.; McMinnville (Ore-
gon), 3:17 A.M.
3^ Publications of the
April 28. San Francisco, 2:57 p.m.; Alameda.
June 20 ±. Tidal wave on the Mendocino coast.
July 3. San Diego, 9:27 p. M.
July 23. Vallejo, 1:50 A.M.
August II. Mt. Hamilton, 8:58:7 ± p.m. (II). E. S. H.;
Alameda.
August 17. Merced, 3:40 a.m.; Visalia, 3:29, or 3:30 a.m.
(another report says 3:26 a.m.).
August 18. Mt. Hamilton, ii:o:24± p.m. (III). E. S. H.;
11:0:13 p.m. a. L. C; Napa, p.m.; Evergreen, 11:0:15
p.m. Reported by Wm. Wehner, Esq.
August 19. Alameda.
August 26. Mount Hood (Oregon). An avalanche. (Due to
an earthquake (?).
September i. Pinole, Contra Costa County, California. Powder
Works exploded at i p. m.
September 10. Santa Rosa, 3:45 a.m.
September 24. 5*^ 25" 30* ± p. m. (III). E. S. H.
5' 25" 45" P.M. (I), CD. P.)
October 19. Santa Rosa, 6 zb a. m.
November 3. Mt. Hamilton, 10:58.44 ±l V a. m , W. W. C.
November 11. Cahto, 2 a.m.
November 29. Mt. Hamilton, 11:3:37 a.m. (I). C. D. P.
December 8. Mexico (Pacific ports), 9:30 a. m., 1:30 p.m. and
5 P.M.
December 17. Santa Barbara. At 8 a. m. a tidal wave destroyed
a large section of the boulevard.
December 22. Mt. Hamilton, i** 52*" 42* p. m., P. S. T.
(TWENTY-SEVENTH) AWARD OF THE DONOHOE
COMET-MEDAL.
The Comet-Medal of the Astronomical Society of the Pacific
has been awarded to Mr. C. D. Perrine, Assistant Astronomer
in the Lick Observatory, for his discovery of an unexpected
comet on December 8, 1896.
The Committee on the Comet-Medal,
Edward S. Holden,
J. M. Schaeberle,
W. W. Campbell.
1897, February 8.
Astronomical Society of the Pacific. 39
NOTICES FROM THE LICK OBSERVATORY.*
Prepared by Members of the Staff.
Photograph of the Solar Surface made at the
Lick Observatory.
[See the Frontispiece.]
The frontispiece of the present volume is a gelatine print of a
portion of the solar surface copied by Mr. A. L. Colton from a
negative made by himself and Mr. C. D. Perrine, with the
thirty-six-inch equatorial, on October 19, 1896, at 10" 21" 2* a.m.
The aperture of the great telescope was reduced to eight inches,
and the exposure was made by means of a quick-shutter presented
to the Lick Observatory by Dr. A. Blair Thaw, of Santa
Barbara. Dr. Thaw bears the expense of making the plate for
this number of the Publications^ and deserves and will receive
the thanks of the Society. Edward S. Holden.
Discovery of Comet g, 1896, (Perrine).
This comet was discovered on the evening of December 8th,
at about 1 1 130 o'clock, in the constellation Pisces, At 20"* 29"" 48*
G. M. T. its position was R. A. o*' 52" 26'. 70, Decl. +6° 24'5i".9.
It was moving rapidly east and more slowly south.
The comet was moderately bright, — about as bright as a star
of eighth magnitude, — and in the four-inch comet-seeker appeared
round, with a well-defined central condensation. In the twelve-
inch equatorial, the comet was about 5' in diameter, and showed
a stellar nucleus. The nebulosity surrounding the head did not
appear to be symmetrical, but was more sharply defined on the
south following side, while it was extended on the north preced-
ing side in the shape of a broad fan. This fan-like extension was
not traceable for any considerable distance. On subsequent
•Lick Astronomical Department of the University of California.
40 Publications of the
nights the air has been full of haze, generally, so that I have not
been able to see the fainter nebulosity about the head.
Observations were secured on the 9th and loth also, — on the
latter date with difficulty, owing to thick haze ; and from these
and the one of the 8th Professor Hussey and I deduce the fol-
lowing system of parabolic elements : —
T = November 25.6659
o) = 164° 36' 5" )
Q, = 243 48 40 \ 1896.0
t = 16 26 29 j
log ^ = 0.06220
Residuals for the middle place (O — C) —
AX' COSTS' -I"
A^' ' +3
An ephemeris from these elements shows the comet to be
rapidly receding from both the Earth and Sun, and consequently
growing fainter. C. D. Perrine.
Mt. Hamilton, December 14, 1896.
ASTRONOMISCHE GeSELLSCHAFT ZoNE — 9° 50' tO — 14° lo'.
This zone was observed with the meridian-circle of Harvard
College Observatory during the years 1888-1892. The observa-
tions have since been reduced, and the apparent place resulting
from each observation can now be furnished. In most cases, the
mean place has also been computed. The work of revision by
additional observations of stars, accidentally omitted or unsatis-
factorily observed, is now in progress, and will probably be com-
pleted during the year 1897. Arthur Searle.
Relief-Map of the Lick Observatory Reservation
(2600 Acres).
By the kindness of Mr. Henry Gannett, Chief of the
Topographical Bureau of the U. S. Geological Survey, a survey
was made of the region about Mt. Hamilton during the summer
of 1 895. A map on the scale of j^, with contours at intervals of
fifty feet has been prepared. In order to exhibit the data in a
more vivid way, Mr. George A. Merrill, Principal of the
California School of Mechanic Arts (the trade-school founded
by Mr. Lick in San Francisco), has kindly undertaken to pre-
Astronomical Society of the Pacific, 41
pare a relief-model of the reservation on a scale of 500 feet to the
inch. This model will be made by the pupils of the Lick School.
When it is finished copies will be deposited at Berkeley, Mt.
Hamilton, and San Francisco. In making plans for the establish-
ment of a State Forestry Station on the reservation, for improve-
ment of the water-supply, for the fencing of the land, for new
roads, etc., etc., this model will be of much use. If the reserva-
tion is ever taken by the State as a Park (which is greatly to be
hoped), such a model will be indispensable. The thanks of the
Observatory are returned to Messrs. Gannett and Merrill for
their valued co-operation in our plans.
Edward S. Holden.
January i, 1897.
Meteors (November 15, 1896.)
Mrs. F. K. Upham, National Soldiers* Home, Los Angeles
County, a member of the Society, reports having counted nine-
teen meteors between four and ^\^ o'clock on the morning of
November 15, 1896, the greater number of which descended
from northwest of the zenith. Two of these were very brilliant,
but none were visible for more than thirty degrees of their path.
On August 25, 1896, at 7:47 o'clock, an unusually brilliant
meteor was seen near the eastern horizon, from whence it
passed over the zenith, disappearing ^v^ degrees to the west.
Its motion was very slow, and it left a bright train.
Observation of the Leonid Meteors.
Mr. William Yates, a member of the Astronomical Section
of the Southern California Academy of Sciences, observed the
Leonids on the morning of November 14, 1896, from his resi-
dence in Los Angeles. From 4 to 5:30 a. m. he counted seven-
teen meteors, of which all but one were true Leonids, One of
the latter left a train, which remained visible between four and
five minutes.
Notice to Members of the Society.
The Lick Observatory publishes for distribution **A Brief
Account of the Lick Observatory of the University of California,"
Svo, (1895), 29 pages and 15 plates. A copy will be sent to any
member of the Society who signifies his desires to have it.
Edward S. Holden.
Mt. Hamilton, January, 1897.
42 Publications of the /
The Great Sun-Spot of January, 1897.
On photographing the Sun with the forty-foot photohelio-
graph, January 5th, after two or three days of cloudy weather, I
found an unusually large spot well-started on its journey across
the disc. It could have been seen a day or two previously with
suitable weather, and had undoubtedly been seen elsewhere.
Occurring near a time of spot- minimum, it was of all the greater
interest. I was enabled to photograph it every day from the 5th
to the nth inclusive, and on the 14th and 15th; on the latter
date just as it was disappearing at the western limb. The ** see-
ing*' on January 5th was so bad that the photographs taken
were very poor; those secured on the following days were
much better. Figure i shows one of the photographs obtained
on the 6th, and Figure 2 one obtained on the 8th, the spot
having meanwhile changed considerably in form. The small,
isolated companion-spot retained its shape with curious per-
sistence. The extreme length of the nucleus of the principal
spot is about 35,000 miles; the length over all of the great spot
and its long attendant train of bits of penumbral matter, about
130,000 miles. The first, second, third, and fifth figures are
enlarged three diameters from photoheliograph negatives, and
have a scale of approximately 64,000 miles to the inch.
January 14th, the spot presented a most interesting appear-
ance as it approached the western limb. Figures 3 and 4 are
from negatives taken on that date. Extending easterly from the
spot is a fine cluster of faculae.
Figure 4 is a full-size reproduction of a negative by Mr.
Perrine and myself, using the photographic correcting-lens
of the thirty-six-inch equatorial, a rapid shutter made especially
for this work and presented to the observatory by Dr. A. B.
Thaw, and a supplementary lens for enlarging directly, giving a
scale about eight times as large as that of the focal image. The
negative from which this picture was made, is one of the best
results yet obtained with this instrumental outfit. Unluckily the
air was very unsteady, as is shown by the edge of the Sun and
the different portions of the spot.
Figure 5 was photographed on the morning of January 15th,
as the spot was on the very edge of the Sun's disc. In the
original negative a faint trace of the nucleus can be seen in the
midst of the penumbra. The appearance of indentation is inter-
Fig. I.
Fig. %
Frii. J.
Prt;, i.
rji;,
■ vii r^ntr hT CTTW_CDr4T /M? TAMfTADV tCao
Astronomical Society of the Pacific. 43
esting, though it must not be ascribed to the actual depression of
the spot, but rather to its deficiency in light compared to the
Sun's sur&ce. In this case, also, **bad seeing*' somewhat inter-
fered with the best results.
Owing to the great size of the spot, it will probably last for
more than a revolution of the Sun, and its reappearance at the
eastern limb near the end of this month will be awaited with
much interest. A. L. Colton.
January 20, 1897.
The Great Sun-Spot of January, 1897.
On Friday, January 15th, the large sun-spot, first noticed by
Mr. Colton, was passing out of view over the west limb of the
Sun, and it was hoped that a favorable opportunity would thus be
presented for determining the relative elevation of umbra and
^culae with respect to the photosphere. I, therefore, watched
the spot with the twelve-inch equatorial, diaphragmed down to
four inches aperture, using a Herschel prism and a 150-power
eye-piece — the highest power the seeing would permit.
At times the principal umbra appeared distinctly depressed,
and the faculae at all times seemed elevated above the average
sur&ce level; but the seeing was at no time good enough to make
it certain that this was not merely the effect of irradiation. The
spot was under observation from lo*" 50" A. m. to '^ 30" P. m.
R. G. AlTKEN.
January 19, 1897.
The Heliocentric Theory and the University of
Cambridge in 1669.*
** After dinner his highness (Grand Duke Cosmo III of Flor-
ence) desirous to gratify the Vice-Chancellor (of the University
of Cambridge), who entreated him to honor the academy with
his presence, went thither with his attendants, followed by the
Vice-Chancellor and the heads of the University. In the principal
hall, into which his highness was introduced, a short Latin oration
was made by one of the Professors, which, being pronounced in
the same manner as that which was spoken in the morning,
was but little understood. And afterward his highness was
•One hundred and iwenty-six years after the death of Copernicus.
44 Publications of the
present at different questions which were propounded for disputa-
tion and strenuously opposed by Professors and Masters of Arts.
De methodo philosophandi in experimentis fundata, et Contra
Sy sterna Copernicamim'' — From Travels of Cosmo the Third,
Grand Duke of Tuscany, through England, during the reign of •
King Charles the Second (1669), (translated from the Italian
manuscript by Count Magalotti in the Laurentian library at
Florence. London, 1821, pp. 224, 225.)
Honor Conferred on Professor Barnard.
The Royal Astronomical Society of London has awarded its
gold medal of the present year to Professor Barnard for his
astronomical discoveries and observations..
Prices of Reflecting Telescopes.
From an article in the Strand Magazine for October, 1896
(an interview with Sir Howard Grubb, F. R. S.), it appears
that the original cost of Lord RossE*s six-foot reflector was about
;^i 2,000, of the four-foot Melbourne reflector about ;^46oo, and
that the estimated cost of a ten-foot reflector of eighty feet focus
is ^33»ooo.
A Brilliant Meteor.
[Extract from a private letter by \Vm. S. Moses.]
**This evening (December 31, 1896) at 6*^ 7" P. S. T.. I
observed a brilliant meteor. It appeared at e Tauri and traveled
in a southwest course, expiring at i Ceti, It moved very slowly,
being visible, I think, three seconds. Its train was dazzling
white and cast a distinct shadow of the trees which intercepted
its light. The upper and lower edges of the train were bluish in
color. The head was scintillating. It did not burst, nor did I
hear an explosion. I happened to be looking at Mars and saw
it from beginning to end. It did not appear to be far distant.
As I took my chart and plotted its course within three minutes
after it disappeared, I think I am reasonably correct. It was the
finest meteor I ever saw. Accompanying I give a sketch of it.*'*
Lone Mountain Observatory, \
San Francisco, Cal. S
* The sketch is here omitted.
i849-
William C. Bond.
1872.
1850.
Benjamin Peirce.
Alex. D. Bache.
1876.
0. M. MiTCHEL. .
1879.
Sears C. Walker.
1855.
F, F. E. Bruennow.
1881.
Matthew F. Maury.
18S3.
Benjamin A. Gould.
1884.
1863.
George P. Bond.
1889.
1866.
Truman H. Safford.
1890.
1872.
Simon Newcomb.
1892.
Hubert A. Newton.
1894.
Astronomical Society of the Pacific, 45
List of American Foreign Associates of the Royal
Astronomical Society.
The first American who was elected one of the fifty Foreign
Associates of the Royal Astronomical Society (founded in 1820)
was William Cranch Bond, who was chosen in 1849. Fol-
lowing is a complete list:
Lewis M. Rutherfurd.
Charles A. Young.
George W. Hill.
Asaph Hall.
C. H. F. Peters.
Edward C. Pickering.
Samuel P. Langley.
Edward S. Holden.
Seth C. Chandler.
Lewis Boss.
William L. Elkin.
Albert A. Michelson.
List of Americans Who have Received the Medal of
THE Royal Astronomical Society.
Since the year 1823, the Royal Astronomical Society has
given a gold medal for services to science. The first American
to receive this medal was George Phillips Bond. The medal
has been awarded to the following Americans:
1865. George P. Bond. 1887. George W. Hill.
1874. Simon Newcomb. 1894. Sherburne W. Burnham.
1879. AsAPii Hall. 1896. Seth C. Chandler.
1883. Benjamin A. Gould. 1897. Edward E. Barnard.
1886. Edward C. Pickering.
Earthquake at Oakland, January 17, 1897.
On January 17, 1897, ^^ i** i^"* ^i* P- ^m P- S. T., two sharp
shocks were observed, about one second apart. The time given
is for the second shock, and is believed to be correct within a
second. In half an hour my watch was compared with W. U.
time, and the correction applied to the observed time.
The first shock seemed heavier than the second, and both
suggested an explosion rather than an earthquake. An examina-
tion of the country in the direction of the powder mills was made
immediately from the house-top with a glass, but no smoke or
M= 2°
3'
9".5
0= 246
30
22.1
0.= 163
51
41-5
«■= 50
22
3-6
«■= 13
45
19.7
46 Publications of the
other evidences of an explosion were visible. A heavy rumbling
was noticed just preceding the shocks, and the house creaked.
The windows on the north side of the house seemed to rattle
before and louder than those on the opposite side. The chan-
delier shook, and as it came to rest the vibrations appeared to be
north and south, approximately. A. H. Babcock.
Oakland, Cal., January 17, 1897.
Elliptic Elements of Comet g, 1896, (Perrine), by
W. J. HussEY AND C. D. Perrine.
From Mount Hamilton observations of December 8th, Decem-
ber 2oth, and January 5th, we have computed the following
elements of this comet:
Epoch, 1896, December 8.5, Gr. M. T.
>-Mean Ecliptic, 1897.0
log € == 9.836649
log fl = 0.549565
log ft = 2.725660
Period = 6.67 years.
With the exception of w or ^, these elements closely resemble
those of Biela's Comet at its last apparition in 1852.
Mount Hamilton, January 14, 1897.
Observations of the Companion to PRocvoNy and of
THE Companion to SiRiuSy bv J. M. Schaeberle.
Measures of the Compayiion to Procyon,
o //
1896. November 13. ^ = 318.8
November 14. 320.4
December 19. 319-3
1897. January 10. 322.3
Measures of the Companion to Sirius,
1896. October 28. 188.3
October 30. 190.0
November 6. 188.3
1897. January 10. 189.4
^ = 4-58
wt. = 3
4.58
2
4.89
I
4.62
3
7 Sirius,
365.
I
365
3
3-85
3
3-72
5
Astronomical Society of the Pacific. 47
Honor Conferred on Dr. Lewis Swift.
A press- telegram of January 5th notifies that the medal
founded by Mrs. Hannah Jackson (nh Gwilt) has been
conferred by the Royal Astronomical Society on Dr. Swift,
Directorof the Ldwef Observatory, **in recognition of his services
to the cause of science in the discovery of comets, etc.* '
The Ladd Observatory (Providence, R. I.)
During the year's leave of absence of the Director of the
Ladd Observatory (Professor Upton), which is to be spent at
the Arequipa station of the Harvard College Observatory, his
place is to be filled by Mr. F. W. Very, who has resigned the
position at the Allegheny Observatory which he has occupied
for so many year^.
Measures of the Companion to Procyon,
I have . secured three measures with the thirty-six-inch
refractor of the companion to Procyofi discovered by. Professor
Schaeberle. The mean is:
1896.98 32i°o 4".84
R. G. AlTKEN.
January 19, 1897.
Erratum in Publications A. S. P., No. 53.
Volume VIII, No. 53, page 311, liqe ^y for Schiaparelli
read Schaeberle. C. A. Y.
Astronomical Telegrams. (Translation.)
Lick Observatory, Dec. 9, 1896.
To Harvard College Observatory ) .g^^^ ^^ ^ .
and Students' Observatory: )
A comet was discovered by Perrine, December 8, 20** 29"
48* G. M. T.; R. A. o^ 52" 26'.7, Decl. + 6° 24' 52"! Daily
motion R. A. + 7"» Decl. — 30'. It is about as bright as a star
of eighth magnitude; has a well-defined nucleus and tail.
Lick Observatory, Dec. 9, 1896.
To Harvard College Observatory ) ^a . ^ ,, \
, ^ , . ^, I (Sent 10:45 p.m.)
and Students Observatory: ;
Comet Perrine was observed by Perrine, December 9,
IS** 37" 50" G. M. T.; R. A. o'' 58™ 9'. 9, Decl. + 6° 4' 30".
4^ Publications of the
Lick Observatory, December lo, 1896.
To Harvard College Observatory ) ^g^^^ ^^^
and Students' Observatory: )
Comet Perrine was observed by Perrine, December lo"*
14*' 8"* 58* G. M. T.; R. A. i** 4'" 51'. 9, Decl. + 5° 40' 46".
Lick Observatory, December 11, 1896.
To Harvard College Observatory: (Sent 10 a.m.)
Elements and ephemeris of Comet g were computed by
HussEY and Perrine. T = Nov. 25.67, 01=164° 3^', S3 =
243° 49', /= 16° 26', q= 1. 1540.
(Ephemeris is omitted here.)
Astronomical Telegrams.
(Dated) Boston, Jan. 11, 1897.
To Lick Observatory: (Received Jan. 11, 7^ 30" P. m.)
Lowell announces rift in Martian north polar cap since
January 7. Longitude, forty degrees.
John Ritchie, Jr.
Telegram.
(Dated) Lick Observatory, Jan. 15, 1897.
To Harvard College Observatory: (Sent lo*" o" a. m.)
HussEY and Perrine find Comet g periodic. Period and
elements, except omegas which differs sixty degrees, closely
resemble Biela.
Telegram (Translation),
(Dated) Cambridge, Mass., Jan. 15, 1897.
To E. S. Holden: (Received Jan. 15, 1897, 3:55 p.m.)
Please telegraph best elements and ephemeris available of
Comet g, Jownial issue awaiting them.
Seth C. Chandler.
The information requested above was supplied in a telegram
sent 8:50 p. M., January 15, 1897.
(See elements on another page, the ephemeris being omitted.)
Astronomical Society of the Pacific. 49
Minutes of the Meeting of the Board of Directors,
HELD IN the Rooms of the Society, January
30, 1897, AT 7:30 p. M.
President Hussky presided. A quorum was present. The minutes
of the last meeting were approved. The following members were duly
elected :
List of Members Elected January 30, 1897.
Mr. Frederick E. Brasch {^^^^ Devisadero St., S. F..
Mr. J. W. Erwin 1 2647^Dunint Avenue. Berkeley,
Mr. Albert Edward Gray Lasata,Oroville, Butte Co., Cal.
Mr. Edward G. Lukens 200 Market St., S. F., Cal.
Mr. Albxandbr W. Roberts .... {''•liJS;^^^ ^''•=*' ^'*^' ^*'
Dr. Horace H. Taylor Los Angeles, Cal.
Mrs. Columbus Waterhouse 2213 Howard St., S. F., Cal.
The following resolutions were, on motion, adopted:
Resolved, That the Directors of the Astronomical Society of the Pacific return the
thanks of the Society to Dr. A. Blair Thaw for his acceptable gift of the frontispiece
to Volume IX of the Publications.
Wherbas, There are at Mt. Hamilton, in the custody of the Secretary, and belong-
ing to the Society, sundry articles of bedding, etc., which, not being used, are deterior-
ating with age; be it therefore
Resolvedt That the Secretary at Mt. Hamilton is hereby authorized to dispose of the
said articles for the benefit of the Society.
Whbrbas. The Society possesses a considerable number of valuable books and
periodicals that are still unbound: and
Whbrbas, A considerable portion of the income from the Alexander Montgomery
Library Fund remains unexpended; be it therefore
Resolved, That the unexpended portion of the accrued interest from this Fund be
expended —
(1) For bindings for valuable unbound books and periodicals already in the posses-
sion of the Society; and then, if any portion of this income remains unexpended,
(2) For the purchase of additional astronomical books and periodicals; and be it
further
Resolved, That the President and Library Committee be authorized to carry these
provisions into effect.
Adjourned.
50 Publications of the
Minutes of the Meeting of the Astronomical Society
OF THE Pacific, held in the Lecture Hall of
the California Academy of Sciences,
January 30, 1897.
The meeting was called to order by President Hussey. The minutes
of the last meeting were approved.
The Secretary read the names of new members duly elected at the
Directors' meeting.
A committee to nominate a list of eleven Directors and Committee
on Publication, to be voted for at the annual meeting, to be held on
March 27th, was appointed, as follows: Messrs. Arthur Rodgers
(Chairman), John Dolbeer, A. . Callandreau, Geo. W. Percy, and
W. H. Hammon.
A committee to audit the accounts of the Tre.asurer. and to report
at the annual meeting, was appointed, as follows: Messrs. Von Geldern
CChairman), McConnell, and James R.' Kelly.
The following papers were presented:
Recent developments in Astronomical Photography, illustrated by
lantern slides, by Mr. Chas. B. Hill.
Some notes on the next Total Solar Eclipse, with lantern-slide illus-
strations, by Mr. Chas. Burckhalter.
Planetary Phenomena for March and April, 1897, by Professor
M. McNeill, of Lake Forest.
List of Earthquakes in California, 1896, by Mr. C. D. Perrine, of
Mount Hamilton.
Some Luminous Ap[>earances in the Sky, by Mr. W. H. S. Monck,
of Dublin.
Mr. Hill read a paper on the recent developments in Astronomical
Photography, illustrated by sixty lantern slides made at the Lick Obser-
vatory and elsewhere; the photographs exhibited were so selected as to
illustrate the results obtained up to the present time in all the different
branches of celestial photography.
Mr. Burckhalter showed a map of the path of the next total
solar eclipse in India, and gave some general information as to the
route and cost of travel to India, and the probable condition of the
weather at the time of the eclipse.
Adjourned.
Astronomical Society of the Pacific, 51
OFFICERS OF THE SOCIETY.
W. J. HussBY (Lick ObitrYatory), PresitUnt
E.J. MoLKRA (606 Clay Street, S. F.) )
E. S. HoLDBN (Lick Observatory), S Vice-Presidentt
O.voK Gbldern (819 Market Street, S. F.) )
C D. PBRRINB (Lick Observatory), Secretary
F. R. ZiBL (410 California Street. S. F.). Secretary and Treaturer
Board ef Directors — Messrs. Edwards, Holdrn, Hussby, Molbra, Miss O'Halloran,
Messrs. Pardbs, Pbrrinb, Pibrsun, bTRiNCHAM, VON Gbldbkn, Ziel.
Finance Committee — Messrs. von Gbldern, Pibrson, Stringham.
Committee OM Puhlication—lAtssxs. Holdbn, Babcock, Aitken.
Lihrary Committee — Miss 0'Hali.oran, Messrs. Molera, Burckhaltbr.
Committee OH the Comet- MedaZ—Mtisrs. Holdbn (ex-officio), Schabbbrlb, Campbell.
OFFICERS OF THE CHICAGO SECTION.
Executive Committee— ^x. Ruthven W. Pike.
OFFICERS OP THE MEXICAN SECTION.
Exeontive Committee— Mttsrs, Camilo Gonzalez, Francisco Rodriguez Rev.
NOTICE.
The attention of new members is called to Article VIII of the By-Laws, which provides that
the annual subscription, paid on election, covers the caiendar year only Subsequent annual
payments are due on January ist of each succeeding calendar year. Ihis rule is necessary in
order to make our book-keeping as simple as possible. Dues sent by mail should be directed to
Astronomical .Society of the Pacific S19 Market Street. San Francisco.
It is intended thai each member of the Society shall receive a copy of each one of the Pub-
lications for the year in which he was elected to membership and for all subsequent years. If
there have been (unfortunately) any omissions in this matter, it is requested that the Secretaries
he at once notified, in order that the missing numbers may be supplied. Members are requested
to preserve the copies of the Publications of the Society as sent to them. Once each year a title-
page and contents of the preceding numbers will also be sent to the members, who can then bind
the numbers together into a volume. Complete volumes for past years will also be supplied, to
members only, so far as the stock in hand is sufficient, on the payment of two dollars to either of
the Secretaries. Any non-resident member within the United States can obtain books from the
Society's library by sending his library card with ten cents in stamps to the Secretary A. S. P.,
819 Market Street, San Francisco, who will return the book and the card.
The Committee on Publication desires 10 say that the order in which papers are printed in
the PHblicntioHS is decided simply by convenience. In a general way, those papers are printed
first which are earliest accepted for publication. It is not possible to send proof sheets of papers
to be printed to authors whose residence is not within the United States. The responsibility for
the views expressed in the papers printed rests with the writers, and is not assumed by the
Society itself.
The titles of papers for reading should be communicated to either of the Secretaries as early
as possible, as well as any changes in addresses. The Secretar>' in San Francisco will send to
any member of the Society suitable stationery, stamped with the seal of the Society, at cost price,
as follows: a block of letter paper, 40 cents: of note paper, 25 cents; a package of envelopes, 25
cents. These prices include postage, and should be remitted by money-order or in U. S. postage
stamps, llie sendings are at the risk of the member.
Those members who propose to attend the meetings at Mount Hamilton during the summer
should communicate with "The Secretar>' Astronomical Society of the Pacific "at the rooms of
the Society, 819 Market Street, San Francisco, in order that arrangements may be made for
transportation, lodging, etc
PUBLICATIONS ISSUED BIMONTHL\.
( February ^ ApriU June, August ^ October, December.)
PvV
j AT--:
T I O N S
or THE
Astronomical Society of the Pacific.
Vol. IX. San Francisco, California, April i, 1897. No. 55.
ASTRONOMY AND ASTRONOMERS IN THEIR RELA-
TIONS TO THE PUBLIC.
By W. J. HussBY.
At this meeting of this Society, it is the custom for the retiring
President to address you on some scientific subject, and it has
occurred to me that it might be well to consider here "Astronomy
and Astronomers in Their Relations to the Public,*' and in doing
so attempt to answer some of the questions that an intelligent
public frequently asks, and at the same time indicate some of the
services to both that have been rendered by astronomical societies.
The work of the astronomer, like that of other scientists, is
only a little understood by the general public. Nevertheless, the
relations between the two are always the most cordial; and while
the astronomer may often be questioned as to the utility of his
labors, he can never complain of lack of appreciation. On the
contrary, the interest that attaches to a working observatory,
especially one that is readily accessible, is always so great that
regulations governing the admittance of visitors are indispensable,
in order that any time may be reserved for scientific work.
As a result of this interest, great advantages accrue to the
science. It has given the world many of its great observatories,
those of the University of Chicago and of the University of Cali-
fornia standing pre-eminent in the power of their telescopes.
So great, indeed, has become the generosity of those who are not
astronomers, that it would almost seem that astronomers have
only to ask for instruments and observatories to find appreciative
persons ready to supply their needs. This responsiveness is all
the more remarkable when we consider that the results of the
54 Publications of the
astronomer's labor are, in general, far removed from commodities
having a commercial value. New comets, new planets, new
satellites, new stars, worlds, and systems of worlds may be
discovered, and their histories may be long and interesting, but
not one of them can be exchanged for real or personal property.
From what has been said, it must not be understood that
astronomy has no practical applications. Far from that. The
determination of time, of latitude, of longitude, of azimuth, are all
problems of practical astronomy, and they are among those that
have more or less important relations to the ordinary affairs
of life.
The land is crossed in every direction by roads of steel.
Smooth tracks, swift locomotives, and comfortable cars make
travel easy and enjoyable; strong and commodious cars make
it possible for cities widely separated to carry on gigantic com-
mercial transactions. The trains glide along the tracks with great
speed, and are ever meeting and passing each other. This they
do with such precision that accidents are comparatively few — so
few, in fact, that on the average, only one passenger out of a
million and a half loses his life. This precision is due, in part, to
their being controlled by some central clock. But who controls
that clock? Who, with entire confidence that his statements
are true, can say that the time it indicates is correct or not?
Astronomers, by their long and laborious investigations, based
on a multitude of refined observations, have learned the motions
of the heavenly bodies with such accuracy that they can predict
the positions these bodies will occupy in the sky for many years
to come. They have prepared tables of these motions, giving the
positions of the Sun, Moon, planets, and principal stars for given
epochs. By means of these tables and astronomical observation,
they can, among other things, accurately determine the time, and
in no other way can it be done.
It was many years ago that the engineer applied mathematics
to the pressure of the wind and pressure of the wave, and
balanced the one against the other. The sail caught the wind, the
hull pressed the wave, and the famous clipper ships with their
precious cargoes sprang forward ten thousand miles, making
records of long-distance speed that have seldom been equaled.
By day and by night, the Sun, Moon, and stars, the compass,
their charts, and well-rated chronometers were their faithful guides,
directing their courses across the trackless oceans. The ships
Astronomical Society of the Pacific. 55
found their ways, and captains delivered rich cargoes, bringing
handsome returns for their voyages. Without these guides, such
voyages could not have been made, and if they had not been
made, the loss to commerce and civilization would have been
incalculable.
The circumstances that hastened, if they did not occasion the
establishment of the Royal Observatory at Greenwich, in 1675,
are full of interest, and since they refer to one of the most
imp>ortant practical applications of astronomy, I will give a brief
account of them.
At this time, a Frenchman, calling himself Le Sieur de Pierre,
came to the English court and announced the discovery of a
method of finding the longitude of a place. Incited by the
discovery of America and of routes by sea to India, the British
ships were beginning to find their way to all parts of the world.
Colonies were planted in many lands, and a commerce built up
that has added vastly to the material wealth of England. On
these long voyages, methods of finding latitude and longitude
were of prime importance. It was easy enough to find latitude,
but how to find longitude was a pressing problem for nearly a
century after the time of which we speak.
A commission composed of distinguished men, with the
privilege of adding others to their number if they saw fit, was
selected to hear and consider the method proposed by Le Sieur,
and to report the results of their inquiries to the king. Among
those whom the commissioners invited to join their number was
John Flamstead, then somewhat under thirty years of age,
but with a considerable reputation because of his astronomical
observations.
Le Sieur's method depended on the Moon's motion, and
required as data the date of observation, the latitude of the place,
the Moon's altitude, and the altitude of two known stars. Flam-
stead at once pointed out that the method was impracticable,
and in the controversy that followed he wrote two letters, one to
Le Sieur and one to the commissioners. In these letters he
said: *'If we had astronomical tables that would give us the two
places of the fixed stars and the Moon's true places, both in
longitude and latitude, nearer than half a minute, we might hope
to find the longitude of places by lunar observations. But that
we were so far from having the places of the fixed stars true, that
the Tychonic catalogues often erred ten minutes or more; * * *
5^ Publications of the
and that the best lunar tables differ one quarter, if not one third,
of a degree from the heavens.***
Flamstead's letter to the commissioners was shown to King
Charles. He was startied at the assertion of the fixed stars*
places being false in the catalogue, and with much vehemence
said : * * I must have them anew observed, examined, and corrected,
for the use of my seamen. I must have it done.** And on being
asked who could or should do it, the king replied: ** The person
who informs you of them."
Accordingly, on March 4, 1674-5, ^^ ^*"& signed a warrant
for Flamstead*s salary, a portion of which reads as follows: —
•* Whereas, w.e have appointed our trusty and well- beloved
John Flamstead, Master of Arts, our astronomical observator,
forthwith to apply himself with the most exact care and diligence
to rectifying the tables of the motions of the heavens, and the
places of the fixed stars, so as to find out the so much-desired
longitude of places for the perfecting the art of navigation.*'
The rest of the warrant relates to the payment of his salary,
which was ;^ioo a year.
On June 22, 1675, King Charles signed the warrant for build-
ing the observatory. It begins as follows: —
** Whereas, in order to the finding out of the longitude of
places for perfecting navigation and astronomy, we have resolved
to build a small observatory within our park at Greenwich, upon
the highest ground, at or near the place where the castie stood, with
lodging- rooms for our astronomical observator and assistant.**
The foundation of the observatory was laid August 10, 1675.
No provision was made for instruments. Flamstead had to
provide them himself, and at his death, after forty-four years of
laborious service, they **were actually claimed by the govern-
ment as their own, and his executors were annoyed with a vexa-
tious and troublesome lawsuit on that account.** [Baily: An
Account of Flamstead, p. 30.]
The Royal Observatory at Greenwich, founded under the
circumstances as related, and having especially in view the kinds
of astronomical work that lead to results of practical value, has
continued to the present time regularly to make those observa-
tions needed for *' rectifying the tables of the motions of the
heavens.'* It is impossible to give, or even to form, an adequate
•Flamstkad's History of his own Life in Baily's Account of the Rev, John Flam'
steady page 38.
Astronomical Society of the Pacific. 57
idea of the great importance of the astronomical work that has
been done at Greenwich.
The long series of observations, on the principal bodies of the
solar system and the brighter fixed stars, surpassing in duration
and magnitude any programme of work that could reasonably
be expected from any, except national observatories, is one of the
richest possessions of astronomy. It has furnished the data for
many of the most important investigations relating to the motions
of the heavenly bodies; the determination of these motions being
the principal problem that astronomers in all ages have been
attempting to solve. Indeed, this problem constituted so large
a part of astronomy even at the end of the first third of this
century, that Bessel, the greatest of practical astronomers,
wrote as follows: —
** What astronomy is expected to accomplish, is evidently at
all times the same. It must lay down rules by which the move-
ments of the celestial bodies, as they appear to us upon the Earth,
can be computed. All else which we may learn respecting these
bodies, as for example, their appearance and the character of their
surfaces, is, indeed, not undeserving of attention, but possesses no
proper astronomical interest. Whether the mountains of the
Moon are arranged in this way, or in that, is no further a subject of
interest to astronomers than is a knowledge of the mountains of
the Earth to others. Whether Jupiter appears with dark stripes
upon its surface, or is uniformly illuminated, pertains as little to
the inquiries of the astronomer; and its four moons are interesting
to him only for the motions they have. To learn so perfectly the
motions of the celestial bodies, that for any specified time an
accurate computation of them can be given — that was, and is, the
problem which astronomy has to solve. Newton gave it no new
problem; but his discovery encouraged the hope that a complete
solution to the old one could be obtained. This before his time
was not deemed possible.**
Astronomy has advanced a long way since these words by
Bessel were written. Two generations of theoretical and prac-
tical astronomers have lived since then ; the former have labored to
perfect the analysis relating to the motions of the heavenly bodies,
and to test its accuracy by comparing observed and computed
places, and the latter, following the methods of which Bessel
was the great exponent, have developed the theory of their
instruments and the theory of observation with mathematical
58 Publications of the
rigor, and have neglected only those terms which could be shown
to be insensible in their effects. Astronomy has also advanced
with marvelous rapidity in other directions. The investigations
which Bessel characterized as not undeserving of attention, but
as possessing no proper astronomical interest, together with
those that have arisen through the development of spectroscopy,
have unexpectedly attained such importance, and are so full of
promise for the future, as to merit a co-ordinate place beside the
investigations of the older astronomy, and constituting, as they do,
a new science, to be distinguished by an independent name —
astrophysics.
The older astronomy has lost none of its importance. There
has been no halt in its progress, and no diminution in the interest
that attaches to its results. This will always be the case. For
so long as civilization endures, it will be a factor in the affairs of
men. Besides, there are moral reasons. In common with other
scientists, the astronomer must strive to a perfect understanding
of the action of natural and moral forces; he cannot stop where
immediate practical applications end. His researches are based
on far-reaching principles, and lead to results that unfold pros-
pects among the greatest and sublimest furnished by any depart-
ment of human knowledge, and which, through the awakening
and proper use of the imagination, may be classed among the
most potent of moral and spiritual forces.
The investigations of the older astronomy are, from an
astronomical standpoint, characterized by a singleness of purpose.
Postulating the law of gravitation and the principles of rational
mechanics, it seeks to determine the motions of the heavenly
bodies. The newer astronomy is likewise characterized by a
singleness of purpose. Calling to its aid every available means
of inquiry, it endeavors to ascertain the nature and conditions of
these bodies, and thence to learn what has been their past and what
will probably be their future hbtories. Haifa century ago, it seemed
that the future advancement of astronomy would be along the
lines already marked out, and that it would consist chiefly in
perfecting the science by increasing the precision of its results.
It did not then seem probable that new departments of astronomy
would arise, and some of the results already obtained through
astrophysical research would then have appeared, even to the
boldest imagination, as hopelessly beyond human possibility.
The spectroscopic and other new methods of investigation have
Astronomical Society of the Pacific, 59
api>eared, more and more powerful telescopes have been con-
structed, by the new methods and by the increase of power many
old problems . have been solved, but new problems in greater
numbers have arisen to take their places. It will always be so.
The universe is infinitely varied. A few astronomers in a few
short years can at best fathom only a comparatively small
number of its mysteries.
Nearly three centuries have elapsed since the invention of the
telescope, and during this entire period rapid and wonderful
improvements have marked its history. For more than two
hundred years the popular use of the telescope was almost entirely
unknown. In fact, it was not until near the middle of the present
century, when the Cincinnati Observatory was established, that
the great revolution in this respect was begun. The foundation
of this observatory also marks an epoch in the history of science
in this country.
In 1832, Airy, **the Astronomer Royal of England, in his'
celebrated * Report on Astronomy * before the British Association,
after recounting with high eulogium what had been accomplished
in the building of astronomical observatories throughout the old
world, closes by saying, that as for the United States he did not
know of the existence of a single public observatory within the
limits of the entire country." It was then the general opinion
abroad that the nature of our institutions was not favorable to
the development of pure science. It was only ten years later,
however, that the Cincinnati Astronomical Society subscribed
$9500 for the purchase of an instrument, and made a provisional
contract for what was then the second largest refracting telescope
in the world. Since then, our observatories have rapidly increased
in number, and have become no less famous for the character of
their work than for the power and excellence of their telescopes.
The history of the foundation of the Cincinnati Observatory
is very interesting. By a series of popular lectures, General
MiTCHEL, then a Professor at Cincinnati, awakened deep interest
in the science of astronomy. The Cincinnati Astronomical
Society was the immediate result, and thence came the Cincin-
nati Observatory, with its long and honorable career.
On the 9th of November, 1843, the corner stone of the ob-
servatory was laid by John Quincy Adams, in the presence of a
vast multitude, with appropriate ceremonies, and followed by the
6o Publications of the
delivery of an address replete with beauty and eloquence. It was
the intention of the board of directors to pay for their telescope
before proceeding to the erection of the building. At this time
only $3000 had been paid in, and to meet their engagements,
$6500 would have to be collected by the following June, when it
was expected the great telescope would be ready for shipment
to the United States. General Mitchel became the general
agent of the society, and by undeviating perseverance raised the
entire sum before the specified time had expired. But after
paying for the instrument, not one dollar in cash remained with
which to begin the construction of the observatory building, which,
at the lowest estimate, must cost five or six thousand dollars.
Some two or three thousand dollars had been subscribed, payable
in work and materials; a suitable site on the summit of Mt. Adams
had been given, subject to certain conditions; but no one could
be found who would take the contract for the building in the face
of the many contingencies by which the affairs of the society were
surrounded. General Mitchel determined to hire workmen by
the day, and personally to superintend the erection of the building.
In attempting to contract for the delivery of brick on the summit
of Mt. Adams, he was asked such a high price for the hauling,
on account of the steepness of the hill, that all idea of a brick
building was at once abandoned, and it was decided to build of
limestone, an abundant supply of which could be had on the
grounds of the society by quarrying. The exorbitant charges
made for delivering lime were at once disposed of by building a
limekiln on the grounds. In a few days it was completed, filled,
and on fire, and soon lime in abundance was ready. Sand was
the next item for which extravagant charges were made. With
considerable difficulty, permission was obtained to open a sandpit
not far away, which had long been closed for fear that further
excavation would endanger a house on the hill above it. Then
the price asked for hauling the sand was so great that General
Mitchel was forced to buy horses, and in not a few cases to fill
the carts with his own hands and drive them to the top of the
hill, in order to demonstrate practically how many loads could be
fairly made in a day. The nearest water was at the foot of the
hill, half a mile away. To avoid hauling so far, a dam was
thrown across one of the deepest ravines on the hilltop, and the
rains allowed to fill it, to furnish the water needed for mixing the
mortar.
Astronomical Society of the Pcu:ific. 6i
The work of construction began early in June, 1844. The
force of hands for the first week consisted of two masons and one
man to tend them. With this force it would have taken about
twenty years to have erected the building, yet according to the
bond it must be completed by the following June, or the title to
the site must be forfeited.
By the end of the first week, General Mitchel had raised
enough money to pay his hands. He instructed his foreman to
double his force for the next week. At the end of it, he had
again obtained sufficient money to pay them in full. The force
was increased week after week in the same manner, until not less
than fifty day laborers were actually engaged in the erection of
the Cincinnati Observatory, and as many more in the shops in
the city were paying their subscriptions by work for the different
parts of the building. The doors were being made by one car-
penter, the window frames by another, the sashes by a third, a
painter took them from the joiner, and in turn delivered them to
the glazier, and finally a carpenter paid his subscription by hang-
ing them, using locks, hinges, cords, pulleys, and weights, all
obtained by subscription.
Each Saturday night saw the funds exhausted; each new week
was commenced in the full confidence that industry and persever-
ance would work out its legitimate results. To raise the cash
means was the greatest difficulty. Frequently, four or ^v^ trades
had to be made to convert due bills into cash, and not infrequently
did individuals cash their own due bills at a discount.
In July and August, the work went on rapidly, and in Septem-
ber, General Mitchel had the great satisfaction of seeing the
building up and covered, without having incurred one dollar of
debt and without neglecting his duties as Professor of Mathematics
and Philosophy in the Cincinnati College, where he was teaching
five hours a day.
By the terms of the subscription, each contributor, whether
of cash, work, or material, became a member of the Cincinnati
Astronomical Society, and came to have a personal interest for
himself and for his family, in this important observatory and its
great telescope. There were about 800 contributors, from all
professions and all ranks of society; probably not less than 4000
persons had acquired the right to look at the heavenly bodies
through this, the then second largest refractor in the world. At
first, many nights were devoted to their instruction and enter-
62 Publications of the
tainment; for the first year, only one night each \iceek was
reserved for scientific work, and in the second year, only three
nights each week.
We have now noted, briefly, the circumstances attending the
founding of two important public observatories, — one by royal
favor, the other by the will of the people. Both have long and
honorable careers; both have served as examples leading to the
establishment of other observatories, and both have ministered to
the wants of the people, though in very diff*erent capacities.
A little more than three quarters of a century ago the Astro-
nomical Society of London was organized, and the objects of the
original members are stated in an address circulated before their
first public meeting, in the following words: —
' * To encourage and promote their peculiar science by every
means in their power, but especially by collecting, reducing, and
publishing useful observations and tables; by setting on foot a
minute and systematic examination of the heavens; by encourag-
ing a general spirit of inquiry in practical astronomy; by estab-
lishing communication with foreign observers; by circulating
notices of all remarkable phenomena about to happen, and of
discoveries as they arise; by comparing the merits of diff*erent
artists eminent in the construction of astronomical instruments;
by proposing prizes for the improvement of particular depart-
ments, and bestowing medals or rewards on successful research
in all; and finally, by acting, as far as possible, in concert with
every institution, both in England and abroad, whose objects
have anything in common with their own, but avoiding all inter-
ference with the objects and interests of established scientific
bodies.'*
Surely, this was an ambitious program of work for a new
society, and that it was able to carry it out in full measure
demonstrates that its council contained masterly ability, and that
its affairs were wisely and carefully administered. Its success
from the beginning was far beyond expectation. In its first
list of members and associates, we find many distinguished
names. Babbage, Brewster, Faraday, Herschel, Arago,
Bessel, Gauss, Laplace, Olbers, Piazzi, and Struve are
among the number. The funds of the society grew, and
were carefully invested. Even at the ** first annual general
meeting*' the council was able to report that the invested funds
amoui^ted to more than $3700. Presents of books, papers, and
Astronomical Society of the Pacific, 63
instruments have been continually received for more than seventy-
five years, so that at the present time the property, aside from
investments, is so extensive that insurance to the extent of ;^5500,
or, approximately, $27,500, is no longer regarded as sufficient.
Its library has always been accessible at all reasonable hours, and
a generous spirit lias prevailed in regard to its instruments. In
its very infancy it began the publication of its Memoirs^ those sub-
stantial astronomical papers intended for the advancement of
science, which, in the aggregate, now number more than 15,000
quarto pages. Just seventy years ago it added to its publications
the Monthly Notices, which are now in their fifty -seventh volume.
The society soon became, and still continues to be, a great
force in the astronomical world. The great value of its publica-
tions, the interest in its regular monthly meetings, the advantages
arising from its library and many other privileges have combined
to make it popular at home and abroad. It has aided in the
advancement of science in a purely technical way; and again by
bringing science and the people closer together, to the great
benefit of both.
The society's early success was attributed by its members
themselves to the policy adopted in the beginning, ** by acting in
concert with every institution, both in England and abroad,
whose objects have anything in common with its own; but avoid-
ing all interference with the objects and interests of established
scientific bodies.** To this may be added the active and sincere
co-operation of its ablest members, without which the healthy
growth and prosperity of a scientific society is impossible, and
which can only exist when, in the management, there is entire
freedom from direction such as wielded by the typical political
boss.
The Astronomical Society of the Pacific has been in existence
about eight years. Its energies have been devoted to the diffu-
sion of astronomical knowledge by means of popular lectures and
by its Publications, In this way its services have been valuable
to the public and to astronomers. The welfare of the Society
demands that work along these lines shall be continued, and
that it shall be made as good in quality as can be obtained, and
as large in quantity as is consistent with an economical manage-
ment. An increase in the membership of the Society is emi-
nently desirable, for this would mean an increase of its funds,
of its possibilities, and of its responsibilities. The limits of its
64 Publications of the
usefulness will not be reached until it becomes an active force,
stimulating and encouraging astronomical research in all its de-
partments, and spreading astronomical knowledge to all classes.
San Francisco should have a great astronomical library.
Nothing could be more appropriate than that this should be the
property of the Astronomical Society. A beginning in this
direction has already been made. There are now some funds
for library purposes, there should be more; and from time to
time, valuable books and papers are being received from cor-
responding institutions and from individuals. Every gift in this
way is welcomed; all works on astronomy and the related
sciences have a value in such a place.
Since the Society is very largely composed of those who are
not professional astronomers, it may be said that the library need
contain only popular works. But this is plainly not enough. It
should be technical as well as popular, and as soon as may
be, complete in the periodical literature of the science. During
the past year, in connection with my Presidency of the Society,
I have learned of more than one case of young persons of this
city who are interested in the science, not as amateurs, but with
the expectation of becoming professional astronomers. To these
the Society has a duty, that of providing library facilities com-
mensurate with their aims. Such persons, if of marked ability,
soon largely outgrow popular books, and demand the works of
the masters and the entire range of periodical literature to satisfy
their wants.
Astronomical Society of the Pacific.
65
ASTRONOMICAL OBSERVATIONS IN 1896.
Made by Torvald Kohl, at Odder, Denmark.
Variable Stars.
January
Z Cygni.
8
18
■{
Z = d.
<d.
>e.
= e.
15' <e.
5: <e.
>r.
<26.
30: a little > b.
September 8 : = b.
February
May
August 15
■{
September 26: ]
October
30
8
<c.
>ci.
id.
■r
November
11:
26:
28:
30:
4:
7:
8:
X' Cygni,
January 8
May
January
May
August
13
18
19
7
9
>a.
<A.
id.
almost = A.
id.
id.
August
15:
17:
>e.
a little > e.
= e.
= e.
= e.
<e.
<e.
<e.
invisible,
id.
September 26: id.
October 8: a little < k.
26: id.
28: id.
The Stars A and B, near X"* Cygni,
8:
13:
18:
19:
5:
7:
9:
15:
17:
18:
30:
A<B.
A = B.
id.
id.
A<B.
id.
A = B
A<B.
A = B.
id.
A<B.
1897, January i
September 3:
8:
26:
30:
October 8:
11:
26:
28:
30:
November 4:
8:
- A>B. N.B.
id.
A=B.
id.
A<B.
A < B.Dislincl
A<B.
id.
id.
A = B.
A<B.
A=B.
66
January
February
March
May
August
Publications of the
S Ursa
8: S = f.
13: a little <f.
19: =g.
15: id.
11: =r.
17: a little > f.
20: > f.
31: <e.
i: =d.
9: id.
18: =f.
30: a little < g.
majoris,
September 3
4
8
26
October
30
8
26
28
November 4
faint.
id.
almost invisi-
ble.
id.
invisible.
almost invbi-
ble.
= f.
id.
January
February
March
May
August
T Ursa
8: T a little > a.
19:
11:
17:
20:
i:
9:
18:
30:
>a.
a little > a.
= b.
=^ e.
id.
id.
invisible,
id.
a little > e.
>c.
.<b.
majons,
September 3
4
8
26
30
8
26
October
28
November 4
7
a little > b.
id.
>b.
>a.
a little > a.
id.
<b.
>c.
almost = c.
= c
a little < c.
The Lunar Eclipse of February 28th.
7 16
30
33
38
40
42
44
48
55
8 9
P. M.
Shadow touching limb of Moon.
Shadow touching Sirsalis a. Heraclides.
Shadow touching Cap Laplace,
Shadow touching Plato,
Shadow touching Copernicus,
Shadow touching Gassendi East.
Shadow touching Gassendi West.
Shadow touching Mare serenitatis East.
Shadow touching Bessel.
Shadow touching Proclus.
Astronomical Society of the Pacific,
67
10
20 p. M. .
. . Shadow touching Tycho East.
46
(Maximum)
17
. . Shadow touching Grimaldu
43
. . Shadow touching Copernicus,
47
. . Shadow touching Heraclidcs,
52
. . Shadow touching Cap Laplace,
57
. . Shadow touching Plato East.
58.5
. . Shadow touching Plato West.
5
. . Shadow touching Aristoteles,
7
. . Shadow touching Proclus,
15
. . Shadow touching limb of Moon.
10
OCCULTATION OF THE PLEIADES,
m. s.
55 45 Immersion of Celeiio.
59 30 Immersion of Electra,
16 40 Immersion of Taygeta,
23 40 Immersion of Maya.
f Immersion of Asterope\
^ ^ \ Emersion of Electra,
53 40 Emersion of Celeno,
5 40 Emersion of Taygeta.
22 50 Emersion of Maya,
68
Publications of the
Shooting Stars.
NO.
Time, P. M. Beginning.
End.
Magni-
tude.
NOTK.
1896. 1
I
Aug.9.io>» 3" 30- 2374- 8
234- 3
9
2
8 Oj 1+29
1+29
^
3
10 20] 343+11
335+ 6
3
4
22 1 300+48 1 289+40
3
5
23 30
33
292+10 1 286+ 4
3
6
348+18 1 342+14
2
7
35
270+56 1 242+75
I
8
38 20
337+30 1 330+20
2
9
39 1 345+65 1 340+49
?
lO
42 1 292+ 3
291— 4
282+10
I
II
42 15 294+26
Fireball.
12
48 10 322+70 1 306+58
I
13
50
290+52 275+30
2
14
53 45
245+63 ' 206+58
2
15
58 10
298+50
344+43
288+42
3
i6
59 15
331+30
3
17
II I
303+20 1 294+ 5
2
i8
4 40
25+30 1 24+14
9
19
8
303+45 ' 287+29
3
20
II 10! 309—11
301—19
225+22
I
3
21
18 30
240+33
22
22 30
307—10 301—16
3
23
26
13+19 3+ 6
9
Train.
24
31 30
309—17 301—23
I
25
39 30
27+32 1 27+22
9
2
26
43 15! 288+10 284+
27
50 40 323— 7 ' 312—13
3
28
51 20 18+32 1 3+22
X(D
Fireball.
29
56 15 1 318+50 ! 304+40
2
30^
59 66+75 I 40+86
Time, A. M.
2
31
Aug.IO.I2 2 —1328+43 3'2+32
3
32
3 — 330+ 2
Time. P.M. |
322- 4
3
33
10 I 10 i 339— 2
331—14
%
34
2 50 341+40 \ 324+18
%
35
5 50 ' 295+61
270+34
9
I
Train.
36"
7 20 0+58
335+50
37
13 321+44
305+40
2
38
13 30 ' 323+ 9
310— 5
%
39
15 351 + 10 1 340— 5
%
40
18 30
332+56
310+44
I
Astronomical Society of the Pacific.
69
Shooting Stars — Continued,
No.
Time, P. M.
■ Beginning.
End.
Magni-
tude.
Note.
1
1896.
1
41
Aug.io.io»»2i»45" 10+40
359+23
2
1
42
25
40 10+25
6+19
I
43
33
40 10+37
19+40
3
44
35
263+36
243+12
9
45
39
258+39
244+23
2
46
44
45 1 303+ 2
295—13
2
47
47
15 ; 293+26
280+ 5
I
48
50
30 337+ 9
342—15
2
49
51
50 348+22
342 + 13
I
Train.
50
56_
57
50 50+70
64+73
I
51
35+29
31 + 19
2
52
59
50 303— 8
302—18
I
53
II 2
20 328—15
324-23
I
54
4
342+33
331+21
%
Train.
55
II
50 319— 5
V307— 14
9
I
Train.
56
14
50; 25+34
~l6+22
57
15
' 266+56
277+42
%
58
17
40+60
74+64
I
59
28
' 10+29
1+17
I
60
35
102+45
102+39
9
61
35
30 310+30
298+11
62
37
40, 29+16
25+ 6
%
63
42
346+
339-14
2
64
45
311+14
301— 2
2
65
45
20 20+27
42+30
2
Slow, undulated light.
66
58
10 16+46
4+36
?
Train.
67
12
26+19
21+ 6 j
I
68
Aug. 1 1 . 10 10
30' 185+50
195+34
I
69
II
148+50
175+29
2
70
16
40 1 183+34
190+22
I
I
71
24
501 3 « 6+33
292+20
72
27
20 337+37
318+22
I
Train.
73
32
20 1 339+75
319+59
4
74
45
10 170+80
160+75
3
75_
55
II 2
45 1 5+36
353+24
2
76
30 25+20
23+13
2
77
4
27+55
21+50
2
78
5
10+39
358+30
2
79
10
4+9
359+ 4
2
80
Aug. 12. 9 57
30I . . . .
70+70
2
70
Publications of the
No. 23 was also observed at Copenhagen (356^ -|- 30° -j — >
341°+ 1 8^ I Magnitude).
No. 28 was also observed at Copenhagen (290° -f" 57^ -f- - >
273°+ 42^ %).
No. 77 was also observed at Copenhagen (248° -|- 40^ -j — >
254*^4" 27°, I Magnitude).
These three meteors give the following results: —
No.
Beginning
End.
h
\ <f>
/i
A.
<A
/
/
/
/
23
120
East.
54 54
28
98
57
West.
55 32
77
107
I 17
West.
55 43
lOI
I 27
West.
55 25
Real Length
ot the Path.
P
Km,
35
Odder is situated in 2° 25' W. longitude from Copenhagen,
and 55^ 58' N. latitude, h and ^ indicate kilometres; \ is longi-
tude from Copenhagen; <^ is N. latitude.
Note. — This paper was accompanied by a drawing of five
phases of the occultation oi Jupiter by the Moon on 1896, June 14.
The drawing is not reproduced here. The radius of Jupiter is
taken as 9 mm, 2.5 mm, were obscured at 10** 42" 50'; 8.3 mm,
at io**43'"io'; 14 mm. at io*'43'"3o'. The middle time is that
of bisection, according to a late note from Mr. Kohl.
The Committee on Publication.
PLANETARY PHENOMENA FOR MAY AND
JUNE, 1897.
Bv Professor Malcolm McNeill.
May.
Mercury is an evening star until May 20th, when it comes to
inferior conjunction with the Sun. It passed greatest east elonga-
tion on April 28th, and during the first ten days of the month is
in very good position for observation, n(>t setting until nearly two
hours after sunset on May ist.
Astronomical Society of the Pacific. 71
Venus is now a morning star, having passed inferior conjunc-
tion on April 28th. It is too near the Sun to be seen during the
early part of the month, but its distance rapidly increases, and
after May loth it rises more than an hour before sunrise. On
May 1st, there is a very close conjunction of the Sun, Moon and
Venus; the Moon passes the planet at about 3 A. M., and the
Sun at I P. M. Of course, both Moon and planet are too near
the Sun to be seen.
Mars is still in the southwestern sky in the evening, but sets
an hour earlier than for the corresponding period in April, at a
little after 11 p.m. on May 30th. It moves about eighteen degrees
east and four degrees south during the month from the constella-
tion Gemini into Cancer, On the morning of May 25th, it
passes just south of the fifth magnitude star 17 Cayuri, the nearest
distance being only two minutes, but this is while they are below
our horizon. During the closing days of the month it passes
through the ** Beehive*' cluster in Cancer The planet has nearly
reached its maximum distance from the Earth, and it will not
diminish very greatly in brightness before reaching its minimum.
It passes aphelion on the night of May 21st
Jupiter is also in the southwestern sky in the evening, setting
after midnight It is in the constellation LeOy and during the
month it moves about two degrees east and forty minutes south.
At the beginning of the month it is about two degrees east of the
first magnitude star Regulus (a Leofiis).
Saturn rises at about sunset in the middle of the month,
coming to opposition on the night of May 17th. It moves west
in the constellation Libra about two degrees during the month.
At the beginning of the month it is about three degrees west of
the third magnitude star /3 Scorpii,
Uranus is quite close to Saturn^ about two degrees south. It
comes to opposition on the same' date as Saturn^ May 17th, but
about twelve hours earlier. Its motion is like that of Saturn^
but only about half as great.
Neptune is in the eastern part of the constellation Taurus^ too
close to the Sun for observation.
June.
The Sun attains its maximum declination at the summer
solstice, and summer begins June 20th, 8 p. M., P. S. T.
Mercury is a morning star, and reaches greatest west elonga-
tion on June 15th. It is several degrees south of the Sun, and
72 Publications of the
the conditions are not very good for visibility ; but after June loth
it rises at least an hour before the Sun, and it may possibly be
seen if the atmospheric conditions are very favorable.
Veiius is also a morning star, and is rapidly increasing its dis-
tance from the Sun, so that by the end of the month it has nearly
reached greatest west elongation. It reaches its maximum bright-
ness early in the month, and during most of the month it can be
seen in full sunlight without telescopic aid.
Mars sets about an hour earlier than during May, at about
ID p. M. on June 30th. It moves about seventeen degrees east
and six degrees south during the month, through the constella-
tion Cancer toward Leo, and at the end of the month is only
about two degrees west and north of Regulus (a Leonis), Its
actual distance from the Earth is about twice the mean distance
of the Earth from the Sun, and its brightness not far from its
minimum.
Jupiter is somewhat to the east and south of MarSy and moves
about four degrees east and two degrees south during June, in
the constellation Leo, away from Regulus, At the end of the
month it is ten degrees east and four degrees north of Mars,
Regulus lying between the planets and nearer Mars,
Saturn is now well above the horizon at sunset. It moves
about two degrees west in the eastern part of the constellation
Libra away from y3 Scorpii. The apparent minor axis of the
ring is four-tenths that of the major.
Uranus is just about two degrees south of Saturn, and
moving in the same direction, but more slowly. It is in con-
junction with Saturn on June 8th.
Neptune is a morning star, quite close to the Sun.
Explanation of the Tables.
The phases of the Moon are given in Pacific Standard time.
In the tables for Sun and planets, the second and third columns
give the Right Ascension and Declination for Greenwich noon.
The fifth column gives the local mean time for transit over the
Greenwich meridian. To find the local mean time of transit for
any other meridian, the time given in the table must be corrected
by adding or subtracting the change per day, multiplied by
the fraction whose numerator is the longitude from Greenwich
in hours, and whose denominator is 24. This correction is
seldom much more than i". To find the standard time for the
Astronomual Society of the Pacific.
73
phenomenon, correct the local mean time by adding the differ-
ence between standard and local time if the place is west of the
standard meridian, and subtracting if east. The same rules apply
to the fourth and sixth columns, which give the local mean times
of rising and setting for the meridian of Greenwich. They are
roughly computed for Lat. 40°, with the noon Declination and
time of meridian transit, and are intended as only a rough guide.
They may be in error by a minute or two for the given latitude,
and for latitudes differing much from 40° they may be several
minutes out.
Phases of the Moon, P. S. T.
New
Moon,
May I, ]
[2 46 p. M.
First
Quarter,
May 9,
I 37 P. M.
Full Moon,
May 16,
5 54 A. M.
Last
Quarter,
May 23,
I 34 A. M.
New Moon,
May 31,
4 26 A. M.
The Sun.
R. A.
Declination.
Rises.
Transits.
Sets.
1897.
H. M.
'
H. M.
H. M.
H.
M.
May I.
2 36
+ 15 15
5 4 AM
. II 57 A.M.
6
50 P.M.
II.
3 14
+ 18 I
4 53
II 56
6
59
21.
3 54
^^ 20 18
4 44
II 56
7
8
31-
4 34
+ 22
4 38
II 57
7
16
Mercury.
May I.
3 55
+ 23 5
5 54A.M
I 17 P.M.
8
40 P.M.
II.
4 9
+ 22 21
5 30
12 51
8
12
21.
3 54
+ 18 5r
4 49
II 56 A.M.
7
3
31-
3 39
+ 15 46
4 7
Venus.
II 2
5
57
May I.
2 12
+ 18 12
4 29 A.M
. II 33 A.M
.6
37 P. M
II.
I 56
+ 14 18
3 49
10 38
5
27
21.
I 54
+ 11 45
3 16
9 56
4
36
31.
2 5
+ 11 I
2 50
Mars.
9 ^8
4
6
May I.
7 30
+ 23 37
9 25 A.M.
4 51 P-M.
12
17A.M.
II.
7 54
+ 22 35
9 14
4 35
II
56 P.M.
21.
8 17
+ 21 19
9 3
4 19
II
35
31.
8 41
+ 19 51
8 54
Jupiter.
4 4
II
14
May I.
10 II
+ 12 33
12 48 P.M.
7 31 P.M.
2
14A.M.
II.
10 12
+ 12 25
12 10
6 53
I
36
21.
10 15
+ 12 II
II 34A.M.
6 16
12
58
31.
10 18
+ II 51
10 59
5 40
12
21
74
Publications of the
Sa turn.
1897.
R.
A.
Declination.
Rises.
Transits.
Sets.
H.
M.
'
H. M.
H. M.
H. M.
May I.
15
48
-17 39
8 1 2 P.M.
I II A.M.
6 IOA.M,
II.
15
45
— 17 30
7 30
12 29
5 28
21.
15
42
— 17 20
6 42
11 42 P.M.
4 42
31-
15
39
-17 II
6
Uranus.
II
4
May I.
15
42
— 19 26
8 14 P.M.
I 5 A.M.
5 56A.M
II.
15
40
— 19 20
7 32
12 24
5 16
21.
15
38
- 19 15
6 47
II 39 P.M.
4 31
3'-
15
37
- 19 9
6 5
10 58
3 51
Neptune,
May I.
5
II
+ 21 37
7 15 A.M.
2 32 P.M.
9 49 P.M.
II.
5
12
+ 21 39
6 37
I 54
9 II
21.
5
14
4- 21 41
5 59
I 16
8 33
31-
5
15
+ 21 43
5 20
12 38
7 56
Eclipses of Jupiter* s Satellites, P. S. T.
(Phenomena near right hand limb of planet as seen in an inverting telescope.)
III. D,
May
I.
H. M.
10 56 P. M.
II.
R,
May
9-
H. M.
10 47 p. M
III, R,
2.
2 16 A. M.
I,
R.
12.
10 8 p. M
II. R.
2.
8 1 1 P. M.
I,
R,
21.
6 31 p. M
IV, D.
3-
6 18 P. M.
II,
R,
27-
5 14 P. M
IV, R,
3-
10 21 P. M.
I.
R,
28.
8 26 P. M
I. R,
4-
I 44 A. M.
Ill,
R.
30.
6 I2P. M
I, R.
5-
8 13 P. M.
Minima of Algol.
The Sun is too near the star, and the star too near the horizon,
for convenient observation of minima.
Phases of the Moon» P. S. T.
H. M.
First
Quarter,
, une 7,
II 2 P. M.
Full
Moon,
une 14,
I I P. M.
Last
Quarter,
une 21,
3 24 P. M.
New
Moon,
^ une 29,
6 55 P- M.
The Sun.
R. A.
Declination.
Rises.
Transits.
Sets.
1897.
H. M.
c /
H. M.
H. M.
H. M.
June I.
4 39
+ 22 8
4 38 A.M
. II 58 A.M.
7 18 P.M
II.
5 20
+ 23 8
4 35
II 59
7 23
21.
6 I
+ 23 27
4 37
12 2 P.M.
7 27
July I.
6 43
+ 23 5
4 41
12 4
7 27
Astronomical Society of the Pacific.
75
Mercury.
A. R.
Declination.
Rises.
Transits.
Sets.
1897.
H. M.
•
H. M.
H. M.
H.
M.
June I.
3 38
+ 15
37
4 3 A.M.
10 57 A.M.
5
51 P.M.
II.
3 49
+ 16
4
3 33
10 29
5
25
21.
4 28
+ 19
4
3 21
10 23
5
35
July I.
5 34
+ 22
35
3 33
Venus.
10 54
6
15
June I.
2 6
+ 11
2
2 47 A.M.
9 25 A.M.
4
3 P.M.
II.
2 28
+ 11
51
2 27
9 8
3
49
21.
2 57
+ 13
32
2 10
8 57
3
44
July I.
3 31
+ 15
35
I 58
Mars,
8 52
3
46
June I.
8 43
+ 19
41
8 52 A.M.
4 2 P.M.
II
12 P.M.
II.
9 6
+ 18
8 43
3 46
10
49
21.
9 30
+ 16
7
8 34
3 30
10
26
July I.
9 53
+ 14
4
8 26
3 H
10
2
Jupiter.
June I.
10 18
+ 11
48
10 56 A.M.
5 36 P.M.
12
16A.M.
II.
10 22
+ 11
23
10 21
5 I
II
41 P.M.
21.
10 27
+ 10
52
9 49
4 27
II
5
July I.
10 33
+ 10
18
9 18
3 53
10
28
Saturn.
June I.
15 39
-17
10
5 56 P.M.
10 56 P.M.
3
56 A.M.
II.
15 36
-17
2
5 13
10 14
3
15
21.
»5 33
— 16
55
4 31
9 32
2
33
July I.
15 32
-16
50
3 49
8 51
I
53
Uranus.
June I.
15 37
-19
9
6 2 P.M.
10 54 P.M.
3
46 A.M.
II.
15 35
- 19
3
5 20
10 13
3
6
21.
15 34
- 18
59
4 39
9 32
2
25
July I.
15 33
- 18
55
3 59
8 52
I
45
Neptune.
June I.
5 15
+ 21
43
5 17 A.M.
12 35 P.M.
7
53 P.M.
II.
5 17
+ 21
45
4 39
II 57 A.M.
7
15
21.
5 19
+ 21
47
4 I
II 19
6
35
July I.
5 20
+ 21
48
3 23
10 41
5
59
Eclipses
or JupiTERs Satellites, P. S.
T.
(Phenomena near right-hand limb of planet as seen
in an inverting telescope.)
H. M
H.
M.
II, R,
June 3.
7 SOP-
M. I, R,
June 13.
6
45 P. M.
I. R.
4-
10 22 p.
M. I, R,
20.
8
41 P. M.
III. D.
6.
6 55 P-
M. II, R,
28.
4
50 P. M.
Ill, R.
6.
10 IIP.
M. I, R,
29.
5
4 P.M.
II, R.
10.
10 24 P.
M.
Minima of Algol.
The Sun b too near the star, and the star too near the horizon,
for convenient observation of minima.
76
Publications of the
EPHEMERIS FOR PHYSICAL OBSERVATIONS OF
THE MOON FOR CERTAIN DATES
BETWEEN 1890 AND 1896.
Communicated by Dr. A. Marth, F. R. A. S.
Note. — Dr. Marth has been so good as to compute the
following table, corresponding to times at which certain negatives
of the Moon have been taken at Mt. Hamilton with the thirty-six-
inch refractor. The times usually correspond to focal negatives
presented by the Lick Observatory to the Observatory of Prague.
The last entry refers to Map No. i of the Observatory Atlas of
the Moon, published by the Lick Observatory. It is Dr. Marth' s
intention to continue these computations. E. S. H.
"
1 Selenographical
Topocenlric
Apparent
Colony:. 1 Latit.
Libration.
Semi-diam
P.
Date.
29
Pacific S. T. 1
of the Sun.
Longit. 1 Latit.
of<CsDisc
1
1890, June
h. m. s. 1
10 10
63.70+0.40
—5.72-1.22
982.6
\ 8.40
10 23
63.81+0.40
—5-75— 1.20
982.7
8.37
July
20
7 53 1
319.23+0.88
—4.56-5.89
893-6
1 23.02
27
10 27 1
46.08+1.05
—7.56 0.00
978.9
\ 5-52
Aug.
31
14 27
115-43 4-1.51
+5.62+6.66
992.3
337.80
Nov.
16
5 53 1
•329.70+0.55
-2.49+4.88
973-2
1 349.29
17
6 835
342.01+0.53
—1.42+6.09
976.2
,34415
i89i,July
13
8 24 57
3.60+1. 13
—4.04—3.85
901.9
1 20.82
28
14 51 5.5
189.91 + 1.37
+6.59+1.88
955.1
1 346.87
Oct.
12
7 29 9 1
3397+0.97
—5.84+7.51
981.8
, 341.39
—
7 30 54.5,
33.98+0-97
-5.85+7.51
981.8
' 341.39
1892, Nov.
10
14 54 31
172 43— 0.35
+ 8.58—6.50
935.5
1 18.68
—
15 52 41 '
172.92—0.35
+8.43—6.49
937.0
18.76
1893, July
20
8 22 45
058+1.52
+4.64+1.92
903.1
' 18.47
23
8 27 53
37.25 + 1.52
+0.94+5.51
891.4
1 782
Aug.
3
15 23 13 ,
17493+1-44
—4.06—0.70
9726
1 341.46
—
15 30 45
174-99+1.44
—4.07—0.72
972.8
, 341.45
Aug.
29
13 13 48.5
J31.43+1 07
—3.77+1.25
966.7
343-33
Oct.
26
10 50 52 1
117.48— 0.41
+001— 4.13
1003.9
349.25
—
16 3 14 I
120.12 — 042
—0.27—4.60
1004. 1
1 350.03
t894, Nov.
8
10 16 52
45-27—1.14
-541+0.76
922.5
338 II
—
10 21 1.5'
4530— 1. 14
—5.42+0.76
922.4
1 338. 1 1
1895, June
27
8 21 1.5.
358.66+1.43
+3-68+1.00
982.6
1 2r.39
Aug.
2
10 I 36
59.41+0.86
+4.84+6.59
904.0
i 354.20
—
II 43 3
60.27+0.86
+4.46+6.48
902.9
353-98
II 44 41 1
60.28+0.86
+446+6.48
902.9
' 353.98
7
15 25 II 1
123. 10+0.73
—2.13+009
893.1
338.63
13
15 10 26 '
196. 2 1 +0.57
—7.01— 6.19
941.2
' 347-97
14
16 17 26.51
209.00+0.54
—6.83—6.46
957-6
1 353- 1 7
—
16 20 6.5
209.02+0.54
—6.84—6.45
957.7
,353- 18
Sept.
6
15 38 22 1
i29-57~o.o6
—4.80-3.82
903-1
' 338.81
Oct.
7
13 56 8
146.77-0.87
—5.81-6.45
933.9
1349-72
8
14 41 2
159.32-0.89
—5.94—6.48
943.9
1 355.00
9
16 20 2 1
172.34— 0.91
—5.96—6.12
956.0
1 094
16 36 20 1
172.48 — 0.91
— 6.or— 6.11
956.3
1 0.99
10
16 49 13.5
184.77-0.93
—548—5.34
967.6
1 6.69
Astronomical Society of' the Pacific.
11
The topocentric libration gives the selenographical longitude
and latitude of the point on the Moon's surface which occupies
the center of the disc, as seen from the Lick Observatory. P.
denotes the position-angle of the Moon's axis, reckoned from
the apparent circle of declination.*
REVIEW OF SOLAR OBSERVATIONS, 1895 (AUGUST-
DECEMBER) AND 1896.
Bv David E. Hadden.
The following solar observations are a continuation of those
communicated to the Society for the years 1891 to June, 1895,
and published in Vol. VII., No. 45, of the Publications,
The instrumental outfit used has remained the same, viz. : a
three- inch equatorially mounted telescope, and a grating spectro-
scope of 14,438 Hnes to the inch.
During the year 1896 the appearance and approximate position
and size of each sun-spot group and facula have been sketched
daily on sheets of paper containing a three-inch ruled circle,
divided into quadrants, the east and west line being set parallel
with the Sun's apparent motion, by allowing the limb of Sun*s
image to move tangent to the horizontal spider-line in the eye-
piece; the observations are afterward properly corrected for posi-
tion angle of the Sun*s axis and inclination to the ecliptic. By
this means an approximate position of the latitude and longitude
is obtained.
Complete observations and detailed descriptions of the results
have been published in the Monthly Review of the Iowa Weather
and Crop Service,
The following tables exhibit the summaries of these observa-
tions: —
RESUMfe OF SOLAR OBSERVATIONS.
1895.
Number of
Mean Daily Number of
Months.
Days. !
Groups.
Spots. !
Faculae.
July
3 1
. ,
August
22 1
4.7
439
2.9
September ....
19 ,
51
22-3 ,
2.8
October
20
4.6
35.5
3.3
November ....
16 1
3.9
16.2
2.9
December ....
17 i
6.3
.7..
2.9
• For a continuation of this article see the Notices L. O.
78
Publications of the
1896.
9
3.2
8.5 i
3-2
18
3.8
24.0
2.5
16
3-7
14.8 •
2.6
17
3.7
21.8
3.2
18
23
10.7
25
16
3.0
231
2.3
23
3.8
15- 1
2.7
20
2.2
10.7
2.6
17
2.9
31.2
3.3
21
2.8
12.9
2.6
12
3.6
16.0
3.2
10
4.0
24.7
3.6
January .
Febnury .
March . .
April . . .
May . . .
June . . .
July . . .
August . .
September
October .
November
December
The steady decline in number of groups and spots noted as
having set in during 1894 and the first half of 1895 has continued
during the period under review, several days without spots being^
noted in April, August, and October, 1896. Among the larger
and more noteworthy groups observed may be mentioned the
following: —
August. 1895. — Several large and interesting groups from ist
to 14th. On the 27th, a fine, single spot, with double umbra,
appeared at the east limb and completed the transit of the disc,
disappearing at the west limb on September 9th, and reappearing
again by rotation at the east limb on September 23d, and once
again completing the transit; its umbra was quite interesting
from day to day, at times being single, double, round, irregular,
and curved. Other large groups were noticed during the closing
days of September and fore part of October, and again during
the third decade of that month.
On September 24th, a fine, bright protuberance was observed
on the east limb.
On October 1 2th, a large stemmed prominence was on the
west limb, near a group which was disappearing by rotation.
On October 20th, faint reversals and distortions of the Ha
line were observed on the east edge of the large east group of
spots.
November ist to 9th, large groups and spots dotted the disc.
December 20th to close of the month, a number of fairly large
and very interesting groups crossed the disc.
The following synopses of my observations for each month of
the year 1896 are reprinted from the Iowa Monthly Weather
Review: —
Astronomical Society of the Pacific, 79
January^ /S^, Sun-spots were few and small during the month of
January, but three groups made the entire transit of the disc from east
to west during the period, and nearly twice as many groups were noted
in the southern as in the northern hemisphere.
February, j8g6. The sun-spots for the first half of February, 1896,
were small, but during the latter half two especially fine and interesting
groups made the transit of the disc. Twice as many groups were noted
in the north as in the south hemisphere in the first half of the month,
while during the latter half there was a slight increase in favor of the
southern.
March, i8g6. The total number of sun-spot groups noted during
the month of March, 1896, was about the same as for the preceding
month, but they were smaller and contained a less number of spots.
But three groups made the transit of the disc, the remaining groups
being of a very transitory character; the average life of all groups visi-
ble was 2.8 days per group. A fairly large group appeared on the 26th,
but after passing the central meridian about April ist, it seemed to be
fading out in small spots.
April, j8^. The average daily number of sun-spot groups for the
month of April, 1896, was about the same as for the preceding three
months, but the individual spots were much smaller. But one fairly
large group was noticed during the month, namely, on the loth.
From the 14th— the date of next observation — until the i8th, the
Sun's disc was free from dark spots. This is the first time since August,
1891, that the disc has been entirely clear. A minimum also occurred in
November, 1895, when a few days were noted in which but one very
faint group was present.
From April 20th to 26th the groups were all small and transient.
The average daily number of groups was about the same in both
northern and southern hemispheres during the month.
May, j8g6. Sun-spots during the first twenty-five days of May, 1896,
were few, small, and uninteresting. On the 26th. an extensive group of
small spots suddenly appeared, which rapidly increased in size and
activity, and at the close of the month was a very conspicuous group of
much interest.
Compared with the preceding four months of the year, there was a
decided falling-off in the daily average number of groups, spots, and
faculae, evidence of the approaching minimum of solar activity.
June, i8g6. Large and interesting groups of spots were visible on
the solar disc during the entire month of June, 1896, with the exception
of a day or two about the 20th, and the three closing days of the month.
The average number of groups was three per day, 2.1 of which were
observed in the southern hemisphere. Five groups made the entire
transit of the disc, while one originated on the visible side and com-
pleted the transit during the month.
July, i8g6. Sun-spots for the first eleven and last eight or ten days
of July, 1896, were few and small. On ihe 12th, a large spot appeared
at the southeast limb, which completed the transit of the disc and dis-
8o Publications of the
appeared at the west limb on the 25th. This group was the most im-
portant one of the month, and proved quite interesting, undergoing
many changes from day to day. Another group appeared on the north-
east limb on the 14th with indications of much activity; it rapidly
increased in size in the next few days, but had entirely disappeared when
near the central meridian on the 2olh. As in the preceding two months,
the southern hemisphere was the region of greatest frequency of spot
groups. But three groups completed the entire transit of the disc from
east to west during the month.
August^ i8g6. The daily average number of sun-spots visible during
the month of August, 1896, was the lowest so far in the present year,
being but 2.2 per day. Five groups completed the transit of the solar
disc from east to west during the month. The principal group of the
month appeared by rotation on the 9th — a large, well-defined circular
spot with nucleus and penumbra, which changed but little during its
transit. On the three closing days of the month, several new and fairly
large groups appeared, which were of interest. The southern hemis-
phere was again the location of greatest frequency of disturbances.
Sep ember, 1896. Sun-spots from September ist to 8th were few and
small. On the 9th, a fine extended stream of spots appeared at the east
limb and made the transit of the disc. It was one of the longest groups
observed in many years; owing to cloudy weather, but few observations
of it were possible; before reaching the west limb it rapidly became
smaller, the spots breaking up and fading out, not to reappear again by
rotation at the east limb. The southern hemisphere continued to be the
region of greatest frequency of spot groups during the month.
October, i8g6. Sun-spots during the first half of October were very
few, no spots being seen on the 5th. From the i8th to the close of the
month, several small groups made the transit of the disc. The southern
hemisphere continues to be the location of greatest spot frequency.
November, 1896. Sun-spots during the month of November, 1896,
were few and small, with the exception of a fairly large and interesting
group, which made the transit of the disc from about the 2d to 14th, but
of which only a few observations could be obtained, owing to the cloudy
weather. As in the preceding six months, the southern hemisphere
still continues to be the region of maximum spot frequency.
December, 1896. During the first half of the month of December,
1896, sun-spots were few and unimportant. During the latter half of the
month, one group rapidly increased in size and made the transit of the
disc, but was on the wane before disappearance at the west limb. The
southern hemisphere still continues to be the predominant region of
spot disturbances.
Notwithstanding the fact that during the year 1896 the period
of minimum of solar activity had set in, several very large and
unusually fine groups of spots appeared during the year. A
brief description of some of these is given here. A reference
number is given to every group each month.
Astronomical Society of the Pacific. 8i
February, 1896.— Groups Nos. ii, 14, 15.
February 20, No 1 1 : a small single spot with penumbra near west
limb; this was an interesting group, first appeared on loth at east limb
as a couple of small spots, soon enlarged, and was quite conspicuous
from 14th to i8th, undergoing many changes from day to day, and pass-
ing over the west limb as a small spot again. No. 14: a quite prominent
group, three large spots. No. 15: a new, fine, large group on east limb,
about twenty degrees south of equator; it consists of a large penumbra,
with double nucleus, the nuclei being connected by a narrow line of
umbra; the nucleus on west side is crossed by a " bridge "; many faculae
surround the group, and many small spots are in its vicinity.
February 21, No. 14: a train of large spots, with two large leader
spots. No. 15: a very fine, large group, still having the nuclei connected
by a narrow dark line.
February 23. No. 14: this group is a superb object; it is fully one-
tenth of the apparent diameter of the Sun in length, and consists of three
fine large spots. Each of the first two spots contains double nuclei, and a
** bridge *' was noticed crossing a portion of the umbra of the second
spot. No. 15 is also a very interesting and superb group; the large
leader spot has triangular umbra in nearly round penumbra; this is
followed by a larger, somewhat rectangular penumbra containing a series
of small spots; many small spots and penumbral matter are also in vicin-
ity. A group of four fine prominences was observed on west limb; one
large banyan-tree-like form was quite interesting.
February 24, No. 14: still a fine object; umbrae of both leader spots
greatly changed. No. 15: umbra of leader spot also much changed.
February 2$- No. 14: about same; umbra of leader spot is getting
large. No. 15 is more extensive; is now about on the central meridian;
multitude of small spots in its vicinity.
February 26. No. 14: the umbra of the leader spot is still enlarging,
and now crossed in center by a narrow *' bridge"; this group is yet a fine
object. No. 1 5 also contains a most interesting group; the nucleus of the
leader spot is nearly round, and that of the next spot long and narrow,
while the third spot contains a somewhat crescent-form nucleus.
March, 1896. — Group No. 21.
March 26. No. 21: a new group of two fine large spots, each with
well-developed nucleus and penumbra; the west spot has three nuclei,
the east, one with an elongated nucleus. A very extensive facula region
appeared by rotation at the east limb.
March jo. No. 21 is now a litile east of meridian, and is a little
smaller; the leader, or west spot, has extensive penumbra, with one large
nucleus and numerous small nuclei; the following spot has divided into
two distinct spots, each with penumbra.
April, 1896.— Group No. 8.
April 10. No. 8: this is probably No. 6; it has changed decidedly
since last observation. It is a very fine group in the northwest quadrant,
82 Publications of the
consisting of a large penumbral area, containing a double umbra; a small
spot is on following side, its nucleus being crossed by a ** bridge"; many
small spots are in its vicinity. A " veiled " group was noticed a little
east of the central meridian, in south latitude.
May, 1896. — Group No. 12.
May 26. No. 12: new group of many small spots, which formed since
yesterday, little south of equator, about three days from east limb, with
slight penumbra around two spots. No. 13: new small spot, east limb.
May 28. No. 12: great activity in this group; it now has a large oval
penumbra, with one large and several smaller nuclei; this is followed
in immediate vicinity by a number of small spots, some with slight
penumbra.
May 2g. No. 12 is a fine, much more extensive group to-day. The
penumbral area is increasing, but breaking up somewhat; the main
nucleus is larger and elongated; a large number of small spots, some
with penumbra, are following this group. Much solar disturbance is
manifest.
May JO. No. 12 is still a fine group; the nuclei seem to be coalescing;
much penumbra surrounds and follows the group.
June, 1896.— Groups Nos. ii, 12.
June 24. No. 11: on the central meridian to-day, is increasing much
in activity; the leader spot has umbra which app)ears to be dividing; this
is followed by a large area of penumbra and numerous small spots. No.
12: a new group in southwest quadrant, very extensive, containing a
large leader spot and followed by many small spots.
June 2^. No. 11: new small spots appearing on east side of group.
No. 12: about the same as on yesterday, except not as many small spots
in vicinity.
June 26. No. it: the group is breaking ^p, the leader spot has
divided into two parts, each with penumbra; a "bridge** is across the
umbra of the large west spot. No. 12: the umbra of leader spot is oval;
the penumbra does not entirely surround it, apparently being overlaid
by facula on its east side.
June 27, No. 11 is fast diminishing in size and breaking up. No.
12: the leader spot is now on edge of west limb; its nucleus has penum-
bra on north and south, but not on east or west sides.
June* 28. No. 11: only a few spots left, with a trace of penumbra.
No. 12: but a dot left on extreme edge of west limb; group disappearing
by solar rotation. Very fine prominence was observed on southeast
limb at 1:20 p.m.; portions of it attained a high altitude, but at 2:20 p.m.
had greatly changed, and at 3:25 p.m. no floating cloud forms were seen,
and prominence was more quiescent; also prominences on west limb^
one of which was pyramidal in form.
July, 1896.— Group No. 12.
July 12, No. 12: fine new spot with double umbra on edge of
southeast limb, penumbra partially visible on west edge of lower
Astronomical Society of the Pacific. 83
nucleus, but not on west edge of upper one, and is visible on all other
sides of both nuclei. A fine aurora last evening. A bright group of
prominences was directly over the group on limb.
August, 1896.— Group No. 13.
August so. No. 13: a new group on east limb, with two nuclei in
large facula. A very fine group of prominences was observed on the
west limb at 3 p.m., also smaller one on east limb.
September, 1896.— Group No. 6.
SepUmber //. No. 6: a very fine train of spots well in, on east limb in
north latitude; about fifteen nuclei were counted in the extended penum-
bra; several portions are detached and of a semi-circular form; the group
is inclined about fifteen degrees, or more, toward the equator.
September ij. No. 6: this is a magnificent group to-day; it has
greatly increased in size, length and interest; fully thirty nuclei are in-
cluded in the long detached groups of penumbral nebulosity which still
has the semi-circular form in numerous portions.
September 16. No. 6: this great group is almost exactly bisected by
the central meridian to-day; several transits of the group were taken to
estimate its length, which was found to be about 190,000 miles.
September //. No. 6: the fine group continues about the same, but
segmentation of the spots has set in.
September /p. No. 6: the group is breaking up somewhat; the fol-
lowing spots are thinning and fading out.
September 20, No. 6 is now breaking up; it has two irregular
penumbral areas, one with a large nucleus and the other containing two
nuclei; the smaller spots are fading out.
September 22. No. 6: but a couple of small spots left of this group
which is disappearing by solar rotation.
October, 1896.— -Group No. 16.
October 23, No. 16: a spot on extreme edge of east limb, south of
equator, near which place, at 11:55 a-^* ^o 12:30 p.m., an intensely bril-
liant small prominence was observed; a detailed account of this phe-
nomenon was published in Popular Astronomy for December, 1896.
October 2 i. No. 16: a well-defined, medium-sized spot, with penum-
bra, which is not visible on west side of umbra yet.
October 2$, A very fine group of prominences on west limb; one
large, feather-like prominence and several smaller ones; the larger one
was fully 90,000 miles in height. See my account of it in Popular
Astronomy for December, 1896.
November, 1896. —Group No. 3.
November 4, No. 3: fine, large spot, one day in, on east limb in
south latitude; has a nearly circular penumbra with umbra, the umbra
being divided by a semi-circular streak of light.
84
Publications of the
November 5. No. 3: only a faint streak of light crossing umbra
to-day.
November 11. No. 3 is now in southwest quadrant Cloudy
weather prevented any observations of this fine sp>ot since the 5th; the
umbra is somewhat oval, and the entire spot larger.
November 12. No. 3: the umbra is more ** triangular*' in form
to-day.
November ij. No. 3: penumbra is not visible on west edge of
umbra to-day.
November 14. No. 3: this fine spot is now on edge of west Jimb;
the penumbra is not apparent on either east or west edges of its umbra.
December, 1896.— Groups Nos. 8, 15.
December 15, No. 8: group of about fifteen small spots a little east
of meridian, several having penumbra.
December 18. No. 8 is larger, and consists of five or six spots, with
penumbra, some with several nuclei.
December ig. No. 8: three spots have three or more nuclei each;
No. 15: minute spots northeast.
December 22. No. 8 is now disappearing at west limb by solar
rotation. No. 15 has developed into a fairly large group; has one fine
leader-spot, with broken umbra in a somewhat circular penumbra, and
followed by a compact group of small spots.
The following table gives the maximum and minimum number
of sun-spot groups observed on any day for the months and
years indicated: —
1 Maximum Daily Number of
Minimum Daily Number of
Months.
Sun-spot Groups.
Sun-spot Groups.
' 1895.
1896.
1895. 1896.
January '
6
. . I
February
6
I
March . .
1
5
I
April . .
7
May . . .
4 '
1
I
June . . .
• • 5
2
July . . .
• • 9
I
August
8 5
2
September
9 6
2
I
October .
8 6
2
November
6 6
I
2
December
II 8
' I
2
Alta, Iowa.— Latitude 42® 40^ N.
Longitude 6** 2i'» W.
Astronomical Society of the Pacific. 85
PREDICTIONS FOR THE SOLAR ECLIPSE OF JULY
29, 1897, LICK OBSERVATORY AND
SAN FRANCISCO.
By C. D. Perrine.
The eclipse of July 29, 1897, which is visible in the tropics as
an annular eclipse, is visible in the United States as a partial one.
I have computed the following circumstances for the Lick Ob-
servatory and San Francisco — the Davidson Observatory — from
the elements of the eclipse given by the American Ephemeris,
taking into account the altitude in the computations for the Lick
Observatory. The altitude in this case has nearly the maximum
effect at the time of first contact, and makes a difference of about
1.5 seconds.
Prediction for Lick Observatory,
Eclipse begins 5** 25" i* a.m., P. S. T.
Greatest obscuration 6 14 44
Eclipse ends 7 921
Amount of greatest obscuration .... 0.387 of solar diameter.
Position-angle of beginning 246° 37'
Position-angle of ending 140 15
Prediction for Davidson Observatory ^ San Francisco,
Eclipse begins S** 26" 23' a.m.. P. S. T.
Greatest obscuration 6 15 21
Eclipse ends 7 8 27
Amount of greatest obscuration .... 0.386
Position- angle of beginning 245° 19'
Position-angle of ending 141 30
(Position-angles are reckoned from the north point through
the east)
February 19, 1897.
86 Publications of the
MAXIMUM OF o CeH (Mira), 1896-97.
By Miss Rose O'Halloran.
In the following observations a record of minute gradations
of lustre has not been attempted, but merely a careful outline of
the distinct changes, relatively to the comparison stars used
during the intervals of clear weather.
Sept. 25, midnight. Not more than one magnitude brighter
than companion, no" distant; in the moonlight alike
in tint.
26. 1:30 A.M. Ditto; seen near meridian.
Oct. II. More than one magnitude brighter than companion.
20. Ditto; noticeably reddish.
27. Ditto.
28. Visible in opera glass of mean power.
Nov. II. Equal to 71 CV//, about 2° to the east.
13. Ditto.
24. Visible to the naked eye; equaj to 70 Ceti; a few
degrees to the north.
25. Ditto.
28 and 29. Brighter than 66 CV//, i J4° to the northwest.
Dec. 2. About as bright as i Piscium,
5. Brighter than i Piscium,
6. Ditto.
7. About one magnitude less than 8 Ce(i\
8. Somewhat brighter than before.
19. Equal to h Celt,
21. Brighter than 8.
24. Ditto; not as bright as y Ceti,
30 and 31. Equal to 8.
Jan. I and 2. Ditto.
5, 6, 7, 8. Less than 8.
9. Brighter than 8; perhaps owing to moonlight.
14. About equal to 8.
Astronomical Society of the Pacific. 87
Jan. 1 5. Fainter than 8, even in the moonlight.
17. Fainter than 8.
22, 23, 25. Ditta
Feb. I. Ditto.
7. About half a magnitude fainter than 8.
21. Equal to i Piscium,
22. Ditto.
23. Not so bright as i Piscium.
24. Ditto; brighter than 70 Ceii.
25. 26, 27. Ditto.
Mar. I, 2, 4, 5, 8, 9, 10.^ Ditto.
1 1 and 1 2. Doubtful.
18. Fainter than 70 Ceii,
20. Ditto. In opera glass about equal to 66 Ceti,
No satisfectory comparisons could be made after this date,
though the variable was observed until March 25th.
San Francisco.
VV. C. BOND.
Astronomical Society of the Pacific. 89
NOTICES FROM THE LICK OBSERVATORY.*
Prepared by Members of the Staff.
Photographs of Donati's Comet in September, 1858.
A letter from Professor G. P. Bond to Mr. R. C. Carring-
Tox. dated April 4, 1859, states that a photograph of Donati's
comet was obtained at the Harvard College Observatory on
September 28, 1858. The exposure was 6", and the plate
showed the nucleus and a little nebulosity, fifteen seconds in
diameter. (^Annals H. C. O., Vol. Ill, p. 210.) In his reply of
May 26th, Mr. Carrington sends another photograph of the
comet to Bond, taken on September 27th by ? ? ? with an
exposure of seven seconds, using a camera lens (I infer that it
was a jx)rtrait lens of some ^\^ inches in aperture), which shows
much more nebulosity. Carrington' s enclosed photograph is
not now to be found, I believe. The photograph was unknown to
Dr. De la Rue. apparently (see Monthly Notices, R. A. S.,
Vol. XIX, p. 353). Both these photographs — the first ever made
of comets — have remained unnoticed by all the historians of
astronomical photography, up to this time, so far as I know.
E. S. H.
Search for Comet, or Comets, Reported by Dr. Swift,
September 2oth.
On September 21, 1896, a telegram from Dr. Swift was
received here as follows: "Last night, at sunset, object as bright
as Venus one degree east of Sun.*'
That afternoon, with a Herschel prism applied to the twelve-
inch telescope, I examined the region immediately about the
Sun, and then with a low-power eye-piece, for several degrees on
• Lick Astronomical Department of the University of California.
90 Publications of the
every side of the Sun, without finding the object. As the Sun
set, I again searched north, south, and east of it, and the next
morning as it arose, north, south, and west of it, without success.
For several mornings and evenings Mr. Perrine searched
with the comet-seeker the region for many degrees about the
Sun. W. J. HusSEY.
Bright Fire-Ball, January 26, 1897 (Mt. Hamilton).
At o** ii" 44" A.M., P.S.T., a brilliant fire-ball fell slowly from
Orion^ almost vertically — inclining a litde towards the south.
It burst into several pieces just before disappearing, but left no
persistent train. It presented quite a sensible disc, and was
several times as bright as Venus 2X her brightest — lighting up
the sky noticeably. C. D. P.
The Metric System.
** President Kellogg submitted the following: A communica-
tion urging active measures to secure the adoption of the metric
system. Professor George Davidson asks the signatures of
our Regents and Faculty in its favor. Regent Houghton oflfered
the following resolution:
Resolved, That the Board of Regents of the University of California
fully indorse and recommend the passage of the bill now before
Congress to adopt the metric system of weights and measurements, as
provided in H. R. 7251 of ist Session of 54th Congress." [Adopted
April 14, 1896.] — Report of the Secretary of the University of California,
189S-6.
Erratum in No. 53 of the Publications, A. S. P.
In the Publications, Volume VIII, page 328, line — i^,/or
AuvvERS read Ambronn, or Anding. (A. A.)
HoENE Wronski.
Most readers of mathematical astronomy have at some time
in their lives met with a paper by Villarceau: Mecaniqiu
Celeste; Expose des Methodes de Wronski, Attracted by the
name of Villarceau, they may have spent more or less time
over it; but finally all must have left it, uncertain whether the
unknown Wronski was '*a charlatan, a madman, or a genius."
At rare intervals the name of Wronski would recur to the
Astronomical Society of the Pacific. 91
memory, accompanied by the uneasy feeling that the remaining
doubt in his regard had not yet been settled. M. J. Bertrand,
Perpetual Secretary of the Paris Academy of Sciences, has lately
taken a review of the whole of Wronski's work,* and makes it
very clear that he was neither genius nor charlatan, but simply
insane. **His madness explains his charlatanism, excuses his
imposture, and permits one to believe in the presence of genius
imprisoned in insanity.'* After reading M. Bertrand* s paper,
few will doubt his conclusions. E. S. H.
Portrait of William Cranch Bond (Director of the
Harvard College Observatory, 1840-1859).
The portrait of Professor W. C. Bond given in this number is
reproduced from a photograph of the oil painting now in the
Harvard College Observatory. It forms one of the illustrations of
a life of BoND,t which will shorriy be printed; and is presented
to the A. S. P* by the undersigned.
Edward S. Holden.
Mt. Hamilton, February 28, 1897.
Meteor of January 24, 1897 (Los Angeles).
Los Angeles, Cal., March 5, 1897.
Professor Holden,
Lick Observatory, Mt. Hamilton, Cal.
Dear Sir: — On January 24th, at about 3:15 p.m., I observed
a very large meteor, which passed over this place and, as near as I
am able to judge, in a direction nearly due east. Unfortunately,
I did not note the exact time of its appearance, and am not able
to state the time positively, though from other circumstances, I
am able to locate it as being about the time mentioned above.
The meteor was visible sufficiently long for me to make a good
observation of it. Its movement was, as before stated, nearly
due east. Its apparent height was about thirty degrees above
the horizon when first observed. At its disappearance it was
approximately twenty-three degrees to twenty-five degrees above
the horizon. Its color was a dazzling white, with a faint tinge of
* Rruur des Deux Monde s. Vol. 139, p. 588.
t Memorials of William Ckanch Bond, Director of the Harvard College Observatory,
1S40-59, and of Gborgb Phillips Bond, Director of the Harvard College Observatory,
1&59-65, by Edward S. Holden.
92 Publications of the
blue. No train of smoke or fire followed, excepting a sheet of
flame, giving the meteorite an elongated appearance. I should
be pleased if you would forward me any notices you may have
from other sources where this meteor has been observed, and
greatly oblige, Yours very truly,
S. J. Reese.
Mr. Lowelj^'s Observations of Mercury and Venus.
The Monthly Notices of the Royal Astronomical Society for
January, 1897, contains plates of drawings of Mercury 2SiA Venus,
made by Mr. Lowell at the Flagstaff Observatory in 1896.
The markings on Mercury were "at once conspicuous'* with the
new twenty-four-inch object-glass; those on Venus are *' perfectly
distinct and unmistakable." The undersigned has made a con-
siderable number of observations of Mercury in the years 1873-
1885, and a very large number of Ventis in the years 1873-1890,
with telescopes of six, sixteen, twenty-six, thirty-six inches in
aperture, without ever once seeing markings of the character
depicted by Mr. Lowell. Other markings of the class drawn
by ScHiAPARELLi and many other observers, have, on the other
hand, been seen and recorded whenever the conditions of vision
were good. I have no hesitation in saying that such markings
as are shown by Mr. Lowell did not exist on Venus before 1890.
It is my opinion that they do not now exist on the planet, but
that they are illusions of some sort. Their general character*
is what would be shown if the adjusting screws of an objective
were set up too tightly, producing a set of strains in the glass, or
if the objective were strained by its cell. Strains of this sort will
produce faint companions to stars sufficiently bright. A com-
parison of all the drawings of Venus available in the library of
the Lick Observatory is very instructive. All observers, except
those at Flagstaff, see faint markings of one class; while those
drawn by Mr. Lowell are of a totally different nature.
Venus has been observed on very many occasions at Mt.
Hamilton, with our essentially perfect twelve-inch object-glass, in
the years 1 888-1 897, without once seeing markings of the kind
drawn by Mr. Lowell, or "distinct" markings of any kind.
Faint and indistinct markings, of the character of those drawn by
scores of observers for a century past, are, however, seen when
the circumstances are good.
•Six or more radial rays, thicker at the outer rim of the image of the planet.
Astronomical Society of the Pacific, 93
The foregoing notes seem to me to throw doubt on the
reality of the markings reported from the Flagstaff Observatory.
Until Mr. Lowell's observations are fully confirmed by other
observers with other telescopes, it will be wise not to accept them
unreservedly. Edward S. Holden.
Mt. Hamilton, March 9 1897.
Measures of
^ DF.i.PHfsi, /3 151
Date.
/>.
S.
1896.828
350^.9
o".45
•839
351 -8
.50
.877
354 -4
.53
1896.85
352°. 4
o".49
These measures were made with the 36-inch telescope, using
powers of 1000 and 1500. On each night the star was close to
the meridian, and the seeing was good. No third star was seen,
though carefully looked for on each night with powers from 350
to 1500. R. G. AlTKEN.
Mt. Hamilton, March 24, 1897.
First Results from the Bruce Photographic Tele-
scope AT Arequipa.*
The Harvard College Observatory Circular, No. 15, (December
30, 1896,) is devoted to the Bruce photographic telescope (now
in use by Professor Bailey at Arequipa), and accompanied by
three maps showing the splendid results which this telescope will
give. It is essentially a huge portrait lens (doublet) of twenty-
four inches aperture and 135 inches focus. These dimensions
give stellar maps on a scale of i'= i mm. This scale has the
advantage of being the same as that of the seventy-two charts
made visually by Chacornac at Paris, and of the twenty charts
made in the same manner by Peters at Clinton. f The Inter-
national Stellar Charts are made with telescopes of 0.33 m. (13.4
inches) aperture, and 3.43 ;w. (134 inches) focal length. Their
scale is therefore essentially the same, but they are subject to a
material disadvantage in comparison with the Bruce telescope.
The field covered by the International telescopes is about four
•Sec Publications A. S. P., Vol. V., pp. 82 and 186.
f The focal length which will give i' = i mm, is 3.438 w.
94 Publications of the
square degrees, whereas the Bruce telescope (a doublet) covers
about twenty-five square degrees (14x17 plates are used). The
exposures for a given magnitude are materially shorter for the
latter instrument. These advantages have been pointed out by
Professor Pickering at various times and places in the years
1883-87. In 1889, Miss Catherine W. Bruce, of New York,
generously provided the means to carry out the suggestion of
Professor Pickering. Mr. Alvan G. Clark undertook the
very difficult task of making the objective, and in 1896 the
complete telescope was mounted at Arequipa.* The maps
accompanying the H. C. O. Circular are wonderfully fine, and
show that the plan adopted for this powerful instrument has been
completely successful. The Bruce telescope is provided with
an objective prism for photographing stellar spectra; and the
preliminary results with this, also, are entirely satisfactory. It
appears that Professor Pickering has abandoned his original
scheme of making a complete photographic map of the whole sky
with this instrument, and intends to leave the map to the Inter-
national Photographic Congress. The Bruce telescope is to be
employed, at least for the present, on maps of special regions and
upon spectrum photography.
Miss Bruce and the Harvard College Observatory are to be
congratulated upon the splendid success of a daring experiment.
E. S. H.
Elements of Descriptive Astronomy: a Text-book. By
Dr. Herbert A. Howe, Director of the Chamberlin
Observatory, Denver. Boston: Silver, Burdett & Co.,
1897, 8vo, pp. 340, with 195 colored, and other, plates and
figures, star-maps, etc., etc.
[Reviewed by Edward S. Holden.]
There is always room for a good text-book of descriptive
astronomy, and the present volume will be welcomed by teachers
in high-chools, and by those who wish to give a general course
to college students without going into the more technical details
of the subject, while insisting on a full treatment of principles and
an accurate account of the present state of knowledge.
Professor Howe has, as might be anticipated, furnished a text
* a pair of telescopic doublets of i6 inches aperture is now being made by Mr.
Brash EAR for Professor Max Wolf at Heidelberg. See Publications A. S. P., Vol.
VII., p. 285.
Astronomical Society of the Pacific. 95
embodying the most approved methods of teaching, as well as
the most recent conclusions and findings of astronomers. His
successful experience as a teacher of astronomy is manifest, not
only in the plan of the book and the logical way in which it is
developed, but also in his apprehension of the student* s diffi-
culties, and the helps over hard places which he affords. The
many illustrations have been carefully chosen with a view to
throwing light upon all phases of the subject In typography,
etc., the book is very successful.
The book is not without interest to the professional astronomer,
also, as it brings the history of each subject down to the present
time. With regard to the canals of Mars, for example, about
which so much nonsense has been written, what summing up
could be more happy than the following? **The majority of
astronomers, while freely admitting the existence of the markings
called canals, are inclined to be conservative with reference to
any explanation of their nature. It has been aptly said, that it is
better not to know so much, than to know so many things that
are not so.**
Mt. Hamilton, March lo, i8st7.
Portraits of Astronomers and Others Belonging to
THE Lick Observatory.
The Lick Observatory possesses a large number of portraits
of astronomers and others, most of which are preserved in
albums. Some of the larger photographs and engravings are
framed and exhibited in the long hall of the Observatory or in
the library room — Adams, Airy, Bailly, Bradley, Bessel,
Bond, Bowditch, Cayley, Chauvenet, the Clarks, the
Drapers, Galileo, Gauss, Gould, Helmholtz, the Her-
schels, Kelvin, Kepler, Kronecker, Lick, Maxwell,
MicHELSON, Newcomb, Newton, Rutherfurd, Stokes,
Struve, Sylvester, and others.
Portraits of the Regents and other officials of the University
of California are included in the collection.
The photographs are derived from various sources: first,
from gifts to the Observatory from many living astronomers, in
answer to a circular of request; second, from a large collection
presented by the undersigned; third, from miscellaneous sources.
The thanks of the Observatory are returned to all those who
96
Publications of the
have contributed to our collections; and if any of our friends
can make our collections more complete, we shall be greatly
indebted.
Following is a list of all separate portraits on hand in March,
1897. Beside these, many others are available in books con-
tained in the library. It is hoped to print a list of the latter at
some future time. Edward S. Holden.
Abbe, C.
Adams, J. C. 3.
Airy, Sir G. B. 2.
Aitken, R. G.
Albrecht, Th.
Alvord, W.
Angot, A.
Anguiano, A.
Arago, F. 2.
Argelander, V.
Ashburner, W.
V. Asten, E.
Astrand, J. J.
Auwers, A. 2.
Bache, A. D.
Backlund, O.
Bailly, S. 2.
Bakhuysen, H. G.
Ball, Sir R. S.
Bardwell, Miss E. M.
Barnard, E. E. 3.
Bartlett, W. H. C.
Bass, E.
Bauschinger, J.
Becker, E.
Besse!, F. VV. 2.
Bessels, E.
Bey, Ali.
Bi^choffsheim, R. L.
Bohlin, K.
Bond, W. C. 2.
Bossert, J.
Bowditch, N. 2.
Boutelle, C. A.
Bradley, J. 2.
Brashear, J. A.
Breniiker, C.
Brendel, M.
Brooks, W. R.
Brown, Miss E.
Bruhns, C. 2.
Bruns, H.
Brunnow, F. F.
Budd, J. H.
Bull, S.
Bunsen, R. W.
Burckhalter, C.
Cacciatore, G.
Campbell, W. VV. 2.
Cayley, A.
Chandler, S. C.
Charroppin, C. M.
Chauvenet, VV^ 2.
Christie, W. H. M.
Clark, A. 3. .
Clark, A. G. 4.
Clark, G. B. 4.
Clausius, R. J. E.
Gierke, Miss A. M.
Coffin, J. H. C.
Colton, A. L.
Common, A. A.
Comstock, G. C.
Condorcet, M.
Cook, J. (Capt.)
Copernicus, N. 2.
Crew, H.
Crocker, C. F.
Crossley, E.
Curley, J.
Dana, J. D.
Davidson, G.
Davis, H. S.
Delambre, J. B. J.
Delmas, D. M.
Dembowski, E.
Doberck, W.
Dolland, J.
Donati, G.
Downing, A. M. W.
Draper, Mrs. A. P. 2.
Draper, H. 2.
Draper, J. VV. 2.
Dreyer, J. L. E.
Dubiago, D. T.
Dun^r, N. C.
Eastman, J. R.
Easton. C.
Ebert, H.
Elger, T. G.
Elkin, VV. L.
V. Engelhardt, B.
Engstrom, F.
Ennis, J.
Euler, L. 2.
Ewing, J. A.
Fabry, L.
Faraday. M.
Fergola, E.
Fernandez, L.
Flammarion, C.
Flamsteed, J.
Fleming, Mrs. M.
Floyd, R. S.
Foerster, VV.
Eraser. T. E
Frear, H. P.
Friend, C. VV^
Fritsche, H.
Frost, E. B.
Galileo, G. 2.
Gaudibert, C. M.
Galle, J. G,
Gauss. C. F.
Geelmuyden, H.
Gibbs, VV.
Gill, D.
Gilliss, J. M.
Glasenapp, S.
Gould, B. A. 3.
Astronomical Society of the Pacific.
97
Grubb, Sir H.
Gyld^n. H. 2.
Hagen, J. G.
Hall, A., Sr.
Hall, A., Jr.
Hallidie, A. S.
Hamilton, L.
Hansen, P. A. 2.
Hansteen, C.
Harkness, VV. 2.
Harrington, M. W.
Harzer, P.
Hazen, H. A.
Hasselberg, B.
Heis. E.
Hell. Father M.
Helmholtz, H. L. F. 2.
Henry, J.
Herschel. Miss Caroline
Herschel, Col. John
Herschel, Sir J. F. W. 2.
Herschel, Sir W. 3.
Hilgard, J. E.
Holden, E. S. 4.
Hough. G. W. 2.
Houghton, J. F.
Howe, H. A.
Hubbard, J. S.
Huggins, W. 2.
Hussey, W. J.
Ivanhof, A.
Janssen, J. 2.
Kaiser. F.
Kayser, H.
Keeler, J. E.
Kellogg, M.
Kelvin, Lord 2.
Kempf, P.
Kepler, J. 3.
V. Kirchhoff, G. R.
Kirkwood, D.
Klinkerfues, W.
Klumpke, Miss D.
Knobel, E. B. 2.
V. Konkoly, N.
Kreuger, A. 2.
Kreutz, H.
Kronecker, L.
de Lalande, J. G. L.
V. Lamont, J.
Lamp, E.
Lang, A., Santa Cruz,
W. I.
Langley, S. P. 3.
Lassell, W. 2.
Law, W. W.
Leadbetter, C.
Leavenworth, F. P.
LeConte, John 2.
Lehmann-Filh^. R.
V. Leibnitz, G. W.
Leuschner, A. O.
LeVerrier, U. J.
Lewis, H. C.
Lick, J. 6.
Lick, J. H.
Lindemann, E.
Lockyer, J. N.
Loewy, M.
Lorenzoni, G.
LoveJl, J. R.
Lowell, P.
Luther, R.
Lyman, C. A.
Macfarlane, A.
Manson, M.
Marcuse. A.
Marth, A.
Martin, E. S.
Marye, G. T.
Mathews, H. E.
Maunder, E. W.
Maury, M. F. 2.
Maw, W. H.
Maxwell, J. C.
McLaren, Lord
Mendenhall, T. C.
Mendizibal-TamborrelJ
Messer, J.
Meyer. M. W. .
Michelson, A. A.
Mills, D. O.
Mitchell, Miss Maria
Mizzi, L. F.
Molera, E. J.
Moller, A.
Monck, W. H. S.
Monge, G. 2.
Morrison, J.
Murphy, B. D.
Negus, J. D.
Negus, T. S.
Newcomb, S. 2.
Newton, H. A. 2.
Newton, Sir I. 4.
Nielsen, V.
Nightingale, J.
Nobile, A. 2.
Noble, W.
Norton, W. A.
Nyren, M.
Olbers, W.
Oom. F. A.
Oppenheim, H.
v. Oppolzer, E.
V. Oppolzer, Th.
Oriani, B.
Otis, J.
Palisa, J. 2.
Parkhurst, J. A.
Paul, H. M.
Pechule, C. F.
Peirce, B.
Peter, B.
Peters, C. A. F.
Peters, C. F. W. 2.
Piazzi, G.
Pickering, E. C.
Pickering, W. H.
Pihl, O. A. L.
Plum, C. M.
Pont^oulant, Comte.
Poor, C. L.
Preston. E. D.
Prince, C. L.
Pritchett, C. W.
Pritchett, H. S.
Proctor, R. A.
Raymond, W. G.
Rees, J. K.
Repsold, J. A.
Repsold, O.
Ricco, A.
Ristenpart, F.
Roberts, L
Rodgers, A.
Rodgers, J.
98
Publications of the
Rogers, W. A. 2.
Ros^n, P. G.
Rosse, Lord
Rotch, A. L.
Rowland, H. A.
Runge, C.
Runkle, J. D.
Rutherfurd, L. M. 4.
Sabine, E.
Salazar, L.
deSaussure, H. B.
Sawyer, E. F.
Schaeberle, J. M. 4.
Schiaparelli, J. V.
Schorr. R.
Schott, C. A.
Schulhoff, L. •
Schultz, H.
Schumacher, R.
Schumann, V.
Schur, W.
Schuster, A.
V. Schweiger-Lerchen-
feld, A.
Scott. I.
Scares, F. H.
Searle, A.
Searle, G. M.
Secchi, Father A.
See, T. J. J.
Seeliger, H.
Seidel, L.
Sestini. A.
Siemens, Sir C. W.
Skinner, A. N.
Smith, H. L.
Snell, K.
Spencer, H.
Stackpole, W.
V. Steinheil, A. C.
St. John, C. M.
Stockwell, J. N.
Stokes, G. G.
Stone, O.
Struve, Otlo. 2.
Struve, W. 2.
Swasey, A.
Swift, J. F.
Swift, L.
Sylvester, J. J.
Tacchini, P. 3.
Tait, P. G.
Taylor, I. M.
Terby, F.
Tesla, N.
Thome, J.
Tisserand, F. F.
Todd, D. P. 2.
Todd, S. E.
Trouvelot, L.
Tucker, R. H. 2.
Tycho Brahe.
Tyndall, J.
Updegraff, Mrs. A.
Upton, W.
Valle, F.
Van Hise, C. R.
Villarceau, L.
Violle, J.
Vogel, H. C.
Walker, S. C.
Warner, H. H.
Warner. W. B.
Waterman, R. W.
Watson. J. C.
Weinek, L. 3.
Wesley, W. H.
White, E. J.
Wiedemann, E.
Winlock, J.
Wislicenus, W. F.
Witkovsky, B.
Woeikof, A. J.
Wolf, C.
Wolf. Max
Wolf, R.
Wolfer, A.
Wolff, F. T.
Wright. T.
Yamall. M.
Young, C. A.
Zenger, C. V.
Ziel, F. R.
Light Absorption as a Determining Factor in the
Selection of the Size of the Objective for the
Great Refractor of the Potsdam Observatory.
In the Transactions of the Royal Prussian Academy of Sciences,
Professor Vogel gives, under the above title, an interesting and
important article on the methods and results of experiments made
to determine the loss of light in refracting telescopes through
absorption by the glass of the objective. The research was
undertaken, as the title suggests, to determine the size of the
lenses for the new Potsdam refractor, with the result that 80 cm.
was adopted as the size of the objective. This lens is corrected
for the actinic rays, and will be mounted with a guiding telescope
of 50 cm, aperture, corrected for visual rays.
Astronomical Society of the Pacific, 99
No abstract of this article is here attempted, as a translation
of the entire paper may be found in the Astrophysical Journal for
February, 1897.
It is of interest, however, to note that, according to Professor
VoGEL*s tables, giving the intensity of the transmitted in terms
of the incident light, as the thickness of the objective varies, the
visual objective of the thirty-six-inch telescope of the Lick Ob-
servatory (thickness about 7^ cm,') transmits about eighty-eight
per cent, of the visual rays that fall upon it, if allowance is made
for absorption only, and seventy-four per cent, allowing for
absorption and reflection. When the photographic correcting
lens is added, the thickness of the objective is approximately
1 2 cm. , and the intensity of the transmitted actinic rays, in terms
of the incident, is sixty per cent, when absorption alone is con-
sidered, and forty- nine per cent, when absorption and reflection
are both taken into account. R. G. Aitken.
March 15, 1897.
Awards of the Comet-Medal of the Astronomical
Society of the Pacific.
The Donohoe Comet- Medal has been awarded as follows,
since its foundation:
1. W. R. Brooks, March 19, 1890. 16. W. F. Gale, April 2, 1894.
2. W. F. Denning. July 23, 1890. 17. J. M. Schaeberle, April 16,
3. J. CoGGiA, July 18, 1890. 1893.
4. R. Spitaler, November 16, 18. E. D. Swift, November 20,
1890. 1894.
5. T. Zona, November 15, 1890. 19. L. Swift, August 20, 1895.
6. E. E. Barnard, March 29,1891. 20. C. D. Perrine, November 17,
7. E. E. Barnard, October 3, 1895.
1891. 21. W. R. Brooks, November 21,
8. L. Swift, March 6, 1892. 1895.
9. W.F. Denning, March 18,1892. 22. C. D. Perrine, February 15,
10. W. R- Brooks, August 28,1892. 1896.
11. E. E. Barnard, October 12, 23. L. Swift, April 13, 1896.
1892. 24. W. E. Sperra, August 31, 1896.
12. E. Holmes, November 6, 1892. 25. E. Giacobini, September 4,
13. W. R. Brooks, November 19, 1896.
1892. 26. C. D. Perrine, November 2,
14. W. R. Brooks, October 16, 1896.
1893. 27. C. D. Perrine, December 8,
15. W. F. Denning, March 26, 1894. 1896.
'^2:} \ (*>(>
loo Publications of the
Memorials of William Cranxh Bond, Director of the
Harvard College Observatory, 1840-59, and of his
Son, George Phillips Bond, Director of the Harvard
College Observatory, 1859-65, by Edward S. Holden,
Director of the Lick Observatory. Svo. 1897. Pub-
lished AT THE COST OF THE DAUGHTERS OF GeORGE
Bond, and Sold by C. A. Murdock & Co., 532 Clay
Street, San Francisco, and by Lemcke & Buchner,
812 Broadway, New York City.
No adequate biography of either of the Bonds is available.
At the request of the daughters of George Bond, I have under-
taken to arrange the manuscript material in their hands in an
orderly form. The book will be printed and published as above.
The contents are: Chapter I, Life of W. C. Bond, 1789-1859;
II, Life of G. P. Bond, 1825-1865; III, Selections from the
Diaries of George Bond; IV, Selections from the Correspon-
dence of George Bond; V, Account of the Scientific Work of
the Bonds; Appendixes, giving a complete list of their published
writings; and Index of Proper Names.
The book will be well illustrated. It is hoped by the
kindness of Professor E. C. Pickering, Director of the Harvard
College Observatory, to reproduce two fine steel engravings
of the Great Comet of 1858 and of the nebula of Orion^
from the plates of the Annals H. C. O. A small edition only
will be issued. The price of a single copy, bound in cloth,
including postage, will be two dollars. Orders may be sent to
C. A. Murdock & Co., 532 Clay street, San Francisco, or to
Messrs. Lemcke & Buchner, 812 Broadway, New York City.
Edward S. Holden.
Lick Observatorv, March 27, 1897.
The Reversing-Layer of the Sun's Corona (Total
Solar Eclipse of 1896, August 9).
A photograph of this eclipse, taken by Mr. Schackelton,
F. R. A. S., at Nova Zembla, shows the Sun*s ** reversing- layer"
first observed by Professor Young (visually) at the eclipse of
1870. The **reversing-layer" is, in a sense, the Sun's true
atmosphere, and Young's observation of 1870 seemed to show
that it can hardly be more than 500 miles in thickness. Professor
Young's conclusions have been much called in question by
Astronomical Society of the Pacific. loi
Professor Lockyer, whose dissociation theory requires a deep
solar atmosphere, with a considerable range of temperature
between its upper and lower levels. Mr. Shackeltgn's photo-
graph has been examined by Professor Young, and fully bears
out his conclusions. E. S. H.
Gift of Miss Bruce to the Observatory of Prague.
**The Director of the Observatory of Prague, Professor
L. Weinek, has received from Miss Catherine W. Bruce, the
high-minded patroness and well-wisher of astronomy in America,
the sum of 2439 florins ($1000) for the publication of the large
photographic Moon- Atlas begun by him in 1893.** — Prager
Abendblatt, March 3, 1897.
MeASI RES OF SiRWS.
Both of the following measures were made with the thirty-
six-inch telescope, using a 520-power eye-piece. Sirius was a
few minutes east of the meridian each night, and the atmospheric
conditions were fair.
Date. p. s,
1897.203 184.^9 3."98
1897.206 185.^3 3- "92
March 16, 1897.
R. G. AlTKEN.
Latitude of the Lick Observatory.
The mean value of the normal* latitude, 4>^^ derived from
observations with the meridian-circle in the interval between
September, 1893, and June, 1896, is —
37^ 20' 25".66 from about 1400 observations of 86 Berliner
Jahrbuch equatorial stars;
37*^ 20' 25".47 from about 1000 observations of 45 Berliner
Jahrbuch circumpolar stars; and
37° 20' 25^.85 from 160 observations of 22 Berliner Jahrbuch
zenith stars.
The correction for bisection and various systematic errors of
observation should be largely eliminated from the mean of cir-
• Corrected for Chandler's Variation.
I02 Publications of the
cumpolar and equatorial results. The bisection correction is
eliminated from the zenith determinations, made facing north
and south alternately, for the same star.
Some of the B. J. declinations of zenith stars have undoubt-
edly large errors; the declinations of the American Ephemeris
would reduce the observed latitude by ©''.23 for sixteen of these
stars. The normal latitude <^o=37° 20' 25".6— corresponding
to the epoch 1895. i may be adopted as the best value furnished
by the series of observations made in this period.
R. H. Tucker.
The International Astrographic Charts.
**The fourth reunion of the Comity Permanent was held in
Paris in May. The reports furnished by the Directors of the
co-operating observatories show that satisfactory progress has
been made in two- thirds of them. Owing to political or financial
difficulties, the work has not yet begun at Santiago de Chili, La
Plata, and Rio Janeiro, and is seriously hampered at several
other observatories.
The following table shows how far the photo- mapping has
advanced in the different zones: —
No. of
Zone. Fields No. taken for
Assifirned. Cat. Chart.
Greenwich +9010+65 1149 728 472 313 plates measured; 102 plate
constants determined.
Rome +64 to +55 1040 280 100 —
CaUnia +54 to +47 1008 21 None. —
Helsingfors +46 to +40 1008 1008 A few. 160 plates measured and
partly reduced.
Potsdam +39 to +32 1232 500 A few. 35«ooo stars measured.
Oxford +31 to +25 1180 800 None. 40,000 stars measured on 160
plates.
Paris +24 to +18 1260 1155 Not stated. 318 plates measured, 60 re-
duced.
Bordeaux +17 to +11 1260 300 60 Measures to be begun soon.
Toulouse +ioto+ 5 1080 150 350 70 plates measured.
Algiers + 4 to — 2 1260 1000 64 168 plates measured with
32,oco siars.
San Fernando — 3 to — 9 1260 1260 About 400. 50 plates measured once and
25 twice.
Tacubaya — xo to —16 1260 529 Not stated. Measuring toibegin soon.
Santiago de Chili. . . —17 to —23 1260 — — —
La Plata —24 to —31 1360 — — —
Rio Janeiro —32 to —40 1376 — — —
Cape of Good Hope . —41 to —51 1512 1512 Nearly half. 30 plates measured.
Sydney —5210—64 1400 1393 1112 —
Melbourne —65 to —90 1149 703 A few. —
Examination of this table shows that (omitting altogether the
three South American observatories which have not yet com-
Astronomical Society of the Pacific. 103
menced) the taking of the catalogue plates is generally well
advanced, and that some progress has been made with the chart-
plates. The measurement and reduction of the catalogue plates
have been begun by more than half the observatories, and consid-
erable progress has been made by six or seven of them.
The Congress first turned its attention to the degree of
accuracy which it was desirable to obtain in the measurement of
the photographs. It was decided that the probable error of the
measured co-ordinates ought not to exceed ±:o". 20.
The choice of the reference-stars and the methods of measure-
ment and reduction were left to the discretion of the Directors of
the co-operating observatories. It was resolved that the meas-
ured rectilinear co-ordinates should be published as soon as
possible, along with the necessary data for obtaining the Right
Ascension and Declination of the stars when required. With
regard to the magnitudes, the Congress laid down no conditions
except that the methods adopted for their determination should
be capable of precise definition, so that the scales employed
at diflferent observatories might be readily comparable. For the
Chart, it was decided that in the odd zones a triple exposure of
30" should be given.
Captain Abney undertook to supply the different observa-
tories with scales which should be printed on the plates at the
same time as the riseaUy and supply a measure of the sensibility
of the plates for light of different intensities. It was also resolved
that two positives of each chart-plate should be made on glass,
and that one of them should be placed in the Bureau National
des Poids et Mesures.** — From Monthly Notices R. A. S., Vol.
LVII, p. 298.
Weather at Mt. Hamilton in the Winter of 1896-97.
The following data are taken from the meteorological records
for the respective months, the record for March being included
to date: —
Cloudy nights ..'.... 14
Rainfall („S2?;"nSw), in inches
Snowfall, in inches i
During the first three of these months, the clear nights, and
occasionally part of a night marked ** cloudy," were suitable for
1896.
Nov.
Dec.
1897.
Jan.
Feb.
Mar.
Total.
14
17
10
18
15
74
5.8
4.9
3.5
5.9
0.6
20.7
I
3
2
17
30
53
I04 Publications of the
observing. A few nights were very good, but from January 25th
to date there have been but fourteen clear nights, and not more
than one-half that number on which the ** seeing'* could be called
good. R. G. AlTKEN.
Mt. Hamilton, March 20, 1897.
The Companion of Sirius, Observed at Glasgow, Mis-
souri, WITH A Twelve-inch Telescope.
[Extract of a letter from Professor H. S. Pritchktt.]
"Saturday night, March 20, 1897, I was at Glasgow, and the
night was unusually fine. I have seldom seen so good a one in
this climate. With the I2j4-inch glass, both my father and
myself saw the Sirius companion (shutting the bright star out of
the field). The result of three settings of the micrometer gave
/= 195°; s (estimated) between 3" and 4".*'
The Bruce Medal of the Astronomical Society of
THE Pacific.
It is the intention of Miss Catherine Wolfe Bruce, to
whom Astronomy in all parts of the world owes so many and
such intelligent benefactions, to found and endow a gold medal,
to be awarded not oftener than once a year by the Astronomical
Society of the Pacific, **for distinguished services to Astronomy.'*
It is Miss Bruce' s desire that the medal shall be international in
character, and that it shall be awarded to citizens of any country,
and to persons of either sex.
The medal is to be of gold, about sixty millimetres in
diameter, and is to bear the seal of the Society on the obverse,^
The reverse is to bear an appropriate inscription. The formal
offer of Miss Bruce will be made, and the medal founded and
endowed, during the present year, so that the first award can be
made (if desirable) for the year 1898. At the proper time, due
acknowledgments will be offered to Miss Bruce for this very
generous gift to Science and to the Society. Not only will the
Bruce medal tend to the advancement of Astronomy, and
enable the Astronomical Society of the Pacific to adequately
recognize scientific work of the highest class (and these are Miss
Bruce' s only desires), but it will forever connect the name of
•Sec these Publications, Volume III, page 78, for a full-sized drawing of the seal.
Astronomical Society of the Pacific. 105
the founder with the progressive advances of Astronomy. Those
who are knowing to her very many and wise subventions
of astronomical research (a few of which are spoken of in these
Publications),^ will welcome this, her latest gift, for personal as
well as for scientific reasons. The Society is to be congratulated
that Miss Bruce has selected it as the Trustee to carry out her
generous desires. If the trust is executed, as it will be, with intel-
ligence, fidelity and circumspection, the time will soon come when
the Bruce medal will be one of the most highly-prized recogni-
tions of original and useful service to Astronomical Science.
Edward S. Holden.
The Lick Observatory, April 6, 1897.
Return of the Lowell Observatory to Arizona.
**The Lowell Observatory has not found the site in the vicinity
of the City of Mexico as favorable as had been expected, and will
be moved back to Flagstaff, Arizona.**! — Science ^ March 26,
1897* page 512.
The Cape Photographic DurchmusterungX
In 1885, Dr. Gill commenced a photographic survey of
the southern heavens from eighteen degrees of South Decl. to
the south pole. The observations have been made at the Cape,
and the measures and many of the reductions by Dr. Kapteyn,
in Holland. The negatives were made with a Dallmever lens
of six inches aperture and fifty-four inches focus, and the expo-
sures (thirty to sixty minutes) are chosen so as to include all
stars as bright as the tenth magnitude. Each plate covers thirty-
six square degrees. The epoch of the Catalogue is 1875.0; and
the probable errors of the positions are o'.27 and 2". 6 in R. A.
and Decl. respectively.
The (photographic) magnitudes are deduced so as to make
the mean photographic magnitude of a group of stars identical
with the mean visual magnitude. The average number of stars
per square degree is 25.4, and the absolute number varies from
•Vol. If, p. 307; Vol. V, p. 82; Vol. V, p. 186; Vol. VlII, p. 243; Vol. IX, No. 55
(Bbuck Telescope, Moon maps, etc.)
t See Mountain Obiervatories, 1896, page 66.
tThe first volume of this work (—19^ to— 37^), containing 152,000 stars, is printed.
The second volume (—38*1052*), containing 158,000 stars, is in the press.
io6 Publications of the
six to more than one hundred. In Arge lander's Durchmus-
ierung, the average number is 15,2, in Schoenfeld*s it is 18.5,
and in the Cordoba D. M. (—22° to —42°) it is 56.1. — Abstract
of a paper in the Monthly Notices R. A. S,, Vol. LVII, p. 297.
International Catalogue of Fundamental Stars.
In May, 1896, a Conference was held at Paris at the invitation
of the Bureau des Longitudes^ to consider a plan for the forma-
tion of a fundamental catalogue of standard stars for the ephe-
merides published in France, England, Germany, and America.
The personnel of the Conference was Messrs. Auwers (Germany),
BfCKLUND (Russia), Bauschinger (Germany), Christie
(England), Downing (England), Gill (Cape of Good Hope),
Loewv (France), Newcomb (United States), Tisserand
(France). M. Faye (France) acted as President, and Messrs.
V. d. S. Bakhuvsen (Holland) and Trepied (France) served
as Secretaries. The conclusions of the Conference were adopted
with practical unanimity. The most important were as follows:
For the fundamental catalogue, the equinox should be determined
solely from observations of the Sun, excluding those of Mercury
and Venus, The equinox of Professor Newcomb* s system
(Nx) in Vol. I of the Astronomical Papers of the American
Ephemeris was adopted.* In view of the uncertainty that still
exists with regard to the numerical value of the personal error
depending on magnitude, which affects the R. A., it was decided
that corrections for such errors should not be applied. But as the
existence of such (small and systematic) errors is undoubted, the
Conference considered that observatories should make researches
to fix their amounts. Professor Newcomb was entrusted with
the duty of fixing the values of the precessions to be employed.
The Conference decided to adopt the following constants:
Nutation, 9".2i;t Aberration, 2o".47;J Solar Parallax, 8".8o.§
It was decided that in the reduction of mean places of stars to
apparent, the term of short period in R. A. (y"') depending on
twice the Moon's longitude should be omitted for both polar and
equatorial stars.
• Catalogue of 1098 stars,
t Dr. Gill's determination = 9".207 i o".oo3.
\ From the adopted solar-parallax and the Nbwcomb-Michblson value of the
velocity of light there results 2o".467 ± c/'.oi2.
\ Dr. Gill's determination (heliometer) 8".8oa ± o^'.oos.
Astronomical Society of the Pacific. 107
Professor Newcomb was entrusted with the duty of preparing
a provisional fundamental catalogue, which is to be finished during
1896. This catalogue is to contain about 1000 fundamental stars.
The Conference laid down various other principles on which the
catalogue should be constructed which are not mentioned
here. It also expressed the hope that a scheme of international
co-operation might be established for the calculation of the per-
turbations and ephemerides of the minor planets (of which there
are now more than 400). The opinion was also formally expressed
that a first-class reversible meridian-instrument, suitable for
fundamental work, should be erected at one of the southern
observatories. The changes of astronomical constants, as recom-
mended by the Conference, are to take effect in the ephemeris for
1 90 1. ** There appears to be every reason to expect that the
catalogue will be ready in good time, and that astronomers may
look forward to the inauguration of a new era in the history of
astronomical ephemerides at the commencement of the twentieth
century." — Abstract of a paper by Dr. Downing in the Monthly
Notices R. A. S., Vol. LVII, page 299.
Probable Error of a Single Observed Position in
Some Frequently Used Catalogues and
Collections of Stars.
The probable accidental error of an observed place, depend-
ing on a single observation, in the following catalogues, etc., is
(approximately) as follows: —
Harvard College Observatory (Vol. XII)
Berlin Observatory (670 stars)
•* Observatory (521 stars)
Lick Observatory (310 stars)
Pulkowa Catalogue (Vol. VIII)
CS634 stars)
Washburn Observatory (303 stars) -
Yamall's Catalogue - - - .
Dunsink Observatory (717 stars)
Harvard College Observatory (A. G. Zone)
Dudley Observatory (A. G. Zone)
Helsingfors-Gotha Observatory (A. G. Zone)
Cincinnati Observatory (2000 stars)
Bonn Observatory (Vol. VI; bright stars)
R a. 1
[Equator).
s.
Decl.
-
.02
0.3
-
.02
0.3
■±^
0.03
±0.3
-
•03
03
-
•03
0.3
-
.04
03
-
•03
0.4
-
.03*
0.5*
-
.04
05
-
•03
0.6
-
.04
0.6
) -
.06
0.6
-
•05
0.6
-
.04
0.6
io8
Publications of the
Bonn Observatory (Vol. VI; stars 9th mag^nitude) .06
** ** (Vol. VI; stars 9.2 and 9.3) -
Grant's Glasgow Catalogue - -
Cordoba Zone Catalogue ....
Bond's Zones (H. C. O. Vol. II)
Schjellerup's 10,000 stars - - - -
Copeland and Borgen's Catalogue
Wilson's 644 stars
Dunsink Observatory (1600 stars)
Armagh Observatory (Catalogue II)
Lamont's Zones (re-reduced in Munich Annals, II)
Harkness* Gilliss Southern Zones
Weisse's Bessel's Zones, I - - -
Gottingen (Klinkerfues Schur, 6900 stars)
Argelander's Southern Zones (Oeltzen)
Weisse's Bessel's Zones, II -
Cincinnati Observatory (4050 stars)
Cape (Photographic) Durchmusierung
Lacaille (B. A. A. S.) - - - - c
Section II, Bonn DurchmusUrting
Cordoba (visual) '*
Section I, Bonn ** . . .
Equator
). Decl.
J.
"
.06
0.6
.07
0.8
.06
0.8
.06
0.8
.07
0.8
.08
0.8
.08
0.8
.09
0.8
.07
0.9
.08
0.9
.08
0.9
.04
I.I
.16
1.4
.10
1-4
.12
1.4
• 15
1.6
.12
1.8
.27*
2.6*
..3*
8.7*
.38*
9.6*
.42*
13-8*
.70*
25.6*
E.
S. H.
Addendum to Dr. Marth's Article on Page 76.
h. m. s.
,.
1890, Aug. 24
7 38 5
26.71 + 1.45
—6.38+1.02
972.3
1.92
i89i,July 14
9 33 29.5
16.40+1.15
—5.25—2,61
908.6
18.45
14
9 35 32.5
16. 42+1. 15
—5.26 — 2.60
908.6
18.45
1895, July 30
8 22 54
21.98+0.93
+6.69+7.5T
929.4
10.16
31
9 '649
34-63-1-0.91
+6.23+7.55
918.8
492
_ 31
9 «7 49
34.64-f-0.91
+6.23+7.55
918.8
4.92
Oct. 10
16 2 2.2
184.33—0.93
—5.35-5.36
966.2
6.57
Notice to Members.
Owing to a misunderstanding, an essential part of the manu-
script of the present number was not received until April loth,
which accounts for the delay in the issue.
The Committee on Publication.
* Probable errors of a printed catalogue-place.
Astronomical Society of the Pcuific. 109
Recent Observations of the Spectrum of Mars,
BY W. W. Campbell.
•*In the year 1894, I described for the Chronicle my observa-
tions of the spectrum of Mars^ and stated the conclusions to be
drawn from them concerning? the presence of atmosphere and
water on that planet. The observations were made by visual
methods entirely. In the spring of 1895 ^"^ ^^ winter of
1896-97, I repeated the observations, making them by pho-
tography. Professor Keeler of the Allegheny Observatory
(formerly of the Lick Observatory), recently wrote me that he
also had observed the spectrum of Mars photographically in the
last few months, and I have his permission to describe his results
along with my own. Our work has an important bearing on the
question of Mars^ atmosphere and the conditions of life on that
planet, and I take this opportunity of making it public. * ♦ ♦
*'The problem was attacked in the years 1862-77 ^y Huggins,
Janssen, Vogel, and Maunder. All came to the conclusion
that the spectroscope was able to detect evidence of atmosphere
containing water-vapor. Their results supported the popular
side of the question, and were accepted without reserve. Their
observations were nearly all made under extremely unfavorable
circumstances: withil/ary near the horizon, with small telescopes,
at stations near sea level and in very moist localities. I feel sure
that the observers themselves would now be willing to say that
much of their evidence was very discordant, and in some points
it was erroneous. A case in court, based on similar evidence,
would be dismissed, with costs levied on the plaintiff.
•* While I believed that the early observations, though weak
and discordant, were essentially correct, it seemed to me well
worth while to repeat them at Mt. Hamilton, on account of the
favorable circumstances of position and climate existing here.
Among the advantages existing here may be mentioned: i. A
more powerful telescope and spectroscope. 2. The altitude of the
observatory, eliminating the lower 4200 feet of atmosphere and
its aqueous vapor. 3. The southern location of the observa-
tory and the northern position of Mars in 1894, bringing the
planet nearer the zenith. 4. The very dry air existing here in the
early summer. With these and other favorable circumstances, I
expected that a confirmation of previous results would be a
simple and easy matter. Accordingly, I compared the Martian
no Publications of the
and lunar spectra on several nights in 1894, when our atmosphere
was remarkably dry, and the two bodies were at equal altitudes
above the horizon. At all times the spectra of the two bodies
appeared to be identical in every respect. The oxygen and
aqueous vapor lines were stronger when the Moon and planet
were near the horizon than when they were near the zenith, for
the obvious reason, that in the lower positions the rays of light
traversed the greater depth of our atmosphere. In fact, an in-
crease of twenty-five to fidy per c^nt. in the length of path in our
atmosphere seemed sufficient to change the spectrum appre-
ciably.
* * The conclusions to be drawn from the observations are very
simple, yet they have been widely misunderstood. They are:
I. The observations furnish no evidence of the existence of a
Martian atmosphere containing aqueous vapor. 2. They do not
prove that Mars has no atmosphere, nor do they even suggest
that idea. They simply set a limit to the possible extent of the
atmosphere, or, rather, to the quantity of oxygen and aqueous
vapor contained in it. The light coming to us from Mars has
been reflected from the planet* s surface, or from the inner strata
of its atmosphere, and has, therefore, passed twice, either com-
pletely or partially, through its atmosphere. If an increase of
twenty-five to fifty per cent, in the length of path of the rays in
our atmosphere changes the spectrum appreciably, the Martian
atmosphere should have been detected, if it is one fourth as ex-
tensive as ours. 3. We know, from the waxing and waning of
the polar caps with the advent of winter and summer, respect-
ively, that Mars has some atmosphere and some vapor analogous
to our water-vapor, but we do not know how much. They do
not seem to exist in sufficient quantities to be detected by
spectroscopic methods; that is, they do not seem to be more
than one fourth as extensive as on the earth, and they may be
considerably less.
** As soon as my 1894 results were published, Messrs. Huggins
and VoGEL repeated their observations of 1867 and 1873, re-
spectively. Both were very positive in the early years that
Mars' atmosphere and aqueous vapor were very easy to detect,
and must, therefore, be of great extent. They were able, in
1894, to confirm their early work in some points, but in others
they were not. This is not the place to make a scientific criticism
of scientific results, but it should be stated that at the points in
Astronomical Society of the Pacific. 1 1 1
the spectrum where Huggins said the aqueous vapor h'nes were
stronger in Afars than in the Moon, Vogel said no difference
could be detected by him; and in the case of the vapor lines in
another place in the spectrum, which Vogel said were stronger
in Mars than in the Moon, Huggins did not detect any differ-
ence. The two distinguished observers did not agree with each
other in even a single point.
** As stated above, the 1894 results were arrived at entirely by
visual methods. The past winter, Professor Keeler and I,
working independently, repeated my 1894 work, using the
photographic method. We photographed the spectrum of
Mars and the Moon when these bodies had equal altitudes.
After a few trials, it was easy to determine the exposure time
necessary to make the two photographic images of the same
density. When the negatives were developed, it remained only
to compare the spectra to detect any differences that might
exist Neither Professor Keeler nor I was able to detect the
slightest difference between the spectrum of Mars and that of the
Moon. (It should be said that the aqueous vapor lines most
studied by the various observers lie in the yellow and orange of
the spectrum, and to record them photographically it was
necessary to use orthochromatic plates. The oxygen lines lie
wholly, so far as we know, in the red, and could not be photo-
graphed satisfactorily. The investigation applies, therefore, only
to the aqueous vapor lines.)
" Professor Keeler considered that if the Moon moved from
the zenith down to an altitude less than forty-five degrees, its
spectrum underwent appreciable changes: the vapor lines were
the stronger in the lower position of the Moon. My estimate of
the sensitiveness of the method was practically the same, or a
trifle less, than Keeler' s. Now, the length of path in our
atmosphere traversed by the Moon's rays, when at an altitude of
forty-five degrees, is forty per ceni, longer than when the Moon
is in the zenith. Again we confirmed my visual results of 1894,
since I then found that twenty-five to fifty per cent increase in
the length of path produced an appreciable change in the spec-
trum. Recalling that the light coming to us from Mars has
passed twice, either completely or partially, through that planet's
atmosphere, we arrive again at the result that the water- vapor
there is not more than one fourth as extensive as on the Earth.
(In speaking of * extensiveness,' I mean the absolute quantity
112 Publications of the
of vapor above a given area — a square mile, for example — of
the planet's surface.)
** Having been led, by the observations of 1894, to take the un-
popular side of the question, viz: the oxygen and water- vapor (or
some other vapor analagous to water- vapor) in Mars^ atmosphere
are of slight amount, probably not more than one fourth as ex-
tensive as on the Earth,— I may be pardoned for saying it is a
pleasure to have so able and conscientious an observer as Pro-
fessor Keeler write: * No doubt you are entirely correct on the
water- vapor question.'
** Assuming that the chemical constituents exist in the same
proportions in the Earth's and Mars' atmospheres — we cannot say
that they do — what would be the density of Mars' atmosphere at
the planet's surface? If there is not more than one fourth as
much atmosphere above a square mile on Mars as there is above
the same area on the Earth, its density at the surface of the
planet would be less than one eighth the density of our air at
sea level; that is, it would be less than half as dense as the
atmosphere at the summit of Mt. Everest. Such being the case,
the conditions of life on the two planets would no longer be
comparable. Astronomers would wisely turn the question of life
on our neighboring planet over to the physiologists for solution;
and possibly the latter would wisely hand it over to the domain
of pure speculation for the present.'* —From the S. F. Chronicle,
April 25, 1897.
Astronomical Society of the Pacific. 113
Minutes of the Meeting of the Board of Directors,
held in the rooms of the astronomical society
OF THE Pacific, March 27, 1897, at 7:30 p. m.
President Hussey presided. A quorum was present. The minutes
of the last meeting were read and approved. The following members
were duly elected:
List of Members Elected March 27, 1897.
Mr. Geo. M, Edgar JUmyer^tyJ>.0.. TusqaloosaCo..
Mr. L. L. Hawkins 268 Oak St., Portland, Oregon.
Free Public Library Newark, New Jersey.
Library of the University OF\r-.^^^^. „ ;ii;„^:.,
iLLLNOis / Champaign, ilhnois.
Library of the University of\d, ^^. .^„ t«^:««^
Indiana j fi'oo»"*"8^on, Indiana.
Mr. John W. Salsbury Clear Water Harbor, Florida.
Mile. Le Brun de Surville .... 3242 Sacramento St., S. P., Cal,
Mr. George Taylor Walnut St., Brookiine, Mass.
Mr. William Yates | Bo^jSs, Station C, Los Angeles,
The following resolution was, on motion, adopted:
Whbrbas, On the lath day of January, 1891, the sum of $70.89 was paid out of the
Alexander Montj^omery Library Fund for sixty Comet -Medals, which amount should
have been paid out of the Donohob Comet-Medal Fund;
Be it resolved. That the Treasurer be instructed to transfer said sum of 570 89 from
the DoNOHOE Comet-Medal Fund to the Alexander Montgomery Library Fund. (•]
The Library Committee presented its report, as follows, and the
report was, on motion, adopted and filed:
San Francisco, Cal., March 27, 1897.
Board of Directors^ Astronomical Society of the Pacific^ San Francisco^ California: —
Gbntlbmrn — At your meeting of January 30, 1897, the following resolutions were
adopted:
" Whbrkas, The Society possesses a considerable number of valuable books and
periodicals that are still unbound; and
** Whbrbas* A considerable portion of the income from the Alexander Montgomery
Library Fund remains unexpended; be it therefore
**Resolved, That the unexpended portion of the accrued interest from this fund
be expended:—
•' I. For bindings for valuable unbound books and periodicals already in the posses-
sion of the Society; and then, if any portion of this income remains unexpended,
"3. For the purchase of additional astronomical books and periodicals; and be it
further
• It seems proper to say here that the medals in question were bought in Paris, in
1890. by the Chairman of the Comet-Medal Committee. They could not be paid for from
the principal of the medal-fund (which can not be impaired), nor from its interest (which
WM not sufficient). Accordingly, on December 15, 1890, the Chairman wrote to the
Treasurer of the Society (Mr. Molbra) to request that their cost be defrayed, provided
the Directors approved, from the General Fund (not the Library Fund).
Edward S. Holdbn.
114 Publications of the
** Resolved, Thai the President aud Library Committee be aathorized to carry
these provisions into eflRect."
We befc to report, that by virtue of Uk authority granted by the above resolutions,
we have examined with care the unbound books, penodicals, and pamphlets in posses-
sion of the society, and have prepared and sent to the binders lox volumes.
We have delivered these books to the Hicks-Judd Company, 33 First Street, San
Francisco, for binding. Their schedule of prices for this work is given in their letters of
March 13. 1897, which are appended to, and made a part of, this report.
In the case of periodicals and works issued in parts, we have found that numbers
are sometimes missing. Such volumes have not been sent to the binders. We have
written to some of our exchanges for missing numbers; we have ordered the missing
numbers of the Astronomische Nackrickten from Dr. Krbutz, Kiel, Germany, the remain-
ing parts of Proctor's Old and New Astronomy^ from Messrs. Longmans, Grkbn &
Co., 15 East i6th St., New York City.
From Prof. W. W. Paynb. Northfidd, Minn., we have ordered] Vol. 1 of the
Sidereal Messenger, to complete our set, and Vols, i to 5, inclusive (the last to be sent as
issued), of Popular Astronomy, The Society already has Vols. 95 to 128 of the Astro-
nomisfke Nackrickten. We have ordered the first ninety-four volumes of this important
periodical from F. A. Brockhaus, Leipzig, Germany, at a cost lour offer) of $300.
We have directed all bills to be sent to the Secretary of the Society in San'Francisco.
We have arranged our orders so as to leave a sufficient balance of the funds available to
cover freight and other charges that may yet arise in connection with our purchases.
(Signed) W. J. Hussby,
President A. S. P,
E. J. Molbra,
RosB O'Halloran,
Chas. Burckhaltbr.
I wish to go on record that the ninety-four vols., A. N, were bought without my
knowledge, and I would not have consented to such a large expenditure. C. B.
Minutes of the Annual Meeting of the Astronomical
Society of the Pacific, held in the Lecture
Hall of the California Academy of
Sciences, March 27, 1897.
The meeting was called lo order by President Hussby. A quorum
was present The minutes of the last meeting were approved.
The Secretary read the names of new members duly elected at the
Directors' meeting.
The following papers were presented:
1. Address of the retiring President, by Prof. W. J. Hussky.
2. Reports of Committees: on Nominations; on the Comet- Medal; on
Auditing; and Annual Report of the Treasurer.
3. Astronomical Observations made in 1896, by Mr. Torvald Kohl, of
Odder, Denmark.
4. Predictions for the Solar Eclipse of July 29, 1897, for Mt. Hamilton
and San Francisco, by Mr. C. D. Perrine.
5. Planetary Phenomena for May and June, 1897, by Prof. M. McNeill,
of Lake Forest, Illinois.
6 . Ephemeris for physical observations of the Moon for certain dates
between 1890 and 1895, by A. Marth, F. R. A. S., of Markree,
Ireland.
Astronomical Society of the Pacific. 115
The Committee on Nominations reported a list of names proposed
for election as Directors, as follows: Messrs. Alvord, Holdbn,
MoLERA, MoRSB, Perrinb, Pierson, Seares, St. John, Von Geldern^
ZiEL, and Miss 0*Halloran.
For Committee on Publication: Messrs. Holden, Babcock, Aitken.
Messrs. Burckhalter and Brasch were appointed as tellers. The
polls were open from 8:15 to 9 p.m.
After counting the ballots, the tellers announced that the following
persons had received a majority of the votes cast, namely: For Direc-
tors — Messrs. Alvord, Holden, Molera, Morse, Perrine, Pierson,
Seares, St. John, Von Geldern, Zikl, and Miss O'Halloran. For
Committee on Publication— Messrs. Holden, Babcock, Aitken.
The Chairman declared these persons duly elected, to serve for the
ensuing year.
Report of the Committee on the Comet-Medal,
Submitted March 27, 1897.
This report relates to the calendar year 1896. The comets of 1896
have been:
Comet a: (unexpected comet), discovered by Mr. C. D. Perrine,
Assistant Astronomer in the Lick Observatory, on February 15th.
Comet b: (unexpected comet), discovered by Dr. Lewis Swift, Director
of the Lowe Observatory, on April 13th.
Comet c: (periodic comet), 1889 V (Brooks), re-discovered by M.
Javelle, Astronomer of the Observatory of Nice, on June 20th.
Comet d: (unexpected comet), discovered by Mr. W. E. Sperra, of
Randolph, Ohio, on August 31st.
Comet e: (unexpected comet), discovered by M. E. Giacobini, Assist-
ant Astronomer of the Observatory of Nice, on September 4th.
Comet f: (unexpected comet), discovered by Mr. C. D. Perrine,
Assistant Astronomer in the Lick Observatory, on November ad.
Comet g: (unexpected comet), discovered by Mr. C. D. Perrine,
Assistant Astronomer in the Lick Observatory, on December 8th.
On September 21st, two comets were reported by Dr. Lewis Swift,
Director of the Lowe Observatory. As no positions of these
objects were secured el^ewhere, they have not been included
in the list of comets for the year.
The Comet-Medal has been awarded to the discoverers of Comets
tf, ^, </, ^, fy gy in accordance with the regulations.
Respectfully submitted,
Edward S. Holden,
J. M. Schaeberle,
W. W. Campbell,
Committee on the Comet-Medal,
ii6 Publications of the
The Treasurer submitted bis Annual Report, as follows: —
Annual Statement of the Receipts and Expenditures op the
Astronomical Society of the Pacific for the
Fiscal Year ending March 27, 1897.
general fund.
Receipts,
Cash Balance. March 28, 1896 1 s8o 73
Received from dues I1491 32
*' *' sale of publications aod reprints 9900
" *' advertisements 7500
' " Comet -medal Fund (engraving 21 medals) 2100
" " Security Savings Bank (interest) 199
" ** Life Membership Fund (interest) 5508
•• " *' " *' (loan August 5, 1896) 12500
I186839
Less transfer to Life Membership Fund Isooo
Returned to Life Membership Fund (loan of August 5, 1896) ... 125 00 175 00 1693 39
I2274 12
Expenditures.
For publications .I1099 93
*' general expenses 68490
$178453
Cash Balance March 27, 1897 489 29
|ga74 "
LIFE MEMBERSHIP FUND.
Cash Balance March 28, 1896 I1700 61
Received from General Fund 50 00
" " " " (loan of August 5, 1896, rttumed) 12500
** '* interest 55 08
I1930 69
Less interest transferred to General Fund I 55 08
" loan to General Fund ( August 5, 1896) 125 00 180 08
Cash Balance March 27, 1897 I1750 61
DONOHOE COMET-MEDAL FUND.
Cash Balance March 28, 1896 | 674 32
Interest 22 72
I 697 04
Less transfer to General Fund for engraving 21 medals 21 00
Cash Balance March 27, 1897 | 676 04
ALEXANDER MONTGOMERY LIBRARY FUND.
Cash Balance March 28, 1896 I1857 38
Interest 75 30
Cash Balance March 27, 1897 |r93a 68
Astronomical Society of the Pacific. 117
FUNDS.
Balances on Deposit as follows:
General Fond:
with Donohoc-Kelly Banking Co I 285 33
** Security Savings Bank 203 96
I 489 29
1750 61
676 04
Life Membership Fund:
with San Francisco Savings Union % 550 61
" German Savings and Loan Society 60000
•* Hibernia Savings and Loan Society 60000
Dooohoe Comet-Medal Fund:
with San Francisco Savings Union. | 266 76
** German Savings and Loan Society 204 63
** Hibernia Savings and Loan Society 20465
Alexander Montgomery Library Fund:
with San Francisco Savings Union. | 670 68
" German Savings and Loan Society 64810
" Hibernia Savings and Loan Society 61390
1932 68
$4^4862
Sam Francisco, March 27, 1897. F. EL ZIEL, Treasurer,
The committee appointed to audit the Treasurer's accounts reported
AS follows, and the report was, on motion, accepted and adopted:
To th^ President and Members 0/ the Astronomical Society of the Pacific:—
Grntlbmrn— Your committee appointed to audit the accounts of the Treasurer for
tbe fiscal year ending March 27, 1897. have made a careful examination, and find same to
be correct. Yours respectfully,
F. H. MCCONNBLL.
D. F. TlLLINGHAST.
President Hussey then read his annual address.
The following resolution was, on motion, adopted:
Resolved, That all the acts appearing in the minutes of the meetings of the B ard
of Directors of this Society, as having been done by said Board during the past fiscal
year, are here now, by this Society, approved and confirmed.
The thanks of the Society were returned to the California Academy
of Sciences for the use of the lecture hall.
Adjourned.
ii8 Publications of the
Minutes of the Meeting of the Board of Directors of
THE Astronomical Society of the Pacific, held in
THE Rooms of the Society, March 27, 1 897,
AT 9:45 P.M.
On motion of Mr. Molera, Mr. St. John took the chair, and called
the meeting to order. A quorum was present. The minutes of the last
meeting were approved.
The business in band being the election of officers and committees
for the ensuing year, the following officers and committees, having re-
ceived a majority of the votes cast, were duly elected:
President: Mr. William Alvord.
First Vice-President: Mr. Edward S. Holden.
Second Vice-President: Mr. Frederick H. Seares.
Tliird Vice-President: Mr. Chauncev M. St. John.
Secretaries: Messrs. C. D. Perrine and F. R. Ziel.
Treasurer: Mr. F. R. Ziel
Committee on the Comet-Medal: Messrs. Holden (ex-officid)^
SCHAEBERLE, CAMPBELL.
Library Committee: Messrs. Hussev and Seares, and Miss
O'Halloran. Mr. Hussev was appointed Librarian.
The President was authorized to appoint the members of the
Finance Committee of the Board of Directors, and accordingly made
the following selections:
Finance Committee: Messrs. Wm. M. Pierson, E. J, Molera, and
C. M. St. John.
The Committee on Publication is composed of Messrs. Holden,
Babcock, Aitken.
Adjourned.
Astronomical Society of the Pacific. "9
OPPICBRS OP THB SOCISTY.
Mr. WjLLiAM Alvord Prtsident
Mr. Edward S. Holdsn First Vice-Pretident
Mr. Frkdbrick H. Ssarbs Second VicfPresideni
Mr. Chauncbv M. St. John Third Viu-President
sjiR-R-i:'.:"-'! ^''"uru.
Mr. F. R. ZiKi. Treasurtt
Board of Directors- }desirs. Alvord, Holdbn, Molbra, Morsb, Miss O'Halloran,
Messrs. Pbrrine, Pierson, Sbakbs, St. John, von Gbldern, Ziel.
Fit%amce Committe* — Messrs. William M. Pibrson, £. J. Molbra, and C. M. St. John.
Cemmittet on Publication — Messrs. Holdrn, Babcock, Aitkbn.
L,ihrary Committee — Messrs. HussBV and Sbarbs and Miss O'Halloran.
Committee on the Comet' Medal— y\^s&r&. Holdsn (ex-ojicio), Schabbbrlb, Campbell.
OPPICBRS OP THB CHICAGO 8BCT10N.
Executive Commit tee—fAr. Ruthvrn W. Pikb.
OPPICBRS OP THB MBXICAN SBCTION.
Executive Committee—Meun, Camilo Gonzalbz* Francisco Rodriguez Rby.
NOTICB.
The attention of new members is called to Article VIII of the By-Laws, which provides that
the annual subscription, paid on election, covers the calendar year only. Subsequent anntial
payments are due on January ist of each succeeding calendar year. This rule is necessary in
order to make our book-keeping as simple as possible. Dues sent by mail should be directed to
Astroooroicad Society of the Pacific Stg Market Street, San Francisco.
It is intended that each member of the Society shall receive a copy of each one of the PuS-
Hcatians for the year in which he was elected to membership and for all subsequent years. If
there have been (unfortunately) any omissions in this matter, it is requested that the Secretaries
be at once notified, in order that the missing numbers may be supplied. Members are requested
to preserve the copies of the Publications of the Society as sent to them. Once each year a title-
page and contents of the preceding numbers will also be sent to the members, who can then bind
the numbers together into a volume. Complete volumes for past years will also be supplied, to
members only, so far as the stock in hand is sufficient, on the payment of two dollars to either of
the Secretaries. Any non-resident member within the United States can obtain books from the
Society's library by sending his library card with ten cents in stamps to the Secretary A.S. P.*
819 Market Street, San Francisco, who will return the book and the card.
The Committee on Publication desires to say that the order in which papers are printed in
the Publications is decided simply by convenience. In a general way, those papers are printed
first which are earliest accepted for publication. It is not possible to send proof sheets of papers
to be print«l to authors whose residence is not within the United States. The responsibility for
the views expressed in the papers printed rests with the writers, and is not assumed by the
Society itself.
The titles of papers for reading should be communicated to either of the Secretaries as early
as possible, as well au any changes in addresses. The Secretary in San Francisco will send to
any member of the Society suitable stationery, stamped with the seal of the Society, at cost price,
as follows: a block of letter paper, 40 cents; of note paper, 35 cents; a package of envelopes, 35
cents. These prices include postage, and should be remitted by money-order or in U. S. postage
stamps. The sendings are at the risk of the member.
Those members who propose to attend the meetings at Mount Hamilton during the summer
should communicate with *'The Secretary Astronomical Society of the Pacific " at the rooms of
the Societ>^, Sio Market Street, San Francisco, in order that arrangements may be made for
transportation, lodging, etc
PUBLICATIONS ISSUED BIMONTHLY.
(February, April, June, August, October, December.)
publil library
ASTOn, LENOX AND
TIUKW WUNDA-nows.
PUBLICATIONS
Astronomical Society of the Pacific.
Vol. IX. San Francisco, Cal., June i, August i, 1897. No. 56.
A NEW OBSERVATORY (VALKENBURG, HOLLAND).
By Rev. John G. Hagen, S. J.
A small observatory has been erected at Valkenburg, Holland.
It consists mainly of an equatorial of nine-inch aperture, and
belongs to the Jesuit College of that city. The dome is con-
structed on the top of the building, at the northeast corner, the
walls having been built especially strong for the purpose. The
room under the dome contains a sidereal clock and switchboard,
with relays, sounder, and chronograph, thus affording connec-
doas with the equatorial, with an outside pier for time observa-
tions, and with the telegraph office of the city. The same room
serves as a library, which, it is hoped, will contain the publica-
tions of other observatories. This room, as well as the dome
and all parts of the equatorial, is lighted by electricity from the
dynamo of the college and a storage battery.
This new observatory has a special interest for Americans,
since the equatorial is entirely of American make: the mounting
by Mr. G. N. Saegmuller, and the optical part by Mr. J.
Clacey, both of Washington. The instrument had been espe-
cially constructed for and exhibited at the World's Fair in Chicago.
It has the latest improvements, and is exceedingly light, the
center-piece of the tube, the cell, and the eye-end being of alu-
minium. It contrasts very favorably with the clumsy mountings
of some instruments of equal or even smaller aperture in Euro-
pean obser\'atories. One of the finest features of the telescope
is its adjustment in azimuth and altitude, close to the polar axis.
Under this axis is the driving-clock, visible and accessible
122 Publications of the
through four glass doors, and provided with electric control.
The weights of this clock are inside the round iron pillar. Dec-
linations are set from the eye-end of the telescope by means of a
.microscope, and Right Ascensions directly (without the hour-
angle) on a dial, which is moved by a sidereal clock at the lower
end of the polar axis. Just under this dial is a small hand-
wheel for setting in R. A. The large base of the mounting is
under the floor, and the observing chair can be moved quite close
to the slender pillar. This chair was made by the carpenter of
the college, on the well-known plan of Professor Hough of
Chicago. The switchboard also presents an American appear-
ance. It is provided with the "spring -jacks " used in the West-
ern Union telegraph offices, and the connections of the wires are
arranged on the plan of the Harvard College, Georgetown Col-
lege, and Lick Observatories. The chronograph is of the Ameri-
can type, with cylindrical barrel, and was constructed by the
mechanician of the college, according to plans kindly furnished
by Mr. Saegmuller, who also made a present of the wheels
and governor for the driving-clock. The batteries are the
** Edison- Lalande," furnished by Bunnell & Co. of New York,
and are admired for their constancy and cleanliness.
The Dutch Ministry kindly allowed the free import of this
** telescope with accessories, for the sake of instruction." The
fitting-up of the observatory was intrusted to the Director of the
Georgetown College Observatory, Father J. G. Hagen, S. J.,
and his plan was to adapt it principally to the observation of
variable stars. The light construction and the comparatively
short focus of the instrument render it especially fit for this pur-
pose, and superior to any telescope now exclusively devoted to
this branch of astronomy. Its first Director, Mr. Jos. Hisgen,
S. J., is already known to the readers of the Astronomische
Nachricht€7i by his observations of variable stars, which he made
at the Georgetown College Observatory, in preparation for his
new position.
Astronomical Society of the Pacific. 123
THE SPECTRA AND PROPER MOTION OF STARS.
By W. H. S. Monck, F. R. A. S.
In the year 1892 I called the attention of the members ot
this Society to a connexion between the character of the stellar
spectra and the proper-motion of the corresponding stars,
which I afterward followed up in Astronomy and Astro-physics
and elsewhere. I had hoped that by this time the Draper
catalogue would have been extended to the Southern Stars,
which would have enabled this theory to be subjected to a wider
test. I recently met with a catalogue which seemed well suited
for a test, though, of course, I had only the original Draper
catalogue (with some corrections kindly supplied to me by Pro-
fessor Pickering) to refer to. This was Dr. Rambaut's cata-
logue of stars observed at Dunsink, consisting mainly of stars
with large proper-motion, which were observed with a view of
detecting the existence of considerable parallaxes not previously
noticed. Dr. Rambaut's limit was an annual motion of o".2
in a great circle; but, unfortunately, his catalogue does not con-
tain the entire number of such stars which are capable of being
observed at Dunsink (he appears to have limited himself to those
respecting which no previous parallactic researches had been
made), while it contains a number of stars with less than the
requisite amount of proper- motion, which were observed at the
request of Dr. Gill, Dr. Downing, and others; and no dis-
tinctive mark is applied to stars of this latter class. I soon found
that, to select from the catalogue of 717 stars, those whose
proper-motion amounted to o".2 and upwards would involve a
good deal of calculation, and I therefore selected instead those
whose proF>er- motion in Declination exceeded o". i. In doing
so, no doubt I omitted some stars with a proper-motion of up-
ward of o".2, but the omissions were not likely to make much
alteration in the relative proportions of the stars with different
spectra, with which alone I was concerned. Of the stars thus
selected, 92 proved to be Capellan (spectrum E, F, or G), 59
Arcturian (spectrum H, I, K, or L), and only 11 Sirian (spectrum
A, B, C, or D). There were very few stars with the spectrum M,
and these were all near the lower limit. Thirteen solar stars to
each Sirian star is rather a startling proportion, but had I adopted
124 Publications of the
o".2 as the motion in Declination, the result would have been
still more startling. There would have been ofie Sirian star
(marked doubtful in the Draper catalogue) to over eighty
solars. But Dr. Rambaut's stars were selected without any
regard to their spectra, and, I believe, without knowing what the
spectra were.
Further, I suspect that several of the eleven Sirian stars in
question will prove, on further examination, to be solar stars.
For they are usually faint stars, and the Draper catalogue often
expresses doubt as to the character of their spectra. Their num-
bers in the Draper catalogue are the following: 4637, 4989,
5207 (7 Sextantis), 5371, 7088, 8379 (iii Herculis), 9039, 9253
(56 Cygni), 9328 (5 Equu/ei), 9428, and 9842.
I had previously made a similar examination of the stars in
the PuLKOVA catalogue having a motion in Declination of over
o".i annually, but went over them a second time. These
stars, of course, included several whose total proper-motion fell
short of o". 2 per annum, whereas the selected stars from Dr.
Rambaut's catalogue contained very few. I obtained (neglect-
ing the notes of interrogation) 27 Sirian stars, 125 Capellan,
and 80 Arcturian. The general fact was thus the same as before.
I then tried the British Association catalogue for stars with a
proper-motion of o". i annually in Declination. The contrast
was less strongly marked, probably because several faint stars
are erroneously described as Sirian in the Draper catalogue.
But the three classes of stars came out in the same order, Capel-
lan first, Arcturian second, and Sirian third. This reverses the
order in which they occur in the Draper catalogue. The
Sirians largely outnumber the Arcturians, and the latter some-
what outnumber the Capellans. And taking the Pulkova cata-
logue and identifying as many stars as possible with the Draper
catalogue, I found that more than half were Sirians, and that of
the remainder the Arcturians outnumbered the Capellans. But
when I came to examine those with large proper-motion only,
the relative numbers were reversed. Nor are these Capellan stars,
on the average, of higher magnitude than the Sirians or Arc-
turians. The stellar magnitudes average about the same for all
three classes. The fact appears to be — however it may be
explained — that Capellan stars have, on the average, larger
proper-motion than Arcturians of the same magnitude, and that
Arcturian stars have, on the average, much larger proper-motion
Astronomical Society of the Pacific. 125
than Sirians of the same magnitude. The proportion of Capel-
lan stars having a proper-motion in Declination of o" , i annually
in Declination is ten times as great as that of the Sirians, and
twice as great as that of the Arcturians — at least, if we adopt
the PuLKOVA catalogue as the test. Such is the fact. How is it
to be explained ? Are the solar stars (and especially the Capel-
lans) moving through space with greater absolute velocity than
the Sirian stars? I believe not. There are two tests on this
subject: first, the spectroscopic results as regards motion in the
line of sight; and, secondly, the result of our investigations on
parallax. The latter can hardly be relied on at present, though
so far as they go they indicate a larger average parallax for solar
stars than for Sirians of the same magnitude. Vogel's results
as to motion in the line of sight appear more satisfactory, though
his hst of fifty-one stars contains but six Capellans. Their aver-
age motion is 9. 5 miles per second, which is somewhat less than
the general average. In fact, Vogel's observations would lead
us to think that all three classes of stars are moving through
space with nearly the same velocity. Another reason for arriving
at this conclusion is, that the effect of the Sun*s motion in space
can be traced just as easily in the case of stars with large proper-
motion as in the case of stars with small proper-motion; whereas,
if the former were really traveling with double or more than
double the usual velocity, the effect of the Sun's motion on them
would be comparatively small. Are the Capellan stars, then,
small stars or dull stars? The latter is, I believe, the true alter-
native. The great number of double-stars of this type which
are known to be binary tends to this result. The smaller the
mass of the pair, the slower will be the revolution of the satellite,
and the greater will be the difficulty in ascertaining the binary
character of the pair and determining the orbit. But I believe it
will be found that more than one half of the binary stars whose
orbits are approximately known belong to the Capellan type.
I pointed out, some years ago, a formula by which the luminosity
of two binaries can be compared with each other, assuming that
the larger stars were globes of equal density, and their compan-
ions very small, compared with them. The result of applying
this formula to the Sirian and Capellan binaries whose orbits were
supposed to be known was to show that the former were much
more luminous than the latter — probably five times as much so.
The Arcturian binaries were puzzling. They appeared to occupy
126 Publications of the
both extremes in the scale of luminosity. But the orbits assumed
for y Leonis and 6i Cygni were probably entirely wide of the
mark; and omitting these, they are certainly less luminous than
the Sirians; but their position as regards the Capellans is more
difficult to define. In fact, there are not enough of them to setde
it satisfactorily. I'here appear to be as many Arcturian as Capel-
lan double-stars, but among known binaries the latter are five or
six times as numerous. In like manner, Sirian double-stars are
numerous enough, but only a small proportion are known to be
binaries. That the vast majority of double-stars are binaries, a
careful examination will, I think, lead us to conclude; but good
observations on their positions being all of comparatively recent
date, we are still without means of proving thb fact when the
period is very long. Now, ceteris paribus ^ the greater the mass
of the pair, the shorter will be the time of revolution; and the
shorter periods of revolution in the case of the Capellan double-
stars go far to displace the theory that these stars are unusuaUy
small. Indeed, unless they are nearer to us than the others, we
should be driven to conclude that their masses were greater than
those of either the Sirians or the Arcturians. Capellan stars will,
I believe, prove not to be the smallest, but the least luminous
class of stars — least luminous, at least, relative to their density;
for there are some reasons for thinking that a Sirian star, instead
of presenting a much brighter surface than a Capellan of the
same mass, presents a much greater extent of surface. The
Capellan is rather denser than duller; but, mass for mass, it gives
much less light.
These results may not be inconsistent with a theory of stellar
development, but if so, it must assume a different form from that
which would naturally occur to us. If the Sirian, Capellan, and
Arcturian stars represent different stages of stellar development,
dependent on cooling and condensation, we must place the Capel-
lan stage last, not second. And if stars pass through what is
called the third type of spectrum (designated by M in the Dra-
per catalogue), they must do so before reaching the Caf>ellan
stage. Very few of the stars with this kind of spectrum possess
large proper-motion. The number which I have identified in the
PuLKOVA catalogue is under fifty, some of which are queried;
but only four of these have a proper-motion in Declination of
over o". I, thus giving a smaller percentage than even the Arc-
turians. Unless they are, on the average, larger stars than the
Astronomical Society of the Pacific. 127
Capellans, — and we would not be likely to find the largest stars
in the last stage of cooling — they are evidently more luminous,
relative to their density, and must, therefore, represent an earlier
stage of evolution.
The stars of the Orion type, designated B in the Draper
catalogue, have less proper-motion than even the ordinary
Sirians, denoted by A. On the development theory, they repre-
sent the earliest stage, while the Capellans represent the latest.
If we cannot represent the development as taking place in this
order, the stars must differ in kind — probably composed of dif-
ferent elements. One circumstance which rather favors the
theory of development is, that every star of the Algol type whose
spectrum I have succeeded in identifying — including those like
Spica Virginis and ^ Auriga, where no actual eclipse at present
takes place — are Sirians. On the tidal theory of satellite devel-
opment, the Algol type of stars belong to the earliest stage,
their satellites ultimately developing into the binary systems with
moderate periods, which are so frequently found among the
the Capellans. The duration of the eclipses in the case of these
Algol stars, compared with the intervals between them, indicate
a low density for these stars; and this character may not improb-
ably belong to all the Sirian stars. It is possible that, as they
become condensed by the cooling process, and their satellites
driven to a greater distance by tidal action, they may become
Capellans. But, then, where do the Arcturians come in? I can
oflfer no plausible theory on this subject.
In conclusion, I desire to point out that if Sirian stars are,
ceteris paribus, visible at a much greater distance than Arcturians,
and the latter visible at a greater distance than Capellans, we
must not regard the Draper catalogue as indicating the relative
frequency with which these classes of stars occur in space. Sup-
posing that the Sirians and Capellans were equally numerous,
and that both were uniformly distributed, but that the former
were (on the average) visible at double the distance of the latter,
we might expect to find eight times as many Sirians as Capellans
in the Draper catalogue. The actual proportion is about 2^
to I ; and the natural inference appears to be that the Capellan
stars are really more numerous than the Sirians. The apparent
numerical superiority of the latter is probably a delusive appear-
ance arising from their greater luminosity. And it is evident
that in the case of a distant cluster, a number of Sirian stars may
128 Publications of the
be distinctly visible when the light of their Capellan companions
is too faint to enable them to be observed separately. This fact
should not be lost sight of in speculations relative to the struc-
ture of the Galaxy. Certainly, among the nearer stars which are
in the same direction as the Galaxy, many (including the famous
o Centauri 2XiA 6i Cygni) are of the solar type. Is there any
valid reason for regarding the more distant stars in this direction
as almost exclusively Sirian ? I think not.
THE SPECTRA AND PROPER-MOTION OF STARS.
[supplemental note.]
By W. H. S. Monck.
Having obtained the spectra and proper-motion of a larger
number of stars than I had hitherto done by a comparison of the
British Association catalogue with the Draper catalogue, I
thought it desirable to take the different sub-classes into which
Professor Pickering divides the stellar spectra separately. I
found a sufficient number of stars with the following spectra to
render a comparison feasible; viz. A, B, E, F, G, H, I. K, and
M. I compared the proper-motions of the stars of these ty|>es
(rejecting, in the first instance, all those marked with a note of
interrogation in the Draper catalogue) in Declination or North
Polar Distance, only ascertaining what proportion of them had a
proper-motion of one tenth of a second annually in this direction.
All my percentages are somewhat too small, because the divisor
included some stars whose proper-motion is not given in the
British Association catalogue, but whose spectra I copied into my
note-book, with a view of subsequently ascertaining their proper-
motions from some other source, which I have not yet done.
The percentages which I obtained were as follows: —
Spectrum. Percentage of stars with requisite motion.
B CO
A 8.8
H 16.0
M 16.7
I 18.9
K 22.6
F 31.2
E 31.7
G 40.7
Astronomical Society of the Pacific. 129
The stars of this last type were not numerous enough to justify
the conclusion that the proper- motion is really greater than those
of the types E and F.
While the stars classed as A gave a percentage of 8.8, those
marked A? (of which there were over 130) gave a percentage of
12.8. This was to be expected, as the intrusion of stars of any
other type (except B) would increase the average proper- motion.
On the other hand, the stars marked F? gave only 22.6 per cent,
and those G? 25.0; but those marked E? gave the high percent-
age of 36.8. Classing E, F, and G, however, together as Capel-
^an stars, the unqueried Capellans gave a percentage of 31.8,
and the queried Capellans a percentage of 28.9, thus confirming
the result that the intrusion of stars of any other type among the
Capellans will reduce their average proper-motion. H ? gave a
percentage of 12.6, as compared with 16.0 for H; but I? and
K? gave 24.4 and 29.0 as compared with 18.9 and 22.6 for
unqueried stars of the same types. On the whole, if we desig-
nate the types H, I, and K as Arcturian, the queried Arcturian
stars gave a little more proper-motion than the unqueried. The
reverse is true of the type M. The extremely low proper-motion
of the stars of the Orion type B is remarkable. I had seventy-
five of them to compare, the proper-motions of seventy-two
being known. Not one of these had a proper-motion of one
tenth of a second in N. P. D., while out of twenty-seven stars
of the type G, no less than eleven possessed it. It will be seen
that the superior proper-motion of the Capellan stars over the
Arcturian (with which stars of the type M may be classed) is
quite as strongly marked as that of the Arcturian over the Sirian.
This diflference of proper- motion will, I think, be found to
arise not from the greater actual velocity, but from the greater
nearness (on the average) of the Capellan stars. The entire sub-
ject, however, calls for further investigation.
I30 Publications of the
THE SAYRE OBSERVATORY, SOUTH BETHLEHEM,
PENNSYLVANIA.
BV C. L. DOOLITTLE.
On the first day of September, 1866, occurred the formal
opening of the Lehigh University, at South Bethlehem, Penn-
sylvania. Professor Alfred M. Mayer, now connected with
the Stevens Institute of Technology, was the first professor of
astronomy, which department was then united with that of
physics.
Professor Mayer felt that the attempt to teach astronomy
with no instrumental means was most unsatisfactory, and mainly
through his eflforts, Mr. Robert H. Sayre, one of the most
prominent men of the place, and a trustee of the University,
became interested in the matter, and undertook to provide means
or a small observatory. The result was the founding of the
Sayre Observatory, in 1868.
The plan was not an ambitious one, the total cost of building
and instruments being only about $5000.00.
The equipment consisted of a six-inch equatorial, by Alvan
Clark & Sons; a portable transit instrument, by Stackpole;
a sidereal clock, by Brand; and, finally, an old zenith telescope,
which is said to have been rejected by the U. S. Coast Survey,
and which was purchased for a small sum, economy being a
matter of necessity. It was with this instrument, repaired by
Kahler in 1875, and afterward by Sagmuller in 1888 and
1892, that a series of latitude observations was carried on by the
writer for a number of years, the results of which, it is believed,
have been of some service in determining what is now known of
the law of latitude variation.
Professor Mayer was more interested in physics than in
astronomy, yet he found time for research work at the observa-
tory, mainly in the direction of solar physics. He was succeeded
in 187 1 by Hiero B. Herr, the chair of astronomy being now
connected with that of mathematics. Professor Herr retired in
1874, the vacancy being filled one year later by the election of
C. L. DooLiTTLE, who remained in charge for a period of twenty
years. He was succeeded, in 1895, by C. L. Thornburg, the
present incumbent.
The original purpose of the obser\'atory was that of instruc-
Astronomical Society of the Pacific, 131
tion, and this has always been a prominent feature of its work^
The university furnishes a very full course in astronomy, an
important feature of which b found in the practical work at the
observatory.
Considerable use has been made of the equatorial in the
observation of planets and comets, and the phenomena of JupU
ter^s satellites; but the most important contribution to astronomy
made by this observatory is the long series of latitude determina-
tions. This series came to an end in August, 1895, but it is
much to be desired that it should be resumed in the near future.
TOTAL SOLAR ECLIPSE, JANUARY 22, 1898.
ENGLISH PREPARATIONS.
By Edward W. Maunder, F. R. A. S.
The importance of total solar eclipses has led in England to
the appointment of a permanent body to organize their observa-
tions. This body bears the rather unwieldy title of the '* Joint
Permanent Eclipse Committee of the Royal Society and Royal
Astronomical Society." The title is, however, descriptive of its
constitution, and if we refer to it in future simply as the *' Eclipse
Committee,'* there need be no misunderstanding as to the body
indicated, and we may avoid repetition of this cumbrous name.
The expeditions sent out by the Eclipse Committee last
August were to widely separated countries, — ^Japan and Norway
— and included six principal observers. Three — the Astronomer
Royal, Professor H. H. Turner, and Captain Hills — went to
Japan; three — Professor Norman Lockyer, Mr. Fowler, and
Dr. A. A. Common — went to the Varanger Fjord, in Lapland.
The same observers, so far as can be at present foreseen, will go
to India for the eclipse of January next, and will take with them
the same instruments, and try to carry out the same programme
as that to which the clouds were so hostile on August 9, 1896.
For, one chief aim to be borne in mind in eclipse observation is
the necessity of strict continuity. If we are to get the maximum
result from the brief moments of totality afforded us at such long
intervals, then the operations to be undertaken at any one eclipse
must bear the strictest relation to the work done at the eclipses
that have gone before, and to the work proposed for those that
132 Publications of the
will follow. It is hoped, however, that the party on the next
occasion will be increased by two additional members; one will
probably be Mr. Newall, the observer with the great Newall
telescope at Cambridge; the other was to have been Mr. E. J.
Stone, the Radcliffe observer, whose untimely death has recently
left so serious a gap in the ranks of English astronomers. No
arrangement has as yet been made for supplying his place on the
expedition.
If we take the stations at present proposed to be occupied,
beginning with the most westerly, the first party we come to is
that of Professor Lockyer and Mr. Fowler, who will be sta-
tioned near Ratnagore, on the west coast. The equipment will
be chiefly spectroscopic, and will include two telescopes of nine
and six inches aperture, respectively, furnished with objective
prisms, the great success which attended this method in 1893,
and again in Mr. Shackleton*s observations in Novaya Zemlaia
in 1896 amply justifying great importance being attached to it.
An integrating spectroscope, having two three- inch prisms of
sixty degrees, will also be used. The method of observation
with all three instruments will, of course, be photographic, a long
series of photographs of varying exposures being used with the
objective prisms, whilst an exposure of sixty seconds will be
given with the integrating spectroscope.
The object of the prismatic cameras is, of course, to give the
details of the bright line spectra of the chromosphere, prominence
and corona, each several luminous point having its own distinct
spectrum. The integrating spectroscope, on the other hand, is
intended to sum up the spectrum of the whole composite phe-
nomenon. It may be hoped, therefore, that the feeble intensity
of the true coronal lines will be more than compensated by the
breadth of the area over which they are diffused. If, then, on
comparing the spectra obtained with these two widely differing
instruments, we find that the integrating spectroscope brings into
considerable evidence new lines beside those which the objective
prism reveals to us as characterizing the prominences, there can
be no hesitation in referring these new lines to the corona.
Crossing the Western Ghauts, the shadow-track intersects two
main lines of railway (the Southern Mahratta Railway and the
Great Indian Peninsular Railway), running southward from Bom-
bay through Poona. The points where these two railway lines
cross the line of totality will be very strongly occupied, but the
Astronomical Society of the Pacific. 133
precise spots are not as yet definitely fixed. Most likely, the
expedition sent by the Eclipse Committee will occupy the one
station, whilst a numerous band, organized in India itself by
Professor K. D. Naegamvala, of Poona, will occupy the other.
The official party in this region will consist of the Astronomer
Royal, Professor H. H. Turner, and Dr. A. A. Common. The
Astronomer Royal will take the Thompson photoheliograph of
nine inches aperture and eight feet six inches focal length, with
secondary magnifier placed a short distance within the focus,
giving an image of the Sun four inches in diameter. The
camera will be furnished with eight plate- holders, taking 12 x 10-
inch plates, and the instrument will be fed by a coelostat with a
sixteen-inch plane-mirror. Photographs will be taken of the
partial phase, as well as of the total.
Professor Turner's apparatus is the double camera used in
the West African expedition in 1893 by Sergeant Kearney.
The body of the instrument is six feet long, and consists of two
square tubes of yxy-inch section. In one is placed the **Abney''
photographic lens, of four inches aperture and ^\^ feet two inches
focal length, used in so many eclipses, and which gives an image
of the Sun 0.57 inch in diameter; in the other, the photohelio-
graph objective No. 2, belonging to the Royal Observatory,
Greenwich, and used in the Transit of Venus Expedition of 1874,
and which is also of four-inch aperture and five feet focal length,
but which is to be used with a Dallmever secondary magnifier
of seven and one half inches focus, placed ^v^ inches within the
focus, so as to give an image of the Sun one and one half inches
in diameter. The double camera is furnished with six plate-
holders, each taking two plates of 160 mm. square, both plates
being exposed by a quarter turn of one shutter. The double
camera, like the Astronomer Royal's instrument, will be fed by a
sixteen-inch plane mirror, on a coelostat mounting. A similar
instrument was to have been placed under the charge of the late
Mr. Stone at the third station. This instrument was taken by
Dr.* Common, in 1896, to Lapland.
Apart from this, it is probable that Dr. Common's equipment
will be the same as that which he had in Norway last year; i. e.
a six-inch doublet lens, by Grubb, lent by Mr. F. Maclean,
F. R. S., and giving an image of the Sun three and one half
inches in diameter; a slit spectroscope, with 3}^ -inch lenses,
and two light flint prisms of sixty degrees, and a grating
134 Publications of the
spedtroscope, to be used without a slit. The plates for Mr.
Christie's coronal photographs, Dr. Common's photographs
with the six-inch Grubb, and those with the grating spectro-
scope, are all to be 12x10 plates.
The third station, at Wardha, on the Great Indian Peninsular
Railway line from Bombay to Nagpur, will be occupied by Mr.
Newall, who proposes to use a large slit spectroscope, with two
prisms of sixty- two degrees, in the attempt to determine the
speed of rotation of the corona by the relative displacements of
its lines as observed east and west of the Sun. In the same
neighborhood, Captain Hills will probably fix his apparatus,
which will consist of two slit spectroscopes, having the slit tan-
gential to the Sun's limb at the point of second contact, and
diametral respectively. The slits are lyi. x 0.004 inches, and
2x0.004 inches respectively; and the prisms are, for the first
spectroscope, of two flint prisms of sixty degrees, 4^ -inch base,
2)^ -inch height at minimum deviation for Hy\ and for the second
spectroscope, of four quartz prisms of sixty degrees, 3^ -inch
base, 2^ -inch height at minimum deviation for Ht, The colli-
mator and camera lenses are single quartz lenses, of 2^4 -inch
aperture, 30-inch focus and 3-inch aperture, 36-inch focus respec-
tively. The objectives are all achromatic Cooke lenses, of 4j4-
inch aperture, 5 feet 10 inches focus, and a single quartz lens of
5-inch aperture, 4 feet 9 inches focus.
Professor Turner's equipment in Japan also included a
polariscopic apparatus, consisting of an ordinary slit spectro-
scope, with an Iceland spar double image prism substituted for
the ordinary prisms. This will probably again be included in
his armory.
Some thirty or forty amateur astronomers belonging to the
British Astronomical Association will also proceed to India, and
divide into four companies, stationed near the four above-men-
tioned sites respectively, but the precise programmes to be
adopted cannot be ascertained at present.
Astronomical Society of the Pacific. 135
EARTHQUAKE OF JUNE 20, 1897 (OAKLAND).
By Allen H. Babcock.
A prolonged shock of earthquake was observed here to-day,
commencing at 12** 13" 9* P. M., P. S. T., and continuing for at
least twenty-five seconds. It was noticed first as a sharp settling
of the floor; then came a rumbling sound, followed by a slow,
swaying motion, which gradually increased in strength and fre-
quency for about ten seconds, when the maximum was reached.
At this time the vibrations were decidedly marked: the house
creaked, the windows rattled, and the pictures bumped against
the walls. The swing of the chandeliers was in an approximately
north and south line. The vibration gradually diminished, until
12* 13" 34", when they could no longer be observed. In a
jeweler's shop, about two blocks away, a pendulum clock, which
was fastened on a wall running in an east and west direction, had
stopped at 12** 13" 27". This clock is usually kept very close to
standard time.
The intensity of the shock at its maximum may be estimated
at IV, or possibly V, on the Rossi-Forel scale. Two persons
report a very faint shock about fifteen minutes later, but it was
not observed by me.
Oakland, Cal., June 20, 1897.
2826 California Street, >
San Francisco, June 23, 1897. j
. . . On Sunday, June 20th, at 12:13 p. M., I felt a slight
shock of earthquake, location N.W. ^ Section 32, Township 17
S., Range 14 E., M. D. B. & M., on Cantua Creek, Fresno County.
Duration about fifteen seconds; 9 shock; undulation and whirling
motion. Yours respectfully, S. C. Lillis.
136 Publications of the
PLANETARY PHENOMENA FOR JULY AND AUGUST,
1897.
By Professor Malcolm McNeill.
July, 1897.
Solar Eclipse, There will be an annular eclipse of the Sun
on July 29th, visible on the morning of that day throughout the
United States as a partial eclipse. The path of the annulus
begins in the Pacific Ocean, crosses Mexico, skirts along the
north shore of Cuba, just touches the northeast point of South
America, and ends in the South Atlantic The greatest duration
of the annulus is considerably less than two minutes.
The Earth is in aphelion on the afternoon of July 9th.
Merairy is a morning star at the beginning of the month,
rising a little more than an hour before sunrise, and may possibly
be seen. It rapidly approaches the Sun, and passes superior
conjunction on the afternoon of July 15th, and becomes an even-
ing star. By the end of the month it is about as far from the Sun
as it was at the beginning, but it is ako too far to the south to be
easily seen as an evening star.
Venus is a morning star, and comes to its greatest west elonga-
tion on July 7th. It rises about three hours before sunrise. It
moves thirty-one degrees eastward and five degrees northward
during the month, almost entirely in the constellation Taurus,
and a little before the middle of the month passes through the
Hyades group, between c and 8 Tauri.
Mars is well out on his way to conjunction with the Sun, and
his apparent distance from the Sun is diminishing rapidly. By
the end of the month it sets before 9 p.m. It moves seventeen
degrees eastward and seven degrees southward in the constella-
tion Leo during the month. On July 5th it passes about one
degree north of the first magnitude star Regiilus (a Leom's), and
is in conjunction with Jupiter on the morning of July 25th. Mars
is only seven minutes south of Jupiter at the time of nearest
approach, but this occurs by daylight in the United States.
Jupiter is in the same quarter of the sky as Mars, and is
moving in the same general direction but very much more
slowly, the whole motion being only about five degrees during
the month. Its conjunction with Mars is noted above.
Astronomical Society of the Pacific. i37
Saturn is in good position for observation, being above the
horizon until after midnight until nearly the end of the month.
It is in the constellation Libra, and moves westward about one
degree until July 28th, when it begins to move eastward again.
The rings are widely opened, the ratio of minor to major axis
being about 0.40.
Uranus is very near Saturn, about two degrees south and
a little east, and is moving in the same general direction as
Saturn^ but does not stop its retrograde (westward) motion until
August 2d. It may be easily found on any very clear, moonless
evening as a small sixth magnitude star, about four diameters of
the Moon, south and east of Saturn,
Neptune is a morning star in the eastern part of Taurus,
Venus passes it about one degree south on the morning of
July 28th.
" August.
Mercury is an evening star, and sets about an hour after
sunset during the greater part of the month. It may possibly be
seen during good conditions of weather in the evening twilight.
It reaches greatest east elongation on August 26th, more than
twenty-eight degrees, its greatest apparent distance from the Sun
during the year; but the conditions for evening visibility are not
nearly as good as they were during the elongations of January
and April, on account of its greater distance south of the Sun.
It is in conjunction with Jupiter on the evemqg of August 12th,
passing about two diameters of the Moon southward.
Venus is a morning star, rising about three hours before the
Sun. It moves about thirty-six degrees eastward, through the
|X)nstellation Gemini into Cancer, and will not be nearly as bright
as it was during the early summer.
Mars is rapidly approaching the Sun, and by the end of the
month it sets only about an hour later. It has lost the greater part
of its brightness, and will not be at all a conspicuous object, but
rather hard to see toward the close of the month. It moves about
eighteen degrees east and south, through the constellation Leo,
Jupiter is still nearer the Sun than Mars, and its much smaller
eastward motion allows the Sun to approach it much more
rapidly. It cannot easily be seen much later than the middle of
the month.
Saturn is still in fair position for observation in the south-
138 Publications of the
western sky in the early evening. It moves about one degree
eastward in the constellation Libra, It is in quadrature with the
Sun on August i6th.
Uranus keeps up about the same position relative to Solum
as during July, but is more nearly due south, about four diameters
of the Moon distant. The two planets are in conjunction on the
evening of August 25th.
Neptune is in the eastern part of Taurus^ and rises before
midnight at the end of the month.
Explanation of the Tables.
The phases of the Moon are given in Pacific Standard time.
In the tables for Sun and planets, the second and third columns
give the Right Ascension and Declination for Greenwich noon.
The fifth column gives the local mean time for transit over the
Greenwich meridian. To find the local mean time of transit for
any other meridian, the time given in the table must be corrected
by adding or subtracting the change per day, multiplied by
the fraction whose numerator is the longitude from Greenwich
in hours, and whose denominator is 24. This correction is
seldom much more than i". To find the standard time for the
phenomenon, correct the local mean time by adding the differ-
ence between standard and local time if the place is west of the
standard meridian, and subtracting if east The same rules apply
to the fourth and sixth columns, which give the local mean times
of rising and setting for the meridian of Greenwich. They are
roughly computed for Lat. 40°, with the noon Declination and
time of meridian transit, and are intended as only a rough guide.
They may be in error by a minute or two for the given latitude,
and for latitudes differing much from 40** they may be several
minutes out.
Phases of the Moon, P. S. T.
1897.
July I.
II.
21.
31-
First
Full
Last
New
Quarter, July 7,
Moon, July 13,
Quarter, July 21,
Moon, July 28,
The Sun.
5 32 A. M.
8 52 p. M.
7 8 A. M.
7 58 A. M.
R. A.
Declination. Rises
Transits.
Sets.
H. M.
® ' H. M.
H. M.
H. M.
6 43
+ 23 6 4 41 A.
M. 12 4 P.M.
7 27P.M.
7 24
+ 22 3 4 46
12 5
7 24
8 4
8 AA
+ 20 23 4 53
-^18 9 5 3
12 6
12 6
7 19
7 9
Astronomical Society of the Pcuific. i39
Mercury.
R. A.
Declination.
Rises.
Transits.
Sets.
1897.
H.
M.
'
H. M.
H. M.
H.
M.
July I.
5
34
+ 22
35
3 33 A.M.
10 54A.M.
6
15 P.M.
II.
7
2
+ 23
45
4 16
II 43
7
10
21.
8
32
-l- 20
43
5 20
12 34 P.M.
7
48
31.
9
48
+ 14
46
6 20
Venus.
I II
8
2
July I.
3
31
+ 15
36
I 58 A.M.
8 52A.M.
3 46 P.M.
II.
4
10
+ 17
41
I 49
8 51
3
53
21.
4
51
+ 19
29
I 45
8 54
4
3
31.
5
36
+ 20
46
I 44
Mars.
8 58
4
12
July I.
9 53
+ 14
4
8 26 A.M.
3 14P.M.
10
2 P.M.
II.
10
17
+ 11
52
8 17
2 58
9
39
21.
10
40
+ 9
32
8 8
2 41
9
14
31.
II
3
+ 7
6
8 I
2 25
8
49
Jupiter.
July I.
10
33
+ 10
18
9 18 A.M.
3 53P-M.
10
28 P.M.
II.
10
39
+ 9 39
8 47
3 20
9
53
21.
10
46
+ 8
58
8 17
2 48
9
19
31.
10
53
+ 8
14
7 48
2 16
8
44
Sa turn.
July I.
15
32
- 16
50
3 50 P.M.
8 51 P.M.
I
52 A.M.
II.
15
30
— 16
48
3 9
8 10
I
II
21.
15
29
- 16
47
2 29
7 30
12
31
31.
15
29
- 16
49
I 49
6 50
II
51 P.M.
Uranus.
July I.
15
33
- 18
55
3 59PM.
8 52 P.M.
I
45 A. M,
II.
15
32
— 18
52
3 18
8 II
I
4
21.
15
31
- 18
50
2 38
7 31
12
24
31.
15
31
- 18
49
I 59
6 52
II
45 P.M.
Neptune.
July I.
5
20
+ 21
48
3 23 A.M.
10 41 A.M.
5
59 P.M.
II.
5
22
+ 21
50
2 45
10 3
5
21
21.
5
23
-)-2t
51
2 7
9 25
4 43
31.
5
24
+ 21
52
I 29
8 47
4
5
Eclipses of Jupiter 's Satellites, P. S. T.
(Off right hand limb as seen in an inverting telescope.)
H. M. H. M.
July 19. 6 53 p. m.
19. 10 4 P.M.
22. 5 18 p. M.
29. 7 13 P.M.
I.
R,
July 6.
7 p. M.
Ill,
D,
IV,
D.
9-
6 31 P. M.
HI,
R,
IV.
R,
9-
10 10 P. M.
I,
R,
III.
R.
12.
6 5 P. M.
I,
R,
I,
R,
13-
8 55 P.M.
I40 Publications of the
Minima of Algol, P. S. T.
July 3-
6.
9.
12.
15.
Phases of the Moon. P. S. T.
H. M.
First Quarter, Aug. 5, 10 24 A. M.
Full Moon, Aug. 12, 6 23 a. m.
Last Quarter, Aug. 20, 12 29 A. M.
New Moon, Aug. 27, 7 29 p. m.
H.
7
3^4 P. M.
July
18.
4
23 P. M.
21.
1
12 P. M.
23.
10
I A. M.
26.
6
50 A. M.
29.
H.
M.
3
38 A. M.
12
27 A. M.
9
16 P. M.
6
5 P- M.
2
54 P. M.
The Sun.
R. A.
Decllna
Lion.
Rises.
Transits.
Sets.
1897.
H. M.
c
t
H. M.
H.
M.
H.
M.
Aug. I.
8 47
+
17
54
5 3 A.M.
12
6 p.m.
7
9 P.M.
II.
9 26
+
15
8
5 13
12
5
6
57
21.
10 3
+
II
57
5 22
12
3
6
44
31.
10 40
H-
8
28
5 32
12
OM.
6
28
Mercury.
Aug. I.
9 55
+
14
6
6 26 A.M.
I
14 P.M.
8
2 P.M
II.
10 54
+
7
12
7 9
I
33
7
57
21.
II 41
+
37
7 38
I
40
7
42
31.
12 13
—
4 40
7 50
I
34
7
18
Venus,
Aug. I.
5 40
+
20
52
I 43 A.M.
8
58 A.M.
4
13 P.M
II.
6 27
+
21
21
I 50
9
6
4
22
21.
7 16
+
20
58
2
9
15
4 30
31.
8 4
+
19
40
2 15
Mars.
9
25
4
35
Aug. I.
II 5
+
6
51
8 OA.M.
2
23 P.M.
8
46 P.M
II.
II 28
+
4
18
7 53
2
7
8
21
21.
II 51
+
I
42
7 45
I
51
7
57
31.
12 15
—
56
7 38
I
35
7
32
Jupiter.
Aug. I.
10 54
+
8
9
7 45 A.M.
2
12 P.M.
8
39 PM
II.
II 2
+
7
22
7 15
I
40
8
5
21.
II 9
+
6
34
6 47
I
9
7
31
31.
II 17
+
5
44
6 18
12
37
6
56
Sa turn.
Aug. I.
15 29
—
16
50
I 46 P.M.
6
47 P.M.
II
48 P.M.
II.
15 30
—
16
54
I 7
6
8
II
9
21.
15 31
—
17
I
12 29
5
30
10
31
31- 15 33 —17 10 II 51A.M. 4 52 9 52
Astronomical Society of the Pacific.
141
Uranus,
R. A.
Declination. Rises. Transits.
Sets.
1897.
H. M.
« H. M.
H. M.
H. M.
Aug. I.
15 30
— 18 49 I 55 P.M.
6 48 P.M. II 41 P.M.
II.
15 31
— 18 50 I 16
6 9
II 2
21.
15 31
- 18 52 12 37
5 30
10 23
31-
15 32
- 18 55 II 59 A.M.
Neptune,
4 52
9 45
Aug. I.
5 24
+ 21 52 I 25 A.M.
8 43^
A.M. 4 I P.M.
II.
5 25
+ 21 52 12 47
8 5
3 23
21.
5 26
+ 21 53 12 9
7 27
2 45
31.
5 27
+ 21 53 II 30 P.M.
Minima of Algol, P. S.
H. M.
6 48
T.
2 6
H. M.
Aug. I.
II 43 A. M. Aug. 18.
4 36 p. M,
4-
8 32 A.M. 21.
I 25 p. M.
7-
5 21 A. M. 24.
10 14 A. M
10.
2 9 A. M. 27.
7 3A.M
12.
10 58 P. M. 30.
3 52 A. M
15.
7 47 P. M.
DOUBLE-STAR MEASURES.
By D. A. Lehman.
The following measures were made with the 12-inch equa-
torial of the Lick Observatory. The position angle is the mean
of four settings, and the distance that of three double-distances.
The position of the stars is given for 1880.0. In estimating
seeing, a scale is used on which 5 stands for the most favorable
conditions. The eyepiece used in most of the measures has a
power of 500 diameters; but some of the measures were made
with lower powers.
2 1788. (6.7-8).
R. A. 13" 48" 43'. Decl. — 7° 28^
«o
Po
Seeing.
1897.460
73°.9
3". 37
3
1897.465
76.1
2 .98
3+
1897.477
75 -2
3-62
4
1897.492
77 -5
3 -23
4
1897.47
75^7
3". 30
142 Publications of the
2 1930.
(5-10).
R.
A. 15' 13- \i:
Decl.
+ 2' 13'.
»o
Po
Seeing,
1897.460
38°. 7
"".35
3
1897.492
37.6
II .04
4
1897.494
37 -5
10 .57
4
1897.48
37°-9
io".99
2 2021 (49 Serpent's). (6-7).
R. A. 16" 7- 43'. Decl. + 13** 48^
«o
Po
1897.460
332°. 9
3".97
1897.492
333 -9
4 .27
1897.514
335 -7
4 .29
1897.49
334°. I
4". 18
Sh
228 Ophiuchi).
(5-7).
R. A. 16' i8" 33*. Decl. -
- 23» I</.
»o
Po
1897.508
354°.6
3".6o
1897.516
354 -4
3 -59
1897.519
353 .1
3 .12
1897.51 354''.o 3".44
2 2055 (A Ophiuchi), (4-6).
R. A. 16" 24- 52'. Decl. + 2° I5^
seeing.
3
4
3
Seeing.
3
4
4
h
Po
Seeing.
1897.522
53°. 3
I ".69
4
1897.525
52.8
1 .63
4
1897.52
53°.o
I ".66
"0
Po
1897.514
1 89°. 3
i4".93
3
1897.519
190 .1
15 -to
4
1897.522
190 .2
15 .17
4
1897.52 189^.9 i5".o7
Astronomical Society of the Pacific. i43
/3 416. (6-8).
R. A. 17'' 10- 46*. Decl. — 34** 51^
^o Po Setring.
1897.508 310° 6 i".90 4
1897-519 311 -o I .77 4
1897.522 309 .2 I .88 4
1897-525 309 -8 I .89 4
1897.52
310°. 2
i".86
2 2262 (t Ophiuchi).
(5-5- 7).
R,
. A. 17' 56"
33'.
Decl.
— 8° II'.
Seeing.
1897.508
259°- 1
2". 2 1
3
1897.514
256 .0
2 .15
3
1897-525
258 .2
I .88
4
1897.52
257°.8
2".o8
S
2272 (70 Ophiuchi).
(4-6).
R.
A. 17' 59"
23'.
Decl.
+ a» 33'.
Po
Seeing.
1897.476
286° 2
2". 74
3
1897.492
280 .7
I .91
4
1897.508
283 .9
2 .60
4
1897.49 283°6 2".42
(Y CoroncB Australis), (5/^-5/4)-
R. A. 18' 58- i8'.
Decl.
-37° 14'.
»o
Po
1897.508
1 58°. 6
2". 1 2
1897.525
155 -o
I .79
1897.52 I56°.8 i".95
2 2579 (8 Cygni). (3-8).
Seeing.
4
4
R.
A. 19' 41-
13".
Decl.
+ 44° 50'.
Pa
Seeing.
1897.508
301°. 2
2". 25
4
1 897.5 1 1
300 .1
I .72
1+
1897.525
305 .1
I .77
4
1897.52
302°. I
i".9i
144 Publications of the
1897.508
1897-525
S2583. (6-6.8).
R. A. 19" 43" 3'. Dec!. -1- ii" 31'.
ii5°.o i".90
113 -2 I .53
S«eing.
4
4
1897-52
1 14°. I l".72
I897.5U
1897-525
/? 151 (/J Delphini). {yA-^Yz).
R. A. ao'si'ss". Decl. + 14° ii'.
K Po
359°-9 o".75
355 -2 .93
Seeing.
3
3
1897-52 357°.6 o".84
Lick Observatory, July 10, 1897.
-■FN rj,,-^M .r'0\3.
Astronomical Society of the Pacific. 145
NOTICES FROM THE LICK OBSERVATORY,*
Prepared by Memrers? of titk Staff.
A New Celestial Atlas.
AxLJiS DER HiMMELSKUNDE — Atlas of Astronomy, based on
€*lesiial photographs — sLxty-two atlas sheeLs, with 135 single
plates and sixty folio sheets of text, containing about 500
illusinilions — by A. VON ScHWHlKacR-LKRCHENFRUD, Pub-
Ibhcii by A. Hartlebek, Vienna, in tsixty parts (issued
twice a month), at thirty- live cents per j>art»
B*iron VON Schweiger-Lerchenfeld proposes to publish,
as above, a folio atlas (about 11 ^j by [6 inches), to rcpre^^eni the
pr^eiTt condition of Celestial Photoj^^raphy — its instrument's,
metbods, and results. The illustrations, over 600 in all. are to
be supplemented by the text, also from Baron vox ScnwniiGKR-
LeRCHENFELD*S hand. Modern instruments and observatories
arc to be represented by some 200 reproductions of photojtirafilis
Rimished to the author by the directors of varirius American and
forcig:n observatories^ or by the in*^iru men t- makers whu actually
cofisiructed the apparatus, A very Iarj:;e proportion of these illns-
tiations is new. Something like a tiiird of tht.^ volume is devtitecl
to obstervatories and instruments. The r niainini; [>lates are moslly
reproductions of original negatives of tht^ Sun, Mmou. planets,
comctii, meteorites, stars, clusters and net Hike, etc. (and oi their
fpectra), furnished to the audio r by the observatories of Mt. Ham-
ilton, Paris* Praj^ue, PoLsdam, Heidelberg, etc. A few on.^inaI
astronomical drawings {o{ .^fars, etc. ) are included ior complete-
Ofcss, as well as maps of the stars, planispheres, etc* A circular
relating to the atlas was distributed by HAKriJ:nr:x in April last,
and it contains plates of the Milky W.iy (tiikeu at lieidclbtTcif),
* Ock AttroDomiul Depart meiu oi the Unlv^tsitv nj Oihroniiri,
146 Publications of the
the Moon (Paris Observatory), instruments (Pulkowa and George-
town), the Sun (Potsdam and Meudon), Mars (drawing by
Professor Hussey at the Lick Observatory), and of the Algerian
meteorite of 1893 (full size). The illustrations of the atlas are
very satisfactory, and the descriptions of the text supplement
them fully.
Smce the foregoing was written, the first part of the Atlas
has been received, and it confirms the favorable opinion expressed
in what precedes. Many of the reproductions are made by the
half-tone process. When these are compared with the original
negatives, or with direct copies from the negatives, they naturally
show less fineness and detail. Only a few observatories and
astronomers can have access to such originals, however. The
present work is intended to meet the wants of the hundreds of
readers to whom such access must always be closed. Its chief
value will be in this regard. Its very complete collection of
plates relating to instruments will be important to all, profes-
sionals and amateurs alike. It is now, for the first time, possible
for the general reader to possess a work which gives an adequate '
account of the present state of celestial photography. Through
the kindness of Baron voN Schweiger-Lerchenfeld, several
illustrations from his text are reproduced in the present number of
the Publications, It may not be out of place to say that the cost
of the Atlas, plates, etc., has been some $20,000.
Edward S. Holden.
May 10, 1897.
Meteor Seen at Mt. Hamilton (May 5, 1897).
On the evening of May 5, 1897, at 7^30" P. S. T., Mr.
Nicholas D. Soto, an employ^ of the Lick Observatory, called
my attention to a very bright meteor-trail, the remnants of an
explosion, which Mr. Soto observed at about "f 26". The gen-
eral direction of the zigzag trail was nearly horizontal (the north
end was perhaps 5' higher than the west end), and about 1° long.
It was seen by nearly all the astronomers of the Lick Observa-
tory. I made two sets of altitude and azimuth determinations
of the brightest portion (extreme west end of the trail) from a
point near the northeast corner of the main residence building.
Azimuth of extreme west end, N. 51^42' W. ) ^ „
Altitude of extreme west end, 3 30 \ i o^ -
PHOTOGRAPHIC EQUATORIAL OF THE MOSCOVV OBSERVATORY.
(Camera-leiis, 4 inches aperture; plales about 9V7 x ii5^ inches; notice llial the declination axis is itself a Iclescop
of 2,'i inches aperture.)
(Atlas (ler Hinimelskunde.)
Astronomical Society of the Pacific. i47
Another set of measures, made at 7** 48™, gave the same
co-ordinates. After 7^ 50"*, the matter became too faint for fur-
ther measures. The peculiarly vivid whiteness of the meteoric
cloud was similar to that of the great meteor of July, 1894.
J. M. SCHAEBERLE.
Lick Observatory, May 6, 1897.
Stability of the Great Equatorial, 1888-1897.
Observations for the position of the great telescope have been
made by Messrs. Schaeberle, Keeler, Campbell, Tucker,
and CoLTON, as below: —
1888, July 27, azimuth +36"; level 8" too low,
1889, May 18, •* .... ; " 36
Sept. 16, " +83 ; - 58
1890, Aug. 23, '* (+54); " 114
Telescope adjusted.
1 89 1, June 30, azimuth .... ; level 35" too low.
Holding-down bolts tightened.
1892, Aug. 5, azimuth +51"; level 25" too high,
1893, Sept. 23, '' +48; ** 57 too low,
1896, Dec. 5, ** ....;** 74
1897, Apr. 24, *' +60 ; '* ..
E. S. H.
Measures of Procyon,'^ by William J. Hussey.
The following measures of Schaeberle's companion to
Procyon have been made with the 36-inch teleScope, using a
power of 520 . . . : —
1897.072 />— 3i9°23 ^ = 4"- 58
.203 320 .06 4 .77
.206 320 .01 4 .59
1897.16 3 1 9°. 8 4". 65
Reflector and Portrait Lens in Celestial Photo-
graphy.
Those who are interested in the technical points suggested by
the above title cannot do better than to refer to a nearly exhaust-
ive discussion of them by Professor Max Wolf in Nature for
• From the Astronomical Journal, No. 403.
14^ Publications of the
April 22, 1897, pp. 582-586, and to the illustrations given there.
I venture, in this connection, to mention remarks printed in these
Publications, Vol. Ill (189 1), p. 249, Vol. VI (1894), p. 24,
which relate to the problems discussed by Professor Wolf in
the paper cited. E. S. H.
Dedication of the Flower Observatory, University
OF Pennsylvania.
On the afternoon of May 12th took place the exercises which
marked the practical completion of the above-named observa-
tory, though observations have been going on regularly there
since last October.
The ceremony of the dedication was not elaborate, but all
present appear to have found it very enjoyable.
A platform had been erected in front of the equatorial build-
ing for the accommodation of the speakers. In front were
seated about four hundred invited guests.
Provost C. C. Harrison, of the University, in a short intro-
ductory address, presented the speaker of the day, Professor
Simon >Iewcomb. Provost Harrison gave a brief oudine of
the bequest of the founder, Reese Wall Flower. This con-
sists of one hundred acres of valuable land adjoining the city of
Philadelphia, and upon which the observatory now stands. It is
not known how Mr. Flower came to make this bequest, as he
had never showed any special interest in astronomy.
Professor Newcomb gave a very interesting paper upon **The
Problems of Astronomy,** which was followed by short addresses
of an informal nature by Dr. W. R., Warner, Mr. Brashear,
Miss Proctor, Dr. Barker, and C. L. Doolittle.
The exercises were followed by a very enjoyable reception at
the residence of the Director.
Record of Experiments with the Moving Floor of the
75-FOOT Dome of the Lick Observatory.
The following summary of experiments with the moving floor
of the 75 -foot dome may appropriately be recorded here. The
original data are scattered in various places, and if brought
together, they will be useful in subsequent comparisons.
The idea of a moving floor was first suggested to the Lick
Trustees by Sir Howard Grubb, F. R. S. The floor was to rise
1 ;,6''OR, LENOX AND
T LDEN FOUNDATIONS.
Astronomical Society of the Pacific. i49
1634 feet. Four nuts were fixed to its edge, and four vertical
screws in tbem were to be driven by a three-cylindered water-
engine in the basement. The available pressure was only
seventy- two pounds per square inch. This plan was tried
(against my advice) and failed; The floor never could be made
to rise its whole height in less than an hour (approximately).
The screws were taken out in May, 1888, and the floor was lifted
by four hydraulic jacks. The supply of water to these jacks
was regulated by four lock- valves, whose scales were divided into
six fjarts. Up to 1895 these were used % open.
May ^r, 1888. — Floor moves down in 5" 45' (i6>^ feet); up
in 1 2" o". Five hundred pounds were then added to the counter-
weights.
June 75, 1S88, — Floor moves down in 5" 33'; up in 7"* 43'.
Experiments between 1888 and 1895 are not here sel down.
August 28, j8(^§. — Valves yi open; the floor moves down
in 5" 42'; I// in 9" 30'. The heavy mahogany chair (needed in
most photographic work) was then removed from the floor. The
floor moved down in 6°*4o'; up in 9"* lo'. About this time the
capacity of the waste pipes from the jacks was increased. The
capacity of the supply pipe should also be increased, but it has
not been done, on account of the expense.
August 79, 18^6, — Valves wide open; floor moves down in
5" 20* ; up in 10" 30'.
April 2^^ i8gj, — Added 592 pounds of lead to the counter-
weights of the moving floor. The valves were V^ open. After
adding the extra weights, the floor moved down in 6"* 30', and up
in 9" 2o'. The valves were then opened wide, and the floor
moved down in 5" 5'; up in 9"* 30'. The valves were left wide
open. The packing of the rams will account for small differences
in time, according as it is tight or loose. The jacks, on the
whole, do not work as efficiently in 1897 as in 1888. This is
probably due to the fact that they are not absolutely vertical,
especially in the upper eight feet of their play. One single ram
of the proper length would have been a better device than the
present telescopic arrangement. All the other machinery of the
moving floor (see Engineering, Vol. 46, p. 204, 1888) is now in
excellent order. Edward S. Holden.
April 30, 1897.
ISO Publications of the
Statistics of the Library of the Lick Observatory.
A count, made on May 31, 1897, of the books and pamphlets
in the library of the Lick Observatory, shows —
41 21 books,
3912 pamphlets,
as against
2885 books,
3343 pamphlets,
in March, 1892.
A comparison of the two counts of pamphlets is classified
below: —
PAMPHLETS.
Drawbr March, May, Drawkr March. May,
URAWBR. jg^2. 1897. URAWRR. ^^^ ^^
X. Mathematics 51 87 26. Proper Motions 30 a*
2. Mathematical Tables i 4 27. Observatories, Reports of 121 243*
3. Cosmology 52 74 28. Miscellaneous Astronomi-
4. Spherical Astronomy — 16 19 cal Observations 70 120*
5. Theoretical Astronomy... 73 113 29. Chemistry and Mechanics 11 37
6. Theory of Instruments .. 78 63* 3a Heat, Sound, Electrics ... 73 150
7. Chronology 6 33 , 31. Optics, etc 73 43*
8. Catalogues of Stars 56 49* 32. Meteorology 109 32*
9. Ephemerides 26 91* 33. Meteorological Observa-
10. Astronomical Tables 31 46* tions 166 8*
11. Geodesy 55 33* 34. History of Astronomy — 157 183*
12. Determination of Geo- 35. Astronomical Biography. . 156 87*
graphical Positions.... 55 no* 36. Astronomical Bibliography 124 133*
13. Metrology 16 27 , .37. Comets and Meteors 161 72*
14. Earthquakes, and Geogra- 38. Spectroscopy 58 62*
phy 75 67* 39. Photography 109 144
15. Refraction 6 8* 40. Star Maps 31 26*
16. Sun, Zodiacal Light 103 73* 41. Geography and Maps 69 67*
17. Solar Eclipses 97 60* 42. Time Service 77 87
18. Moon . 72 86* 43. Price Lists of Instruments 144 233*
19. Transits of Interior Planets 51 24* 44. Photographs 158 234
20. Planets and Satellites 99 91* 45. History of the Lick Ob-
21. Fixed Stars 17 21* servatory 62 74
22. New and Variable Stars . . 30 36* 46. Catalogues of Colleges ... 23 92*
23. Double Stars 55 33* 47. Miscellaneous 95 170
24. Nebulae 53 76* 48. Publishers' Book Lists. . . 78 233
25. Obliquity, etc 14 22* — —
In addition to the above, I have counted i6 Smithsonian and
18 miscellaneous pamphlets, bringing the total to 3912. Photo-
graphs, drawings, maps, and charts are included in both counts.
A large number — not far from 1000, probably, — of pam-
phlets has been selected from the drawers marked (*), and bound
into volumes since the count was made in 1892. Many pam-
phlets are also sent, from time to time, to the General Library of
the University at Berkeley. R. G. Aitken.
'p
Fi -V V JR Kl
/if'OR, LENCX AND
T LDEN FOUNDATIONS.
APPARATl'S I-OR MKASrRING PIUrroCRAPHIC PLA rES-(RF:PSOLn).
(Alias (kr Himinelskuiide.)
Astronomical Society of the Pacific. 151
Post Office at Mt. Hamilton.
The post office at Mt. Hamilton was established in 1890, with
Professor S. W. Burnham as postmaster. His successor was
Mr. A. L. COLTON, the present incumbent. The salary of the
postmaster has been a part of the pay of these officers of the
observatory. The salary was, for the fiscal year ending
June 30. 1891, $301-42 June 30, 1894, $330-86
1892, 346.10 1895, 341-01
i893» 285.08 1896, 307-69
E. S. H.
May 31, 1897.
Appointment of Professor Robert G. Aitken as Assist-
ant Astronomer in the Lick Observatory.
At a meeting of the Regents of the University, held May 25,
1897. Professor Robert G. Aitken, B. A. (Williams College,
1887), M. A. (Williams College, 1892), was appointed Assistant
Astronomer in the Lick Observatory. Edward S. Holden.
Graduate Students in Astronomy at the Lick Observa-
tory (1897).
The following-named gentlemen have been admitted as special
students for the summer of 1897: Professor H. D. Curtis (Uni-
versity of the Pacific), B. A. (Michigan, 1892), M. A. (Michigan,
1893); Professor D. A. Lehman TUniversity of the Pacific), B. S.
(State Normal School, Penn., 1889), Ph. B. (Wesleyan, 1893).
Instruments Making in Allegheny.
The following instruments have been made recently by Mr.
J. A. Brashear, of Allegheny, or are at present in process of
construction at his shops: —
Two 16-inch photographic doublets (Petzval system), for
Professor Max Wolf, of the University of Heidelberg.
Eight-inch photographic doublet, with camera, for the Uni-
versity of Tokio. This instrument was shipped in time for use
during the total eclipse of August 9, 1896, but observations were
prevented by cloudy weather.
Siji-inch photographic doublet for Harvard College Observa-
tory. The focal length of the combination is forty-five inches,
152 Publications of the
and the field is fourteen degrees. According to preliminary tests,
this should be a very satisfactory instrument. The star- discs are
nearly round, though slightly enlarged at the extreme edge of
the field.
Eight-inch visual objective, for Park College, Missouri.
Four-and-one-half-inch equatorial, complete, for the U. S.
Military Academy, West Point.
Three 5j4-inch reflectors, equatorially mounted, for Messrs.
J. M. Cook, of Macon, Georgia, J. R. Bettis, of St. Louis,
and J. O. Devor, of Elkhart, Indiana.
Small photographic correcting lens, for spectroscopic work
with the 1 2^ -inch equatorial of the Ohio State University.
Concave grating spectroscope, complete, with many acces-
sories, for Dr. Hauswaldt, of Magdeburg, Germany; for a
6-inch concave grating of twenty-one feet radius.
Star spectroscope, with many accessories, including grating,
photographic objectives, and camera, for the lo^-inch equatorial
of the University of Minnesota (Professor Leavenworth).
Two large star spectroscopes.
Spectrometer, with prisms and grating, for Mr. C. F. Brush,
of Cleveland, Ohio, and various smaller pieces of apparatus.
Death of Alvan G. Clark.
Alvan G. Clark, the last survivor of the famous firm of
Alvan Clark & Sons, died in Cambridgeport on June 9,
1897, at the age of sixty-five years. The best monuments to the
members of this gifted family are the splendid telescopes which
they have set up during the last fifty years all over the world,
from St. Petersburg to California. E. S. H.
Royal Observatory, Greenwich, 1896-97.
At the annual visitation of the Royal Observatory, Green-
wich, the report of the Astronomer Royal, which refers to the
period from May 11, 1896, to May 10, 1897, was submitted. It
stated that the building of the north wing and central dome was
completed in September last. Under this dome is erected the
largest telescope in the world devoted exclusively to photog-
raphy — the 26-inch refractor, the gift of Sir Henry Thompson.
This instrument, completed in April, is already in good working
order. On the same mounting is carried the 12^-inch Merz
Astronomical Society of the Pacific. i53
refractor, as a guiding telescope (in years gone by called the
Great Equatorial), and the Thompson 9-inch photoheliograph;
and in place of a counterpoise at the other end of the declination
axis, a Cassegrain reflecting telescope of 30-inch aperture, with
a new photographic spectroscope attached, and with the 6-inch
Hodgson telescope as guiding telescope. The Thompson equa-
torial thus forms a remarkable and powerful combination of
telescopes, adapted to visual, photographic, and spectroscopic
work, mainly due to private munificence. When the new
altazimuth was ready for use in September, it was found that
there were serious discordances in the readings of the circles
under the different microscopes, depending on the direction
in which the instrument was previously turned. Quite recently
Mr. SiMMS has discovered an entirely unsuspected source of
error. Owing to the method of giving a helical twist to the
grinder while grinding the pivots, it was found that the pivots
had a tendency to act as a screw, a longitudinal force being
set up, the direction of which depended on the direction in
which the telescope was turned, the effect of which was to
slightly move the iron standards carrying the bearings and the
microscopes, and thus to change the position of the microscopes
relatively to the graduated circles. This action of the pivots has
been cured by a few circular turns of the same tool. With the
transit circle the Sun, Moon, planets, and fundamental stars have
been regularly observed as in previous years, and the annual
catalogue contains 3454 stars. The end of the year 1896
finished the period of observation for the new ten-year catalogue
for the epoch 1 890, which will comprise the accurate places of
some 7000 stars, of which a large number are those previously
observed by Groom bridge, so that good data for proper-motions
will be available. For the next ten years the programme of
observations with the transit circle will comprise the observations
of stars (down to the ninth magnitude inclusive) within twenty-
six degrees of the pole, in addition to tfie usual observations of
the Sun, Moon, planets, and fundamental stars.
With the astrographic equatorial half the number of required
chart plates and two thirds of the catalogue plates have been
obtained. Of the fields still required, 197 are within ten degrees
of the pole, and photographs of this part of the sky have been
purposely deferred till near the epoch 1900. At the present rate
of progress, the whole work will occupy about nine years.
154 Publications of the
With the 28-inch refractor 195 double stars have been
measured, each star on the average on two nights, and the
satellite of Neptune on four nights. The excellence of this object
glass is practically demonstrated by the fact that the actual power
of separation by observation of two close stars is greater than the
theoretical value, and, curiously enough, the same holds good in
the case of the large telescope at the Lick Observatory, a fact
which speaks volumes for the instrument-makers. Some photo-
graphs of the Moon and close double stars made in the course of
the year have likewise demonstrated that the reversal of the
crown lens makes this telescope an equally efficient instalment
for purposes of photography. With the Dallmeyer photo-
heliograph the usual Sun photographs have been made, and
gaps in the series at Greenwich filled up by photographs from
India and Mauritius, so that there are records on 360 days.
The spot activity of the Sun has continued to decline since the
date of the last report, but has undergone two remarkable cases
of temporary revival, the first in September, 1896, when the
longest connected group ever photographed at Greenwich was
observed, and the second at the commencement of the present
year.
During the year under review, the average number of chro-
nometers and deck watches being rated at the observatory was
446; the total number received was 1220, the total number issued
1 1 24, and the number sent for repair 519. For the annual trial
of chronometers, which lasted twenty-nine weeks, in tempera-
tures ranging from 42^ to 107^, ninety-seven chronometers were
entered, and fifty-four of these were purchased by the Admiralty
for the navy. The Greenwich time ball was not raised on five
days, owing to the violence of the wind, and that at Deal on ten
days, for the same reason. The meteorological and magnetical
observations have been made as usual. The selection of a site
in Greenwich Park for a new magnetic pavilion has caused a
good deal of trouble, owmg to the difficulty of finding a suitable
position, free from any suspicion of disturbance from iron. Dur-
ing the year there were no days of great magnetic disturbances.
The rainfall for the year ending April 30, 1897, was 26.83 inches,
being 2.29 inches above the fifty years' average. The highest
daily temperature in the shade on the open stand was 91^.1, on
July 14th; the highest recorded temperature under similar con-
ditions in the preceding fifty-five years was 97°. i, on July 15,.
Astronomical Society of the Pacific. 155
1 88 1. — Condensed from a report in the London Times, June 7,
1897.
Expedition from the Lick Observatory to Observe the
Eclipse of January, 1898, in India.
The total solar eclipse of January, 1898, will be observed by
Professor Campbell, of the Lick Observatory, and volunteer
assistants. The expedition was authorized by the Regents of the
University of California at their meeting of June 23d, and its
expenses will be met from a fund generously provided by Colonel
C. F. Crocker, a member of the Regents' Committee on the
Lick Observatory.*
The programme of the expedition will be both spectroscopic
and photographic. The principal subjects of observation will be: —
1. Photographs of the spectrum of the reversing layer.
2. Spectrum photographs, to determine the velocity of rota-
tion of the corona.
3. Observation i repeated with a different instrument.
4. Photographs of the spectrum of the corona.
5. Photographs of the corona on a large scale (40-foot lens),
on the plan first employed by Professor Schaeberle in Chile.
6. Photographs of the corona with a portrait lens, on 8 x 10
plates.
7. Photographic photometry of the corona, as in the Lick
Observatory expeditions of January and December, 1889, April,
1893, (August, 1896).
It is hoped and expected that this expedition will be favored
with good observing weather. Edward S. Holden.
Mt. Hamilton, June 24, 1897.
Astronomical Telegram,
[translation.]
L. O., June 30, 1897; s.^^^ 9-5^ a. m.
To Harvard College Observatory: —
D' Arrest's comet was discovered by C. D. Perrine, June
28.9764 G. M. T.; R. A. 2»^ i" 24".6; N. P. D. 89^46' 29".
[The comet is faint, about 2' in diameter, with a faint conden-
sation, but no nucleus.]
• It will be remembered that the Lick Observatory eclipse expeditions to Cayenne
(December, 1S89) and to Japan (August, 1896) were sent at the expense of Colonel
Crockbr.
156 Publications of the
Photographic Atlas of the Moon.
[extracts from a circular.]
Based chiefly on focal negatives of the Lick Observatory, to the
scale of ten feet to the Moon's diameter; executed by Pro-
fessor Ladislas Weinek, Ph. D., Sc. D., Director of the
Imperial and Royal Observatory of Prague. Published by
Carl Bellmann in Prague [price J[^i for each part (twenty
plates) ; ten parts will complete the first series].
** My long experience in producing drawings and pictures of
lunar landscapes, some with the direct aid of the telescope, others
by enlargement from a number of photographic plates of the
Lick Observatory, has supplied me with the materials for under-
taking the following work, which claims to produce an accurate
and artistic representation of the whole visible surface of the
Moon.
Dissatisfied with the photographic enlargements made by
experts in various quarters, I began, on April 19, 1893, a series
of experiments, with a view to discover a method which, while
rendering the minutest details with absolute exactness and
accuracy, might at the same time ensure a plastically perfect and
beautiful delineation of the object portrayed. That method I
flatter myself to have now found. I intend to publish, in the
immediate future, an account of it.
The materials that form the basis and bulk of the Photographic
Lunar Atlas, begun by me in 1894 and now almost completed,
are mainly derived from the Lick Observatory. The contributions
from that source consist of ninety-four exquisite negatives, includ-
ing the various phases of a whole lunation, taken at the focus of
the telescope of 36-inch aperture of that observatory during the
years 1 890-1 896, and of about i4odiapositives of the same size.
To these must be added four striking lunar negatives made by
Messrs. Loewy and Puiseux at the focus of the large Equatorial
Coud6 (of 60-rw aperture and i8-m focal length) of the Paris
Observatory, and two excellent lunar diapositives of the Arequipa
branch station of the Observatory of Cambridge (Mass.), taken
by Professor Bailey with the telescope of 13-inch aperture, and
enlarged with an ocular placed near the focus. Hence, my
Photographic Lunar Atlas had to be based essentially on the
lunar negatives of the Lick Observatory; whilst the enlargements
Astronomical Society of the Pacific. i57
of Paris and Arequipa plates are added chiefly for the purpose of
facilitating comparative study.
The scale adopted in enlarging the Lick negatives is uniformly
twenty- four times the original, whilst the scale of enlargement of
the Paris negatives and Arequipa diapositives is slightly less. For
the first, the enlargement corresponds, at the mean distance of
the Moon from the Earth, to a lunar diameter of lo feet (= 3, i m^
I mm = I, I km=^ o,"6). For the last, the enlargement gives
a diameter of 4 metres (i mm = 0,89 km = o,"48) i. e. the
double of the diameter of Schmidt' s Map. In enlarging the focal
plates twenty-four times, one brings out to the naked eye, and with-
out any difficulty, the smallest details of the lunar surface, while
its plastic beauty is not altered; and in the second, a simple ratio
with the map of Schmidt is maintained. The following instance
will help to illustrate this remark: On the photographic enlarge-
ment (twenty- four times) from a Lick negative, June 27, 1895, 8*"
21" 1% P. S. T., I discovered, on January 10, 1896, on the top of
the mountain in the northwestern part of the interior of CyrUlus^
a small round object like a crater of i. i km in diameter. I at
once communicated my observation to the French selenographer,
C. M. Gaudibert, and sent him at the same time the print con-
taining it. On the 20th of January, 1896, he was able to
confirm, without any possible doubt, the existence of this crater
on that mountain, with his telescope of 260 mm aperture. The
diameter of that crater is i mm on the print, and it would hardly
be visible to the naked eye were the enlargement made on a
smaller scale.
The work of enlarging from the above focal plates went on up
to Easter, 1897. From April 19 to December i, 1893, 100
photo-lunar enlargements were made; most of these are of the
size of 13X18 cm; and they come from diapositives; they com-
prise e.xperiments of the utmost variety. From December i,
1893, up to Easter, 1897, I made 485 photo-lunar enlargements
from original negatives only (with the exception of seven
enlargements taken from two Arequipa diapositives), and of the
size of 21X26 or of 26X31. From among these the first 196
were made by myself, with an assistant for the development of
the plates, etc.; the last 289 were executed, since November 1894,
by myself alone in all the stages of their execution. The last,
mentioned enlargements, based, too, on more favorable original
negatives, were the first to give complete satisfaction. Funds to
158 Publications of the
defray the very considerable outlay for plates in pursuing this
lengthy and laborious work were provided, partly by a govern-
ment grant and a grant from the Vienna Academy of Science,
partly by the munificence of private donors, especially Baron
Albert von Rothschild in Vienna, and Miss Catherine W.
Bruce in New York.
And now that the principal part of this preparatory work is
done, the plan is to publish at Prague a Lunar Photographic
Atlas on a scale of ten feet, relatively four metres, to the diameter
of the Moon, having 200 maps of the size of 26X31 cm, contain-
ing the principal lunar formations viewed under the most varied
conditions of illumination. If this atlas is favorably received, I
propose to publish, later on, a second series of 200 maps, to com-
plete the first. The 200 maps first mentioned come from enlarge-
ments made since November, 1894, and show the best of what
has been done up to the present time. The order in which the
pictures will be arranged must not be supposed to follow the
phases of the waxing or waning Moon; it will rather be deter-
mined by the degree of excellence or of beauty exhibited in the
enlargements available for publication. Shown at the top of each
sheet will be the selenographical latitude and longitude for the
centre of the picture, and also the selenographical longitude of
the terminator for the latitude 0°. By this means it will be easy
for every one to arrange the sheets according to the relative
positions of the lunar objects they portray, or according to the
terminator of the corresponding lunar phase. To secure the
utmost precision in the minutest details, the reproductions of
enlargements done at Prague will be executed by the phototype
process in a manner as closely approaching perfection as possible.
They will be printed direct from my enlarged glass diapositives,
under my constant personal supervision and control, by the well-
known Art-Photographical Institute of Carl Bellmann, Prague.
The enclosed print, showing the Maginus Walled Plain* (L. O.
1895, Oct. 9, 16^ 20"" 2' — 2,' 5, P. S. T.), is an example of the way
in which each map will be printed on card board of the size of
33 X 43 cm, so that they may be easily handled at the telescope or
framed for scientific collections. Each map will be detached, and
one fascicle, containing twenty maps, will appear every two—
• The circular is accompanied by a reproduction of Professor Wbinrk's enlargement
of Maginus^ which is admirable in every respect. Copies of the circular and this plate
will be sent by Carl Bbllman, as above, to those who apply to him. E. S. H.
Astronomical Society of the Pacific. 159
three months. This will obviate the difficulty that observatories,
academies, scientific societies, and institutions might else find in
purchasing the entire work in one issue.
The publication of the atlas in the dimensions proposed (ten
issues, making a total of 200 lunar landscapes) cannot be under-
taken until the requisite pecuniary support is forthcoming in the
shape of promises of numerous subscribers to the work. I
venture to appeal in the first instance to the various observatories
at home and abroad, and to solicit their promises to become
subscribers for the ten issues, each to contain twenty lunar land-
scapes.
Pursuing, as I do, different ends from those of the Paris Lunar
Atlas (its diameter of nearly 2^ metres makes it a little larger
than Schmidt's map) which aims at securing great beauty of
relief and plastic effect, as well as from those of the Mt Hamilton
Atlas (its diameter is equal to that of Madler's map, i.e. one
metre), which endeavors to preserve the faint contrasts of light
and shade in their true value, my enlargements published in
the Prague Lunar Atlas should have ample justification for publi-
cation, in that they will together afford a faithful and accurate
reproduction of the striking results obtained in the field of
photo-selenography at the end of* the nineteenth century."
Professor Dr. L. Weinek, Director of the Imperial
and Royal Observatory of Prague.
Prague, April 18, 1897.
Trial of the Crosslex Reflector.
At the beginning of April, 1897, Professor Hussey was placed
in full charge of the Crossley reflector, to give it a thorough
trial, visually at the Newtonian focus, and photographically at both
the Newtonian and principal foci, thus continuing the work begun
by him in June, 1896.* A new driving clock for the instrument
has been made by the instrument- maker of the Lick Observatory
during the past winter, from drawings by Professor Hussey. It
b on the same general plan as the driving-clock of the 36-
inch equatorial, and promises well. The weights on the double
conical pendulum are about twenty-eight pounds each. Mirror
A is now in the instrument. During the winter and spring the
Bruce spectrograph has been constructed (at Mount Hamilton)
*S€e Pmblications A. S. P., Volume VIII, page 236.
i6o Publications of the
for the reflector, from designs by Professor Campbell, who pro-
poses to employ it in the principal focus.
Edward S. Holden.
Death of Hon. Charles Frederick Crocker.
After a short illness, Hon. C. F. Crocker, Regent of tlie
University of California, and a member of the Committee of
the Regents on the Lick Observatory, died at his country place.
Uplands, San Mateo County, on Saturday, July 17, 1897, ^t the
age of forty-three years. His loss will be felt in very many rela-
tions of business and friendship, and in none more than in those
he sustained to the University of California and to the Lick
Observatory. Edward S. Holden.
July 18, 1897.
Small Telescope For Sale.
Mr. C. A. ScRASE (care of Messrs. Percy & Dearsley,
328 Montgomery Street. San Francisco), has in his hands for
sale for $130 a telescope of 3^-inches aperture by E. G. Wood,
of London, complete in its box. Intending purchasers should
address themselves to him. . E. S. H.
July 19, 1897.
Appointments in the Lick Observatory.
At a meeting of the Regents, July 13, 1897, Mr. William
H. Wright was appointed to be Assistant Astronomer and Mr.
E. F. Coddington to be Fellow in Astronomy. E. S. H.
Meeting of the Board of Directors and of the
Society, June 12, 1897.
Saturday, June 12th, was the date for a regular meeting: of the
Directors and of the Society at Mt. Hamilton. As no quorum for the
transaction of business (in either body) was present, no meetings were
held. The papers presented for reading will be printed in the Pubiica-
tions in due course.
Astronomical Society of the Pacific. i6i
OFFICERS OF THE SOCIETY.
Mr. William Alvord PnsitUnt
Mr. Edward S. Holdbn Firtt Vice-Prtsident
Ut. Frbdcrick H. Srares Second Vict-PresitUnt
Mr. Chauncbv M. St. John Third Vict-President
JI;:R-?:i;".r"'M ^"reuru.
Mr. F. R. ZiEL Treasurer
B^rd of Directors^ Messrs. Alvord, Holden, Molbra, Morse, Miss O'Halloran,
Messrs. Pbrrinb, Pibrson, Sbarbs, St. John, von Gbldkrn, Zibl.
Finance Commi/tee— Messrs, William M. Pibrson, E. J. Molbra, and C. M. St. John.
Committee on Publication — Messrs. Holdbn, Babcock, Aitkbn.
Library Committee— yitxsx%, Hussby and Sbarbs and Miss O'Halloran.
Committee on the Comet- Medal— }Aes&x%, Holdbn (ex-ojfficio), Schabbbrlb, Campbell.
OFFICERS OF THE CHICAGO SECTION.
Executive Committee— Hx. Ruthven W. Pike.
OFFICERS OF THE MEXICAN SECTION.
Executive Committee— Mts&rs, Camilo Gonzalez, Francisco Rodriguez Rev.
NOTICE.
The attention of new members is called to Article VIII of the By-Laws, which provides that
the annual subscription, paid on election, covers the calendar year onlv. Subsequent annual
payments are due on January ist of each succeeding calendar year. This rule is necessary in
order to make our book-keeping as simple as possible. Dues sent by mail should be directed to
Astronomical Society of the Pacific Sig Market Street,* San Francisco.
It is intended that each member of the Society shall receive a copy of each one of the Pub-
lications for the year in which he was elected to membership and for all subsequent years. If
there have been (unfortunately) any omissions in this matter, it is requested that the Secreuries
he at once notified, in order that the missing numbers may be supplied. Members are requested
to preserve the copies of the Publications of the Society as sent to them. Once each year a title-
page and contents of the preceding numbers will also be sent to the members, who can then bind
the numbers together into a volume. Complete volumes for past years will also be supplied, to
members only, so far as the stock in hand is sufficient, on the payment of two dollars to either of
the Secretaries. Any non-resident member within the United States can obtain books from the
Society's library by sending his library card with ten cents in stamps to the Secretary A. S. P.i
3 19 Market Street, San Francisco, who will return the book and the card.
The Committee on Publication desires to say that the order in which papers are printed in
the Pn^icationx is decided simply by convenience. In a general way, those papers are printed
tirst which are earliest accepted for publication. It is not possible to send proof sheets of papers
to be printed to authors whose residence is not within the United States. The responsibility for
tne views expressed in the papers printed rests with the writers, and is not assumed by the
Society itself.
The titles of papers for reading should be communicated to either of the Secretaries as early
ai possible, as well as any changes in addresses. The Secretary in San Franci:»co will send to
any member of the Society suitable stationery, stamped with the deal of the Society, at cost price,
a% follows: a block of letter paper, 40 cents; of note paper, 25 cents; a package of envelopes, 25
cents. These prices include postage, and should be remitted by money-order or in U. S. postage
stamps. The sendings are at the risk of the member.
Those members who propose to attend the meetings at Mount Hamilton during the summer
should communicate with "The Secretary Astronomical Society of the Pacific " at the rooms of
the Soctetjr, 810 Market Street, San Francisco, in order that arrangements may be made for
(raosportation, lodging, etc
PUBLICATIONS ISSUED BIMONTHLY.
(February^ Aprils June^ August^ October^ December.)
PUBLIC LlBRARYl
PUBLICATIONS
OF THE
Astronomical Society of the Pacific.
Vol. IX. San Francisco, Septbmbbr i, 1897. . No. 57.
BY-LAWS
OF THB
ASTRONOMICAL SOCIETY OF THE PACIFIC.
ARTICLE I,
This Society shall be styled the Astronomical Society of
THE Pacific. Its object shall be to advance the Science of
Astronomy, and to diffuse information concerning it.
ARTICLE II.
This Society shall consist of active and life members, to be
elected by the Board of Directors.
1. Active members shall consist of persons who shall have
been elected to membership and shall have paid their dues as
hereinafter provided.
2. Life members shall consist of persons who shall have been
elected to life membership and shall have paid $50 (fifty dollars)
to the Treasurer of the Society.
3. A certain number of Observatories, Academies of Science,
Astronomical Societies, Institutions of Learning, etc., not to
exceed one hundred, shall be designated by the Board of
Directors as Corresponding Institutions, and they shall receive
the publications of this Society in exchange or otherwise.
ARTICLE in.
At each annual election there shall be elected a Board of
eleven Directors, and a Committee on Publication, consisting of
three members. The officers of this Society shall be a President,
three Vice-Presidents, two Secretaries and a Treasurer. The
1 64 Publications of the
Directors shall organize immediately after their election, and
elect from their number the officers of the Society. They may
also appoint a Librarian, and such other assistants as may be
required. The Directors shall fill by appointment any vacancies
which may occur after the annual election.
The Library of the Society shall be kept in San Francisco,
and shall be open to the use of all the members.
ARTICLE IV.
The President, or, in his absence, one of the three Vice-
Presidents, or, in the absence of both the President and the
Vice-Presidents, any member whom the Society may appoint,
shall preside at the meetings of the Society. It shall be the duty
of the President to preserve order, to regulate the proceedings
of the meetings, and to have a general supervision of the affairs
of the Society. The President is, ex-officio, a member of all
Committees of the Board of Directors.
ARTICLE V.
The Secretaries shall keep, and have the custody of, the
records; they shall have the custody of all other property of the
Society, excepting the money thereof; they shall give timely notice
of the time and place of meetings; they shall keep in books a
heat and accurate record of all orders and proceedings of the
Society, and properly index them; they shall conduct the cor-
respondence of the Society; they shall preserve and index the
originals of all communications addressed to the Society; and
keep a copy of all their letters, properly indexed; and they shall
prepare for publication an accurate summary of the transactions of
the Society at each of its meetings.
ARTICLE VI.
The Treasurer shall receive and deposit in such bank as may
be designated by the Directors, to the credit of the Society, all
donations and bequests of money and all other sums belonging
to the Society. He shall keep an account of all money received
and paid by him, and at the annual meetings shall render a partic-
ular statement of the same to the Society. Money shall be
paid by him only on the written order of the Finance Committee
of the Board of Directors. He shall give such bonds as may be
required by the Board of Directors.
Astronomical Society of the Pacific. 165
ARTICLE VII.
Candidates for active or life membership may be proposed by
any member of the Society to either of the Secretaries, in writing.
A list of such candidates shall be certified to the Board of Direc-
tors by the Secretaries at each of their meetings, in writing. A
majority (not less than three) of the Directors present at any
such meeting shall be required for election.
ARTICLE VIII.
Each active member shall pay an annual subscription of ^\^
dollars, due on the first of January of each year, in advance.
Each active member shall, on his election, pay into the Treasury
of this Society the sumr of ^\^ dollars, which shall be in lieu of
the annual subscription to the first of January following his
election, and in lieu of an initiation fee. No one shall be deemed
an active member, or receive a diploma, until he has signed the
register of members, or accepted his election to membership in
writing, and paid his dues for the current year. Any member
may be released from annual dues by the payment of fifty dollars
at one time, and placed on the roll of life members by the vote
of the Board of Directors. Any failure on the part of a mem-
ber to pay his dues within six months after the time the same
shall have become payable, shall be considered equivalent to a
resignation.
ARTICLE IX.
The annual meeting of this Society shall be held on the last
Saturday in March, at eight o'clock p. m., at the rooms of the
Society in San Francisco; and meetings shall be held for the
ordinary transactions and purposes of the Society, as follows: —
Meetings shall be held in the Library of the Lick Observatory,
Mount Hamilton, at a suitable hour on the second Saturday of
June and the first Saturday of September; and meetings shall be
held in the rooms of the Society, in San Francisco, at eight
o'clock p. M., on the last Saturdays of January, March, and
November.
A special meeting may be called by the President, or, in his
absence or disability, by one of the Vice-Presidents, or, in the
absence or disability of both the President and the Vice-Presi-
dents, by the Secretary, on the written requisition of ten active
or life members; and the object of such meeting shall be stated
in the notice by which it is called.
1 66 Publications of the
The annual election shall be held on the day of the annual
meeting, between the hours of 8:15 and 9 P. m.
No member shall be permitted to vote at any meeting of the
Society who has not paid all his dues for past and current years.
There shall be no voting by proxy.
ARTICLE X.
Fifteen active or life members shall be a quorum for the trans-
action of business.
ARTICLE XI.
No papers or manuscripts shall be published by the Society
without the consent of the Directors. Any motion to print an
address, or other paper read before the Society, or any other
matter belonging to the Society, shall be referred to the Com-
mittee on Publication, who shall report to the Directors. The
Committee on Publication may make suggestions to the Directors,
from time to time, with reference to the publication of such
papers as in their judgment should be published by the Society;
and this Committee shall have the care, direction and supervision
of the publication of all papers which the Directors may authorize
to have published.
Members of the Society shall receive all the publications of
the Society free of charge.
ARTICLE XII.
This Society may, by a vote of a majority of all its active and
life members, become a branch of an American Astronomical
Society, should one be formed.
ARTICLE XIII.
It shall be the duty of the Directors, in case any circumstances
shall arbe likely to endanger the harmony, welfare or good order
of the Society, to call a special meeting of the Society; and if, at
such meeting, after an examination of the charges, and hearing
the accused, who shall have personal notice of such proceedings,
it shall be proposed that the offending member or members shall
be expelled, a vote by ballot shall be taken, and if two thirds of
the members present vote in favor thereof, the offending member
or members shall be expelled.
Astronomical Society of the Pacific. 167
ARTICLE XIV.
The Directors shall meet half an hour before the stated time
of each bi-monthly meeting, and at such other times as they may
appoint. The President, or, in his absence, any one of the Vice-
Presidents, may call special meetings of the Board of Directors
at any time. Notice of the time and place of such meeting shall
be given by the Secretaries, by depositing in the post-office at
San Francisco a notice of the time and place, addressed to each
Director personally, at his last known place of residence, with the
postage thereon prepaid, six days before the time of meeting.
ARTICLE XV.
The By-Laws may be amended at any time by a consenting
vote of nine members of the Board of Directors at any duly
called meeting thereof.
ARTICLE XVI.
In order to increase the usefulness of the Society, any groups
of its members residing in the same neighborhood (except in the
City and County of San Francisco, State of California,) are
authorized to form local organizations which shall be known as
**The Section of the Astronomical Society of the Pacific.*'
No Section shall be formed except by the consent of the
Board of Directors of the parent Society.
The proceedings of such Sections may be printed in the
Publications of the Astronomical Society of the Pacific, either in
full or in abstract, and the parent Society shall not be in any way
responsible for publications made elsewhere.
No person not a member of this Society in good standing shall
be eligible to membership in a Section, nor shall membership in a
Section interfere in any way with the status of the person as a
member of this Society.
The special expenses of each Section shall be borne by the
group of members composing it, and this Society shall not be
liable for any debts incurred by any Section.
Publications of the
R THE BESTOWAL OF THE BRUCE
OF THE ASTRONOMICAL SOCIETY
OF THE PACIFIC.
I. A medal is founded by Miss Catherine Wolfe Bruce,
of New York, to be given, not oftener than once a year, for dis-
tinguished services to astronomy. The medal is international in
character, and it may be awarded to a citizen of any countrj',
and to a person of either sex.
II. The cost of the medal is to be met from the interest of
the Bruce Medal Fund of $2500. The capital of this fund is
not to be impaired. Une;cpended interest is to be added to the
capital to become an integral part thereof
III. The medal is to be of gold. The obverse is to bear the
Seal of the Astronomical Society of the Pacific. The reverse is to
bear an inscription as follows: This medal, founded A. D.
MDCCCXCVII, BY Catherine Wolfe Bruce, is presented
TO FOR distinguished
services to Astronomy (date in years).
IV. The Bruce Medal is not to be given twice to the same
individual.
V. On the first of September of every year one of the Secre-
taries of the Astronomical Society of the Pacific is to address an
official letter to the Director of each of the following Observa-
tories, namely: —
The Harvard College Observatory, The Observatory of Paris,
The Lick Observatory, The Observatory of Greenwich,
The Yerkes Observatory, The Observatory of Berlin,
enclosing the statutes relating to the Bruce Medal, and requesting
each of the six Directors just named to nominate not to exceed
three Astronomers worthy to receive the medal for the ensuing
year.
The replies of the said Directors are not to be communicated
by the Secretary to any person until the first of November, when
a list containing the names of the Astronomers so nominated is
to be certified, in writing, by the Secretary, to each of the eleven
Directors of the Astronomical Society of the Pacific; and a
special meeting of the Directors called for the last Saturday in
November, at 2 p. m. At that meeting these Statutes are to be
read ; and the original letters from the Directors of the Observa-
Astronomical Society of the Pacific, 169
tories are to be submitted by the Secretary, and afterwards sealed
in an envelope and deposited in the archives of the Society, not
thereafter to be opened except by a formal resolution of the
Directors, passed at a regular meeting. All such letters and
nominations are to be regarded as confidential by all who are
knowing to them.
VI. The Directors of the Astronomical Society of the
Pacific, at the special meeting aforesaid, may vote in person or
by written proxy.
The medal is not to be awarded unless the votes of at least six
Directors are cast at this meeting. It may be awarded to any
individual named in the list certified by the Secretary by the con-
senting votes of six Directors; or, the consenting votes of six
Directors may order that no award shall be made for the ensuing
year.
The award of the medal, if made, is to be for the calendar
year commencing with the January after the meeting at which the
award is made; and on January ist one of the Secretaries of the
Astronomical Society of the Pacific is to officially notify the
recipient of the award, and on receiving a letter of acceptance, is
to transmit the medal, engraved with name and year. The name
of the recipient of the medal is not to be made public until after
the receipt of a letter of acceptance.
The President of the Astronomical Society of the Pacific, in
hb address at the annual meeting of the Society in March is to
announce the award and the reasons for making it.
VII. It is competent for the eleven Directors of the Astrono-
mical Society of the Pacific, by a unanimous vote, and not other-
wise, to substitute for any one of the Observatories named in
Article V some other Observatory. It is desirable, though not
essential, that three of the Observatories aforesaid shall be
American and three Foreign.
Not more than one such substitution is to be made in any
single calendar year.
I70 Publications of the
RULES RELATING TO THE COMET MEDAL OF THE
ASTRONOMICAL SOCIETY OF THE PACIFIC.
I. A medal of bronze is established, as a perpetual founda-
tion, to be given for the discovery of comets, as follows: —
The medal is to bear on the obverse side the effigy of a brig^ht
comet among stars, with the legend, ** Astronomical Society
OF THE Pacific," around the border; and on the reverse the
inscription; "This Medal founded in 1890 by Joseph A.
DoNOHOE, IS presented TO (the nkme
of the discoverer) to commemorate the Discovery of a
Comet on (the date).**
It is to be understood that this medal is intended solely as a
recognition of merit, and not as a reward.
II. The medal will be given to the actual discoverer of any
unexpected comet.
III. The discoverer is to make his discovery known in the
usual way, and, in order to simplify the work of the committee,
which, in certain cases may be called upon to consider the merits
of several independent discoveries of the same object, he should
also address a letter to the Director of the Lick Obser\'atory,
which should state the exact time of the discovery, the position
of the comet, the direction of its motion (when this can be deter-
mined), and the physical appearance of the object.
No application for the bestowal of the medal is required. The
letters received from discoverers of comets will be preserved in
the records of the Lick Observatory. Cable telegrams to the
Lick Observatory aie to be addressed to '* Astronomer, San
Francisco. * *
IV. All communications will be referred to a committee con-
sisting of the Director of the Lick Observatory, ex officio^ and
of two other persons, members of the Astronomical Society of
the Pacific, who are to be annually appointed by the Board of
Directors. The decisions of this committee are to be final upon
all points relating to the award of the medal. The committee will
print an annual statement of its operations in the publications of
the Society.
Under ordinary circumstances the comet medal will be
awarded within two months after the date of the discovery. In
cases of doubt a longer period may elapse. The medal will not
Astronomical Society of the Pacific, 171
be awarded (unless under the most exceptional circumstances) for
the discovery of a comet until enough observations are secured
(by the discoverer or by others) to permit the calculation and
verification of its orbit.
V. This medal is to be a perpetual foundation from and after
January i. 1890.
OFFICERS OF THE SOCIETY.
Mr. William Alvord President
Mr. £dwaiid S. Holdkh First y ice- President
Mr. Frbdbrick H. Sbares .... Second Vict" President
Mr. Chaunxby M. St. John Third Vice-President
s;:^.-?.-i;:r'"! ■ ^««/--w
Mr. F. R. ZiKL .... Treasurer
B^esr-d 0/ Directors— hlessn. Alvoru, Holdsn, Molbra, Morse, Miss O'Halloran,
Messrs. Pbrrine, Pibrson, Sbarbs. St. John, von Gbldern, Ziel.
FifuxMue Committee—Messrs. William M. Pibrson, E. J. Molbra, and C. M. St. John.
Commtittee on Pn^/ication—tAtssrs. Holdbn. Babcock, Aitken.
I.thrtuy Committee— lUtssn, Hussby and Sbares and Miss O'Halloran.
Comfftittee on the Comet- Medai—Mtssn. Holden (ex-officio)^ Schakbbrlk, Campbbix.
OFFICERS OF THE CHICAGO SECTION.
Ejc€cutive Committee— Mr. Ruthven W. Pikb.
OFFICERS OF THE MEXICAN SECTION.
Exfrntivf Committee—fAtssrs, Camilo Gonzalez, Francisco Rodriguez Rev.
JUPITER, UPiXiCn 22, 185?.
(Taken at the Lick Observatory with an 18-inch Reflecting Telescope^
Exposure Times
8>» 22" 0" to 40'
10 11 o to 40
10 16 o to 4Q
P. S. T.
PUBLICATIONS
Astronomical Society of the Pacific.
Vol. IX. San Francisco, October i, 1897. No. 58.
PHOTOGRAPHS OF /[/P/T£Ji.frBE~N^^y .
[Taken with an i8-inch Reflecting Telescope.] /pTTDr rr^ , ' O h i\
j^uiJUC LIBRAIV,
By J. M. SCHAEBERLE.
The three silver prints of Jupiter given in the present
are contact copies of negatives taken with the 18-inch reflecting
telescope described in Volume VII of these Publications, The
particular secondary for focal images of this scale can only be
used advantageously when there is no wind and when the seeing
is first-class. The equivalent focal length, corresponding to the
linear dimension of the image, is about 650 feet.
Held at a distance of ten inches from the eye, the effect, so
ias as simple magnification is concerned, is the same as a view of
Jupiter through a telescope magnifying 780 diameters. With
such a power, the visual observations of planetary details are
ordinarily unsatisfactory; in view, therefore, of the improvement
(mentioned farther on) in the definition of the 18-inch mirror,
which will surely result from the increase in the principal focal
length, these photographs are of peculiar interest.
I recently discovered a most serious optical defect which is
common to all parabolic mirrors.* The magnitude of this defect
increases rapidly as the angular aperture of the mirror increases.
In order to obtain results which are not seriously affected by this
error, the ratio of focal length to aperture should never be less
than, say, fourteen to one. I have decided to regrind and refigure
the 18-inch reflector, and make the ratio of focal length to
aperture about twice as great as it is at present.
•See Astronomical Joumalt No. 413.
174 Publications of the
The silver prints were made by Mr. William Pauli of the
Lick Observatory. Much of the detail in the original neg^ative
k, of course, lost in the paper prints. By comparing the three
photographs, allowing for the rotation of the planet, no mistake
can be made as to whether a given marking actually corresponds
to a surface feature of the planet, or whether it is due simply to
a defect in the plate. J. M. Schaeberle.
Lick Observatory, University of California,
September 20, 1897.
PLANETARY PHENOMENA FOR SEPTEMBER,
OCTOBER, NOVEMBER AND DECEMBER. 1897.
Bv Professor Malcolm McNeill.
September.
The Sun crosses the equator and autumn begins at about
II A.M., P. S. T., on September 22d.
Mercury is an evening star at the beginning of the month,
having passed greatest east elongation on August 26th, but it is
too near the Sun for naked-eye observations, and passes inferior
conjunction on the morning of September 2 2d. It then becomes
a morning star and moves rapidly away from the Sun, so that by
the end of the month it rises more than an hour before sunrise,
and can be easily seen under good-weather conditions. It is in
conjunction with Jupiter on September 27th, but the conjunction
is not so close, nor are the planets as well situated as they will be
at the conjunction which will take place in October.
Venus is a morning star, rising about three hours before sun-
rise. During the month it moves thirty-six degrees east and nine
degrees south through the constellations Cancer and Leo* On
the night of September 24-25th it is very near the first magni-
tude star Regulus (a Leonis)^ passing the star on the north at a
distance of about half of the Moon*s diameter.
Mars is still an evening star, but it is rapidly nearing conjunc-
tion with the Sun, and it can scarcely be seen without telescopic
aid, except perhaps during the first few days of the month, when
it sets about two hours after sunset. It is also nearly at its
greatest distance from the Earth, and least brilliancy. It moves
Astronomical Society of the Pacific. i75
about eighteen degrees east and eight degrees south through the
constellations Leo and Virgo,
JupiUr comes to conjunction with the Sun on the night of
September i2-i3th, and becomes a morning star; but does not
get far enough away to become visible to the naked eye until
nearly the end of the month.
Saturn is still in sight as an evening star, but is nearing the
Sun. By the end of the month it sets before 8 p.m. It moves
about two degrees eastward during the month along the borders
of the constellations Libra and Scorpio. The rings are nearly at
their maximum opening.
Uranus is near Saturn, about two degrees south at the begin-
ning of the month, and is also moving eastward, but only about
half as fast as Saturn. It is so near the horizon after sunset that
the conditions for visibility are not good.
Neptune is in the constellation Taurus, rising quite late in the
evening and is too faint to be seen with the naked eye.
October.
Mercury b a morning star throughout the month, and during
nearly the whole time is in good position for observation in the
twilight just before sunrise. It comes to its greatest west elonga-
tion on the evening of October 7th, and at that time rises
more than an hour and twenty minutes before sunrise. On the
morning of October 6th it is very close to Jupiter, conjunction
occurring at midnight, P. S. T. At the time of nearest approach,
the planets are only twelve minutes of arc apart, a distance much
less than the semi-diameter of the Moon, and they will show as a
fine double star to the naked eye,
Venus is also a morning star, a little nearer the Sun than it
was during September. It moves thirty-four degrees east and
sixteen degrees south through the constellations Leo and Virgo,
On the afternoon of October 19th it is in conjunction with Jitpiter,
the nearest approach being a little less than the Moon's diameter,
Venus being twenty-eight minutes north.
Mars b still an evening star, but closer to the Sun than it was
in September. It is now only about as bright as the pole star
and cannot readily be seen after sunset. During the latter half
of the month it reaches its greatest distance from the Earth,
about 236,000,000 miles, a distance a little greater than the
average maximum distance, and not quite seven times as great
as the least possible fJistance at opposition.
176 Publications of the
Jupiter IS a morning star, rising about two hours earlier than
during the corresponding period in September. It moves about
four degrees east and south in the western part of the constella-
tion Virgo, Its conjunctions with Mercury and Venus have
already been noted.
Saturn is an evening star, nearer the Sun than it was in
September, and by the end of the month it will not be an easy
object for the naked eye after sunset. It is moving eastward, near
the boundary of Libra and Scorpio,
Uranus is still near Saturn, and is also moving eastward, but
at a much smaller rate. At the end of the month it is about
three degrees west and one degree south of Saturn,
Neptune is in about the same position in the eastern part of
Taurus, as in September.
Occultation of the Pleiades, The Moon will again pass over
the Pleiades group on the evening of October 13th. As the
Moon is then three days after full, the immersions will occur at
the bright limb and the emersions at the dark. The eastern part
of the United States is better situated than the western for seeing
this group of occultations, as the Moon will have passed over a
considerable part of the group when it rises in the Pacific States.
November.
Mercury is a morning star quite near the Sun until November
7th, when it comes to superior conjunction with the Sun, and is
an evening star for the rest of the month, but does not get far
enough away to be easily visible. It is in conjunction with Mars
on November 12th, with Uranus on November i6th, and with
Saturn on November i8th, but the planets are all too near the
Sun for naked-eye observations.
Venus is still a morning star, but it is gradually drawing
nearer the Sun, and at the end of the month rises only about an
hour and a half earlier. During the month it moves thirty-six
degrees eastward and thirteen degrees southward through the
constellations Virgo and Libra, passing four degrees north of
Spica (a Virginis) on the morning of November 7th, and about
one degree north of a Librte on the morning of November 25th.
Mars is too near the Sun for observation throughout the
month. It comes to conjunction on the morning of November 21st,
and changes from an evening to a morning star, moving about
twenty-two degrees eastward and southward during the month.
Astronomical Society of the Pacific, i77
It is in conjunction with Merctiry^ on November 12th, with
Uranus on November 21st, and with Saturn on November 27th.
It reached its greatest distance from the Earth toward the end of
October, about a month before the time of conjunction.
Jupiter is a morning star, gradually increasing its distance
from the Sun and rising earlier. During the month it moves
about ^\e degrees eastward and southward in the western part
of the constellation Virgo. On the morning of November 15th
it passes the fourth magnitude star 7; VirginiSy the planet being
about half of the Moon*s apparent diameter south of the star.
Saturn is quite close to the Sun coming to conjunction, and
changing from an evening to a morning star on the night of
November 24-25th. It moves about four degrees eastward in
the constellation Libra. It is in conjunction with Mercury on
November i8th, and with Mars on November 27th.
Uranus is near Saturn^ three degrees to five degrees west,
and comes to conjunction with the Sun on the morning of
November 21st It comes to conjunction with Mars on^ hour
later, and Mars^ conjunction with the Sun occurs only three
hours later than his conjunction with Uranus.
Neptune is retrograding (moving westward) in the constella-
tion Taurus.
December.
The Sun enters the sign Capricorn (not the constellation), and
winter begins December 21st, 5 a.m., P. S. T.
Mercury is an evening star, and after the first few days of the
month sets more than an hour after sunset, so that it can be seen
under good weather conditions during the greater part of the
month. It reaches greatest eastern elongation on December
20th, and then sets about an hour and half after sunset.
Venus is still a morning star, but is drawing nearer to the Sun,
and by the end of the month it rises less than an hour before
sunrise. It moves about forty degrees eastward and seven
degrees southward during the month through the constellations
Libra and Scorpio. At the end of the month it is very close to
Mars, the planets coming to conjunction on the evening of
December 30th.
Mars is a morning star, and by the end of the month rises
almost an hour before sunrise, but it is still too faint to be easily
seen, on account of its great distance from the Earth. Its
brightness will keep on increasing throughout the whole of 1898.
178 Publications of the
Jupiter is also a morning star. Its distance from the Sun is
increasing, and by the end of the month it rises at about mid-
night. It moves about three degrees eastward in the western
part of the constellation Virgo.
Saturn is also a morning star, and during the month it gets
far enough away from the Sun to be seen in the morning twilight.
It is in the western part of the constellation Scorpio, and moves
about three degrees eastward during the month.
Uranus is also a morning star about ^\^ degrees west of
Saturn, in the constellation Scorpio.
Neptune is in opposition on the evening of December 12th.
Explanation of the Tables.
The phases of the Moon are given in Pacific Standard time.
In the tables for Sun and planets, the second and third columns
give the Right Ascension and Declination for Greenwich noon.
The fifth column gives the local mean time for transit over the
Greenwich meridian. To find the local mean time of transit for
any other meridian, the time given in the table must be corrected
by adding or subtracting the change per day, multiplied by
the fraction whose numerator is the longitude from Greenwich
in hours, and whose denominator is 24. This correction is
seldom much more than i". To find the standard time for the
phenomenon, correct the local mean time by adding the differ-
ence between standard and local time if the place is west of the
standard meridian, and subtracting if east. The same rules apply
to the fourth and sixth columns, which give the local mean times
of rising and setting for the meridian of Greenwich. They are
roughly computed for Lat. 40°, with the noon Declination and
time of meridian transit, and are intended as only a rough guide.
They may be in error by a minute or two for the given latitude,
and for latitudes differing much from 40® they may be several
minutes out.
Phases of the Moon, P. S. T.
H. M.
First Quarter, Sept. 3, 3 13 p. m.
Full Moon, Sept. 10, 612 p. m.
Last Quarter, Sept. 18, 6 51 P. M.
New Moon, Sept. 26, 5 46 a. m.
Astronomical Society of the Pacific. i79
The Sun.
1897.
R. A.
Declination.
Rises.
Transits.
S«ts.
H. M.
'
H. M.
H. M.
H. M.
Sept. I.
10 43
+
8
6
5 33 A.M.
NOON.
6 27 P.M.
II.
II 19
+
4
22
5 43
II 57 A.M.
6 II
21.
II 55
+
30
5 52
II 53
5 54
Oct. I.
12 31
—
3
24
6 I
II 50
5 39
Mercury.
Sept I.
12 16
—
5
5
7 49 A.M.
I 32 P.M.
7 15 P.M.
II.
12 24
—
7
I
7 24
I
6 36
21.
II 5^
—
3
8
6 5
II 55 A.M.
5 45
Oct. I.
II 37
+
2
37
4 46
Venus.
10 55
5 4
Sept I.
8 9
+
19
29
2 21 A.M.
9 25 A.M.
4 39PM.
II.
8 58
+
17
It
2 34
19 34
4 34
21.
9 45
+
14
4
2 55
9 43
4 31
Oct I.
10 32
+
10
16
3 15
Mars.
9 50
4 25
Sept I.
12 17
—
I
12
7 37 A.M.
I 33PM.
7 29 P.M.
II.
12 41
—
3
52
7 31
I 18
7 5
21.
13 5
—
6
30
7 24
I 2
6 40
Oct I.
13 30
—
9
6
7 19
12 48
6 17
Jupiter.
Sept I.
II 18
+
538
6 15 A. M.
12 34 P.M.
6 53 P.M.
II.
II 26
+
4
48
5 47
12 3
6 19
21.
II 34
+
3
57
5 19
II 32 A.M.
5 45
Oct I.
II 42
+
3
7
4 50
II
5 10
Sa turn.
Sept I.
15 33
—
17
II
II 49 A. M.
4 49 P.M.
9 49 P.M.
II.
15 35
—
17
22
II 13
4 12
9 II
21.
15 38
—
17
34
10 36
3 35
8 34
Oct I.
15 42
—
17
48
10 2
3
7 58
Uranus.
Sept I.
15 32
—
18
55
11 55 A.M.
4 48 P.M.
9 41 P.M.
II.
15 33
—
18
59
II 16
4 9
9 2
21.
15 35
—
19
5
10 39
3 32
8 25
Oct I.
15 37
—
19
II
10 I
2 54
7 47
Neptune.
Sept I.
5 27
+
21
S2,
II 22 P.M.
6 41 A.M.
2 P.M.
II.
5 28
+
21
53
10 42
6 I
I 20
Oct
21. 5 28
I. 5 28
4- 21 53 10 4
+ 21 52 9 24
5 23 12 42
4 43 12 2
i8o Publications of the
Minima of Algol, P.
S. T.
H. M
H.
M.
Sept 2.
12 41 A.
M. Sept. 15
I.
5
35 A. M.
4-
9 30 P.
M. 22
.
2
24 A. M.
7.
6 19 P.
M. 24
..
II
12 P. M.
10.
3 8 P.
M. 27
.
8
I P. M.
13-
II 57
A.
M. 3C
\,
4
50 P. M.
16.
8 46 A.
M.
Phases of the Moon, ]
p. S. T.
First
Quarter,
Oct. 2,
H. M.
9 31 P-
M.
Full
Moon,
Oct. 10,
8 42 A.
M.
Last
Quarter,
Oct. 18,
I 9 P.
M.
New
Moon,
Oct. 25,
3 28 p.
M.
The Sun,
R
A.
Declina
tion.
Rises.
Transits.
Sets.
1897.
H.
M.
c
/
H. M.
H. M.
H. M.
Oct. I.
12
31
- 3
24
6 I A.M.
II 50 A.M.
5 39P-M.
II.
13
8
- 7
14
6 12
II 47
5 22
21.
13
45
— 10
54
6 23
II 45
5 7
31.
14
24
— 14
18
6 33
II 44
4 55
Mercury,
Oct. I.
11
37
+ 2
37
4 46 A.M.
10 55 A.M.
5 4P-M.
II.
12
7
+ I
16
4 51
ID 46
4 59
21.
13
4
- 4
56
5 21
II 4
4 47
31.
14
6
— II
51
6 7
Venus,
II 26
4 45
Oct. I.
10
32
+ 10
16
3 15 A.M.
9 50 A.M.
4 25 P.M.
II.
II
18
+ 5
57
3 37
9 57
4 17
21.
12
3
+ I
18
3 59
10 3
4 7
31.
12
49
- 3
29'
4 20
Mars,
xo 9
3 58
Oct. I.
13
30
- 9
6
7 19 A.M.
12 48 P.M.
617 P.M.
II.
13
55
— 11
37
7 14
12 34
5 54
21.
14
22
- 14
7 9
12 21
5 33
31-
14
49
- 16
15
7 6
12 9
5 12
Jupiter,
Oct. I.
II
42
+ 3
7
4 50 A.M.
II OA.M.
5 10 P.M.
II.
II
50
+ 2
17
4 21
10 29
4 37
21.
II
57
+ I
29
3 52
9 57
4 2
31.
12
5
+
43
3 23
Saturn,
9 25
3 27
Oct. I.
15
42
- 17 48
10 2 A.M.
3 P.M.
7 58 P.M.
II.
15
46
— 18
2
9 27
2 24
7 21
21.
15
50
— 18
17
8 53
I 49
6 45
31.
15
55
- 18
32
8 19
I 14
6 9
Astronomical Society of the Pacific.
i8i
1897.
Oct. I.
II.
21.
31.
Oct. I.
II.
21.
31.
R.A.
H. M.
15 37
15 39
15 41
15 43
5 28
5 28
5 27
5 26
Declination.
o /
— 19 II
— 19 18
- 19 25
- 19 34
Uranus.
Rises.
H. M.
10 I A.M.
9 25
8 49
8 12
Neptune.
+ 21 52
+ 21 52
+ 21 51
+ 21 50
9 24 P.M.
8 45
8 5
7 25
Transits.
H. M.
2 54 P.M.
2 17
I 40
I 3
4 43 A.M.
4 4
3 24
2 44
Sets.
H. M.
7 47 P.M.
7 9
6 31
5 54
12 2 P.M.
II 23 A.M.
10 43
10 3
Minima of Algol. P. S. T.
Oct.
3-
6.
9-
12.
15-
17.
I
10
7
4
12
9
39 P. M.
27 A. M.
16 A. M.
5 A. M.
5 A. M.
43 p. M.
Oct.
Nov.
20.
23.
26.
29.
I.
6
3
12
8
5
M.
32 P. M.
21 P. M.
10 P. M.
58 A. M.
47 A. M.
Phases of the Moon, P. S. T.
1897.
Nov. I.
II.
21.
Dec. I.
Nov. I.
II.
21.
Dec. I.
Nov. I.
II.
21.
Dec. I.
First Quarter,
Full Moon,
Last Quarter,
New Moon,
First Quarter,
R. A.
H. M.
14 28
15 8
15 49
16 32
14 U
15 15
16 20
17 26
12 54
13 40
14 28
15 17
Nov. I,
Nov. 9,
Nov. 17,
Nov. 24,
Nov. 30,
The Sun.
H. M.
6 37 A. M.
I 50 A. M.
6 2 A. M.
I 20 A. M.
7 14 P. M.
Declination.
o '
- 14 37
- 17 35
- 20 3
- 21 54
Rises.
H. M.
6 34 A.M.
6 45
6 57
7 8
Mercury.
12 31 611 A.M.
18 25 6 57
22 49 7 39
25 19 8 17
Venus.
4 22 A.M.
• 3 58
8 40
13 5
16 58
4 46
5 10
5 33
Transits.
H. M.
II
II
II
II
44 A.M.
44
46
49
II 28 A.M.
11 52
12 17 P.M.
12 44
10 9 A.M.
10 16
10 25
10 34
Sets.
H. M.
4 54P-M.
4 43
4 35
4 30
4 45 P.M.
4 47
4 55
5 II
3 56 P.M.
3 46
3 40
3 35
I82
Publications of the
Mars.
1897.
R. A.
Declination.
Rises.
Transiu.
Sets.
H. »
1.
'
H. M.
H.
M.
H.
M.
Nov. I.
H 52
- 16
28
7 4 A.M.
12
7 P.M.
5
ID P.M.
II.
15
20
-18
29
7 I
II
56 A.M.
4
51
21.
15
49
— 20
15
6 58
II
46
4
34
Dec. I.
16
19
— 21
44
6 55
II
37
4
19
Jupiter.
Nov. I.
12
5
+
39
3 19 A.M.
9
21 A.M.
3
23 P.M.
II.
12
12
—
4
2 49
8
49
2
49
21.
12
18
—
43
2 18
8
16
2
14
Dec. I.
12
24
— I
18
I 46
Saturn.
7
42
I
38
Nov. I.
15
55
- 18
34
8 16 A.M.
I
II P.M.
6
6 p.m.
II.
16
— 18
49
7 42
12
36
5
30
21.
16
5
- 19
3
7 9
12
2
4
55
Dec. I.
16
10
— 19
17
635
Uranus.
II
27 A.M.
4
19
Nov. I.
15
44
- 19
34
8 8 A.M.
12
59 P.M.
5
50 P.M.
II.
15
46
— 19
42
7 32
12
22
5
12
21.
15
49
— 19
51
6 57
II
46 A.M.
4
35
Dec. I.
15
51
-19
59
6 20
II
9
3 58
Neptune.
Nov. I.
5
26
+ 21
50
7 26 P.M.
2
44 A.M.
10
2 A.M.
II.
5
25
+ 21
49
6 46
2
4
9
22
21.
5
24
+ 21
48
6 5
I
23
8
41
Dec. I.
5
23
+ 21
47
5 24
12
42
8
Eclipses of Jupiter^s Satellites, P. S.
(Oflr Ief\ hand limb as seen in an inverting telescope.)
H. M.
I, D, Nov.
2.
6 43 A. M.
I, D, Nov.
II.
3 4 A.M.
IV, D,
4.
12 45 A. M.
I. D.
18.
4 57 A. M.
I, D.
4.
I 1 1 A. M.
I. D,
19.
II 26 p. M.
IV, R,
4-
3 24 A. M.
II. D.
21.
6 48 A. M.
III, D.
4.
6 35 A. M.
I, D.
25.
6 51 A. M.
II, D,
7.
I 39 A. M.
I, D,
27.
I 19 A. M.
Minima of Algol, P. S.
T.
H. M.
H. M.
Nov. I.
5 47 A. m.
Nov. 18.
10 41 A. M.
4.
2 36 A. M.
21.
7 30 A. M,
6.
II 25 P. M.
24.
4 19 A. M,
9.
8 14 P. M.
27.
I 7 A. M,
12.
5 3 P. M.
29.
9 56 P. M.
15-
I 52 p. M.
Astronomical Society of the Pacific. 183
Phases of the Moon, P. S. T.
Full
Moon,
Dec. 8,
H. M.
8 54 p. M.
Last
Quarter,
Dec. 16,
8 22 p. M.
New
Moon,
Dec. 23,
II 55A.M.
First
Quarter,
Dec. 30,
II 27 A. M.
The Sun.
R. A.
Declination.
Rises.
Transits.
Sets.
1897.
H. 1
M.
'
H. M.
H. M.
H. M.
Dec. I.
16
32
— 21
54
7 8 A.M.
II 49 A.M.
4 30 P.M.
II.
17
15
-23
4
7 17
II 54
4 31
21.
18
-23
27
7 24
II 59
4 34
31.
18
44
— 23
4
7 36
12 3 P.M.
4 40
Mercury.
Dec. I.
17
26
-25
19
8 17 A.M.
12 44 P.M.
5 II P.M.
II.
18
32
-25
32
8 46
I II
5 36
21.
19 27
-23
26
8 51
I 26
6 I
31.
19
38
— 20
29
8 10
Venus,
12 57
5 44
Dec I.
15
17
- 16
58
5 33 A.M.
ID 34 A.M.
3 35PM.
II.
16
8
— 20
6
5 57
ID 46
3 35
21.
17
I
— 22
18
6 20
II
3 40
31.
17
56
- 23
24
6 40
Mars.
II 15
3 50
Dec. I.
16
19
— 21
44
6 55 A.M.
11 37 A.M.
4 19 P.M.
II.
16
50
— 22
54
6 51
11 28
4 5
21.
17
22
-23
40
6 48
II 21
3 54
31.
17
54
-24
3
6 42
II 14
3 46
Jupiter.
Dec I.
12
24
— I
18
I 46 A.M.
7 42 A.M.
I 38 P.M.
II.
12
29
— I
48
1 14
7 8
I 2
21.
12
33
— 2
13
12 40
6 33
12 26
31-
12
37
— 2
31
12 6
Saturn.
5 57
11 48 A.M.
Dec I.
16
ID
- 19
17
6 35 A.M.
II 27 A.M.
4 19 P.M.
II.
16
14
- 19
30
6 2
10 53
3 44
21.
16
19
- 19 42
5 28
10 18
3 8
31.
16
24
- 19
52
4 54
Uranus,
9 43
2 32
Dec I.
15
51
- 19
59
6 20 A.M.
II 9 A.M.
3 58 P.M.
II.
15
54
— 20
6
5 43
10 32
3 21
21.
15
56
— 20
13
5 7
9 55
2 43
31.
15
58
— 20
20
4 30
9 18
2 6
1 84
Publications of the
Neptune,
R. A.
Declination.
Rises.
1897.
H. M.
H. M.
Dec. I.
5 23
+ 21 47
5 24P.M
II.
5 22
+ 21 46
4 44.
21.
5 21
+ 21 45
3 59
31. 5 20 +21 44 3 19
Transits. Sets.
H. M. H. M.
12 42 A.M. 8 OA.M.
12 2 7 20
II 17 P.M. 6 35
10 37
5 55
Eclipses of Jupiter-s Satellites, P. S. T.
(Off left-band limb as seen in an inverting telescope.)
Ill, R, Dec.
3-
H. M.
I 20 A. M.
II. D, Dec.
16.
H. M.
3 49 A.M.
I, D,
4-
3 13 A. M.
III. D,
17.
6 22 A. M.
II, D,
9-
I 14 A.M.
I.D,
20.
I 27 A. M.
III. D,
10.
2 24 A. M.
II. D,
23-
6 24 A. M.
III, r;
10.
5 17 A. M.
IV, D.
24.
6 49 A. M.
I,D.
12.
II 34 P. M.
I, D,
27-
3 20 A. M.
Minima of Algol, P. S.
T.
H. M.
H. M.
Dec. 2.
6 45 p. M.
Dec. 19.
II 39 P. M.
5-
. 3 34 P- M.
22.
8 28 P. M.
8.
12 23 P. M.
25-
5 16 P. M.
II.
9 12 A. M.
28.
2 5 P. M.
14.
6 I A. M.
31.
10 54 A. M.
17.
2 50 A. M.
THE BRUCE PHOTOMETERS OF THE LICK
OBSERVATORY.
By R. G. Aitken.
[Abstract.]
A paper with the above title was prepared for the September
meeting of the Society, and the following abstract is now printed to
put on permanent record some data concerning the instruments.
Photometer II. in principle is identical with Photometer H.
described in the H. C. O. Annals, Vol. XL, p. i. It consists of
a double image prism, which can be moved along the axis of the-
telescope to any desired distance from the focus, and a NicoL
prism in front of the eye-piece, which can be turned by an amount
which is measured with a graduated-circle and index.
In practice, the double image prism is moved toward or away
from the focus, and the whole instrument turned on its axis, until
the ordinary image of one of the stars to be compared is brought
as close as is desired to the extraordinary image of the other star
— the two remaining images either being cut off by the eye-
Astronomical Society of the Pacific, 185
stop, or being symmetrically placed in the field of view, with
respect to the two images that are to be compared. The Nicol
is then turned until the two images are of equal brightness,
and its position is read on the graduated circle. Four such posi-
tions are found — one on each side of the two points of disappear-
ance of the brighter image. Turning the whole photometer
through 180°, the images at first neglected are brought together
and a similar comparison is made. From these readings the
angular distance of the point of equality of the images of the two
stars (v) from the point of dbappearance of the brighter star
(Vo) is determined; and the difference in magnitude (M), (using
Pogson's photometric scale) follows from the equation
M = 5 log tan (v — Vo).
The Harvard College observers have found that * * this instru-
ment leaves little to be desired in the measurement of close
double stars. Nearly all sources of systematic error are elimin-
ated when it is properly used, and the relative brightness of two
adjacent stars may be determined with great accuracy.'* In fact,
they have found that **the results on different nights will give
average deviations considerably less than a tenth of a magnitude.*'
A careful test of the Bruce Photometer II., attached to the
thirty-six- inch telescope, has proved that it will give results in
every way comparable with those obtained with the Harvard
instrument.
This photometer, however, when attached to the thirty-six-
inch cannot be used to compare stars more than two minutes
of arc apart.
The Bruce Photometer I., which is a duplicate of the '* New
Form of Stellar Photometer,** described by Professor E. C.
Pickering in the Astrophysical Journal for August, 1895, is
based upon the same photometric principles as number II., and
the method of observing and of reducing the observations is the
same for both instruments. The only difference is, that only one
image of each star is seen in the field of view at one time, the
other two images being cut off by the eye- stop.
But in Photometer I. the double image prism, which has an
angle of separation of about four inches, is placed at the focus,
and two images of the object glass are formed by two achromatic
prisms, which can be slid by a chain and sprocket-wheel to a
distance of about forty inches from the focus. The position of
these prisms is indicated by a divided wheel, which is turned by
1 86 Publications of the
a screw cut on the axis of the sprocket-wheel. One turn of the
screw moves the prisms about three inches. The achromatic
prisms are about two and one-quarter inches (6 cm.) on a side and
their combined deviation is 4^ 23' 35", somewhat greater than
that of the double image prism when they are brought near to
it, but less when they are moved to their extreme position.
The simplicity of construction of this instrument insures the
stability of its adjustments. Practically » it is only necessary to
see that the line joining the centres of the two images is perpen-
dicular to the edges of the achromatic prisms. If this is not the
case, the adjustment is easily made by turning the tube holding
the double image prism.
When the photometer is attached to the thirty-six-inch tele-
scope and the achromatic prisms are brought as near as possible
to the focus, stars about two and one-half minutes of arc apart
may be compared. This is the minimum limit. The practical
maximum limit is reached when the prisms are moved thirty-
two inches from the focus, for at this point the diameter of the
cone of rays from the object-glass equals the length of the side
of the achromatic prism. In this position of the prisms, stars
about twelve minutes of arc apart may be compared.
The loss of light by the process of polarization and by reflec-
tion and absorption of the various prisms used, reduces the
brightness of the stars by about one and one-half magnitudes.
It is, therefore, possible to measure with great accuracy the bright-
ness of any star one and one-half magnitudes brighter than the
limit of visibility of the telescope.
Mt. Hamilton, September 6, 1897.
CATALOGUE NO. II, OF NEBULAE DISCOVERED AT
THE LOWE OBSERVATORY, ECHO MOUN-
TAIN, CALIFORNIA.
By Lewis Swift.
The following list of twenty-five nebulae follows No. I of fifty,
discovered at this observatory and published in the Astronomical
/oumal of November 13, 1896, and also in the Publications of the
Astronomical Society of the Pacific. Since my return to this
observatory in April last, after an absence of several months, I
have devoted my time to searching for comets, as well as for
Astronomical Society of the Pacific.
187
nebulae, for which this anomalous climate is so well adapted.
The following facts will illustrate its truth. The number of clear
nights in May, 1897, were twenty-five, and rain-fall 0.87 of an
inch.. On June 28th, rain-fall o.io; in July, precipitation 0.15.
I have never seen a month, except jhe last, when every night was
clear, but in June, 1896, every one was clear with a single
exception, and that was foggy. One peculiarity about this
climate is, that there are more cloudless nights than days, which
is the reverse of conditions at the Warner Observatory at
Rochester, New York.
d
2
Datk of
Discovery.
R. A.
p
Dec.
OR 1900.
Dkscription.
h m 8
e / //
I
Mar.
23/95
8 538
+
5 22 47
eeeF. vS. IE. v close f. 12- * .D ♦ nf. points
nearly to it. eedif.
2
May
4,
II 47 23
—
3 10 12
vF. pS. R. B*f55'. npof 2.
3 Mar.
23/95
II 48 33
—
3 25 15
eP. pS. R. 2 B St in field one n the other np.
4
Mar.
23. '95
II 48 48
—
4 34 15
eeeF. vS. eE. a ray. in vacancy. 4 F st in
line s. I B & 3 F St n.
5
May
23,
II 49 23
—
2 10
vF. vS. R. vF*near nf.
6
May
23,
12 43 2
+ 54 59 45
eeF. S. CE. in field with N. G. C. 4732.
7
May
23,
13 4 27
+ 53 22 48
eF. pL. R.
8
May
22,
13 18 33
+
6 45 16
eeeF. pS. CE. in vacancy, v dif.
9
June
25,
13 47 20
+ 14 46 55
eeeF. pL. R. eeedif. 3d of 4.
to
Apr.
30.
13 47 38
—
38
vL. pF. CE. n & s. in field with 5334. A Fst
close to each end of major axis.See note.
II
June
2.
14 46 16
+
27 59 17
eeF. S. IE. pB*p. eeedif. another near
suspected.
\i
June
2,
14 49 37
+
16 47 5
vF. pS. R. only i * near lo" nf.
13
June
21,
15 14 59
+
2 8 52
vF. vE. pS. B * in field n partly obscures it.
f4
June
3.
15 19 52
+
13 50 10
eF. pS. vF* close np.
15
June
21,
15 30
+
520
eF. pS. R. near the ist of 6 or 8 st in a
curved line.
16. July
22,
16 18 45
+
12 59 16
eeeF. S. IE. F»near f. 2 B st in field s
nearly point to it. eeedif.
ir July
1
6,
19 22
—
36 24 05
B. eS. IE. stellar, looks like close D * both
nebulous. Note.
IS ; July
6.
19 49 10
—
37 37 13
eeeF. pS. 3 st s like belt of Orion point to
it. eeedif.
19 July
6,
19 53 17
—
38 53 33
eeeF. S. IE. precedes the below 37* eedif.
pof 2.
eeF. pS. R. 8-*f2o'fof 2.
3D
July
6.
19 53 55
38 53 33
21
July
8.
19 59
—
48 42 25
eeeF. pS. R. F * near n. eedif. p. of 2.
a
July
22,
20 2 16
—
45 55 42
vF. pS. R.
»3JJune
9.
20 38 39
—
30 16 30
eF. pS. vE. eeF * and a vF * near sf. point
to it. s p. of 2.
Mjune
9.
20 38 45
—
30 6 30
eeF. pS. vE. 8r*3i'n. v dif. nf of 2.
!5 Jaly
7.
22 35
—
38 33 48
vF. pS. R.
i88 Publications of the
Notes.
No. lo. This is a remarkable object. I have never seen one
just like it. It resembles an elliptical planetary nebula. The
light is evenly diffused, and the limb as sharp as a planet
Strange, Sir William Herschel missed it, being so near his
III 665. Munich 9619 is nf 121'.
No. 17- This also is a singular object. I have never seen
but one resembling it, and that was on the same night, which I
think is N. G. C. 6861. It resembles a close, bright, double
star, each component having a small, bright, round, star-like,
nebulous disc. A power of 200 failed to divide it
The places are for 1900.0, and the year of discovery, except
when otherwise noted, is for 1897.
N. G. C. 6550 must be struck out, as it is identical with
H. Ill 555.
ECLIPSE OF THE SUN, JULY 29, 1897.
By David E. Haddkn.
The partial eclipse of the Sun on July 29th ult. was observed in
Alta, Iowa, under favorable conditions, the sky being cloudless.
First contact occurred at 7* 33°* 02*; the Sun's disc was a little
unsteady, and this time is probably a few seconds late. Last
contact was noted at 9'' 35™ 47' and is quite accurate, the defini-
tion being fine.
The limb of the advancing Moon bisected the larger sun-spot
nearest the west limb at 7'' 47°* 20', and its reappearance was
observed at %^ 20°" 55'. An interesting phenomenon was the
apparent blackening of the umbra of the sun-spot, as the edge
of the Moon reached it (the umbra before appearing a shade
lighter than the Moon). I also noticed a peculiar lengthening of
the umbra toward the Moon's limb as it reached its edge — a
** black drop" appearance on a very small scale. I hardly
think this was owing to the inequalities of the Moon's edge,
as the same appearance was repeated during the spot's
reappearance.
The sunlight was quite decidedly changed about mid-eclipse,
and the temperature of the air in the shade fell four degrees, as
recorded by a registering minimum thermometer. Time used is
Astronomical Society of the Pacific. 189
Central Standard. Telescope used was a four-inch Brashear
equatorial, with Herschelian eye-piece, power 78.
Alta, Iowa{J^^„g42Mc/^N^ JApprox.
NOTES ON THE TOTAL ECLIPSE OF THE SUN,
JANUARY 21-22, 1898, IN INDIA.
By Colonel A. Burton-Brown, R. A., F. R. A. S.
[Member of the Astronomical Society of the Pacific]
The central line of totality on the west coast of India passes
between Ratnagiri and Rajapur, the latitude of which place is
16° 40' N., and longitude 73° 35' E. of Greenwich. Totality com-
mences 22d — o^ 47" 42"; has a duration of nearly 2™ 2', and the
Sun's altitude is 53°, about. The line of shadow strikes across
India, cutting the river Ganges a few miles south of Balia and pass-
ing^ on to Jubang in Nepaul, where the duration of totality would
be reduced by about 23" and Sun's altitude by about one-third.
There are many circumstances which will influence observers in
selecting stations beyond that of the Sun's altitude and length of
totality. The most important one will probably be the weather
conditions between o** 30" and z^ 15"*. Now, if India were a great
plain, we might consider that in the third week in January that the
conditions of weather will be equally favorable from the west coast
to the Ganges, but as the country is a series of undulations, includ-
ing some hills, local circumstances must be takeh into account,
and from my own observations and those of others, I am inclined
to consider the height of the station which is from 500 to 1500
feet above the sea would be the most satisfactory if not in close
proximity to higher ground, and if not within twenty miles either
of the seacoast or the Ganges river. Places from 73° 30' to
75° 45' east longitude I find are slightly freer from cloud than
places east and west of that longitude. Although the daily mean
cloud in other places may not be greater, it is often more variable.
I am inclined to advise, from atmospheric conditions as well as the
position of the Sun and length of totality, that a fairly elevated
position on or near the central line between those limits be taken
up. No doubt stations north of Rajapur and Nagpur will be
selected by some observers, but while the climatic conditions
I90 Publications of the
should be good there, they will probably not come up to a carefully
selected spot near Indapur, Aundh, or Parainda, none of which
are difficult to get to with the requisite instruments. I would
here take the opportunity of saying, if a fairly large party is
formed, they should be divided as much as possible. This I
strongly urged for the British-Norwegian expedition in 1896, but
instead of selecting places near Bodo on the west coast and
places on the Tana Fjord and Russian frontier, as well as Vardoe
and Vadsoe, they all huddled together at the latter two most
accessible places, where, unfortunately meeting with unfavorable
atmospheric conditions, no good results were obtained. It must
not be forgotten that two or three exceptional circumstances are
now occurring in India — famine and plague — and more recently,
earthquakes, so that it may be impossible much before the close
of the year to give an exact locality suitable for a scientific expe-
dition. We all hope that in the cooler season these unfortunate
conditions will be materially improved and that there may be
no obstacle to progress in any part of the country. An elevated
post near Indapur would give about 1°* 58' totality at Sun*s
altitude of about fifty degrees.
THE CAUSE OF GRAVITATION.*
By V. Wellman.
According to Newton's law of gravitation, the attractive
force of matter is proportional to the mass and inversely propor-
tional to the square of the distance. The rigorous validity of
this law has, in recent times, been doubted; but its extraordinary
approximation to the truth is unquestionable. Consequently,
without going into the question as to whether the law is rigor-
ously valid, I will endeavor to verify it.
The propagation of light through interstellar space shows
that this space cannot be absolutely vacant. It is filled with a
material, the condition of which we assume to be like that of
a gas of extraordinarily rare density. The barometer- formula
gives, for the density of air at an altitude, h = 00, which, there-
fore, corresponds approximately to the density of the interstellar
medium,
D 00 = D, 10-346,
• Translated from Astronomische Nachrichten by E. F. Coddington.
Astronomical Society of the Pacific. 191
where Do designates the density of air at sea level. Evidently
this formulae is not exact, since Mariott's law, on which it is
based, holds good only for a finite pressure and therefore for a
finite altitude. Nevertheless, this value can be regarded as an
approximate measure for the density of the interstellar medium.
We can also assume that the matter of bodies is composed of a
very large number of very minute particles, whose dimensions are
exceedingly small compared with the space between them. Sup-
pose we consider a single particle of the Sun and one of a planet.
The particles of the interstellar medium move, according to the
kinetic theory of gases, with an enormous velocity among each
other. If we imagine a body particle, a, it will be struck on all
sides by particles of the medium ; therefore will receive an equal
pressure on all sides and will remain at rest. If there exists a
second particle, by a will not be struck in the direction ba^ and
likewise b will not be struck in the direction ab. Therefore, the
impulses acting on a in the direction ab and those acting on b
in the direction ba^ will tend to push the two particles together;
that is, there will seem to be an attractive force between them.
The question is, whether this force will act according to New-
ton's law.
First of all it is clear that a body consisting of n particles will
receive n times the number of impulses, and, therefore, the
moving force will be proportional to the mass, provided the
single particles are far enough apart not to cover each other from
impulses, and that each particle is struck just as often as it would
be if it existed alone; or, in other words, provided the interstellar
medium can go through the celestial bodies without apparent
resistance. Evidently it can and must happen that in a certain
element of time some body atoms will cover others, but in the
same or equal elements of time other body atoms will receive
many impulses. Therefore, according to the theory of proba-
bilities, since the number of particles is assumed to be infinitely
large, there will be a constant value for the number of impulses
which lies within the limits of our perception, and which is
proportional to the number of body atoms or to the mass. The
phenomenon of the diffusion of gases seems to give additional
evidence that we can assume such a free passage of the inter-
stellar medium.
According to the investigations of Graham especially, the
192 Publications of the
diffusion volume (V) df a gas is inversely proportional to the
density of the gas; that is;
In fact, this law is easily explained from molecular structure.
The less dense the particles of a gas are, the more of the same will
pass through resisting bodies without striking them. That is, the
number n of gas particles going through each row of body
particles, is inversely proportional to the density 8 of the gas.
But if the number of particles passing a row be increased v times,
the number passing a cross-section and also the volume will
be increased v* times, and the ratio of the volumes will be
inversely as the square root of the densities.
According to this law, it is evident that the ability of the
celestial bodies to allow such a free passage of the interstellar
medium of the above-mentioned minimum density must be such
that the above-made assumption will appear correct. Of course
it will not be maintained here that the passage of the world
particles (as we will name those of the interstellar medium)
occurs accurately according to Graham's law; rather it will only
be shown that the assumption of this perviousness of the celestial
bodies for the world particles in the assumed measure contains
no inconsistency or improbability.
We come then to the consideration of the question, whether
the power produced by the interstellar medium must act inversely
proportional to the square root of the distance. For this purpose
we make the assumption that the density of this medium is con-
stant within an attraction system (solar system), if not in the
whole universe. This assumption is certainly allowable, since
there is no evidence for the opposite assumption of unequal
densities; and if there should be inequalities of densities, tliey
would become equalized by expansion in finite distances and in a
finite length of time. Moreover, it is not absolutely excluded
that in other attraction systems, at an infinite distance away, there
cannot exist temporarily other densities.
We see that, of the world particles, only those have a dislo-
cating effect upon the body particles which move in a line connect-
ing the two particles; or that the planets are pushed towards the
Sun only by those world particles which move in directions
radial to the Sun. The number of these motions is independent
of the distance from the Sun; therefore, an equal number of
Astronomical Society of the Pacific. 193
world particles will rebound radially against the surfaces of spheres
which surround the Sun concentrically. Therefore, the number of
impulses received by a surface unit is inversely proportional to
the square of the distance, as Newton's law requires.
I will illustrate this point in another way. The pressure of a
gas upon the side q of the inclosing vessel is,
p = c m u'q ^,
where m is the mass of a gas particle, u its velocity, n the
number of particles, and / the length of the enclosing vessel to
the opposite, side q. For - we can use the density of the gas 8,
whereby we become independent of the assumption of finite
enclosed space. Therefore, the pressure of the interstellar
medium upon the surface units of two spheres described about
the Sun with radii r and r' is,
c m u' q 8 , , c m u' q 8'
p = -i— and p = ^— -i —
According to Newton's law, the following relation should
hold:-E. = -^, and, therefore, 8 must equal 8'. That is, New-
ton's law is satisfied if the density of the interstellar medium is
constant within the attraction sphere.
It is also easily seen by a simple geometrical representation,
without applying mathematical formulae, that the pressure directed
radially toward a center must be inversely proportional to the
square of the radius. Within other attraction-spheres in which
other densities of the interstellar medium reign, Newton's law of
gravitation would still be valid, but the gravitation constant for
the unit of mass would have different values. Possibly the
remarkable mass and distance relations reigning in some of the
systems, such as Aigoiy are due to these conditions. At places
of transition, where the density of the medium is variable, a
stable system is as a rule impossible.
Since the conceptions given in the above lines will probably
meet many objections, I may be permitted to discuss some of
the expected ones. To the assumed rare density of the inter-
stellar medium, comes the objection that the number of single
impulses of the world particles in the unit of time is far less than
that of a particle of gas (earthly), whereby its effect must be
correspondingly diminished. But this decrease of effect would
194 Publications of the
be more than overbalanced by the enormous velocity which we
must attribute to the world particles, wholly disregarding the
above- made assumptions, except those concerning light velocity.
The velocity of the world particles is assumed to be of the same
order of magnitude as the velocity of light.
If such a velocity is assumed, the number of particles passing
a plane in the unit of time will be increased in the same measure,
while the kinetic energy will be increased according to the square
of the velocity. To be sure, masses moved with such a velocity
appear very improbable, but the assumed wave velocities in the
theory of light are no more plausible, and besides an upper
limit to cosmical relations can scarcely be drawn. Indeed, the
assumed value is not so striking if, instead of the velocity of
the world particles, the kinetic energy be introduced, which is
infinitely small compared to that of a planet, in spite of their very
much greater velocity.
Furthermore, the attraction of the formulae holding good for
the pressure of a gas appears to be unadmissible, since with gases
the rectilinear courses traversed by the gas particles are infinitely
small compared with those which we have assumed. It is also
easily seen that the above-introduced formula for p is nothing
other than the expression for the kinetic energy and, therefore, in
general, is valid.
Astronomical Society of the Pacific, i95
NOTICES FROM THE LICK OBSERVATORY.*
Prepared by Members of the Staff.
Observation of the Partial Solar Eclipse, July 29, 1897.
At Professor Holden*s request, I observed the times of con-
tact for this eclipse, using the twelve-inch telescope cut down to
four inches aperture, and a Herschel prism with eye-piece of
150 diameters. The Moon's disc was first seen certainly at
5^ 25" 8' A.M., P. S. T. Geometrical contact occurred one or
two seconds earlier. The observed time of last contact was
7* 9" 14" A.M. These times are seven seconds later and seven
seconds earlier, respectively, than the predicted times of contact
for the Lick Observatory computed by Mr. Perrine (see Pub-
lications A. S. P. , No. 55).
The Moon's disc touched the umbra of a well-developed
sun-spot on the south-preceding quadrant of the Sun's disc at
5** 38" 12', and the umbra had entirely disappeared at ^ 39" 29'.
At the time of greatest obscuration about one-third of the
Sun's disc was covered. R. G. Aitken.
Mt. Hamilton, July 29, 1897.
Unusual Lunar Halo, August 5, 1897.
Napa, Cal., August 5, 1897.
* * * * On August 5th at 4:45 p.m. * * * a
circle (appeared) about the Moon, or rather around the circular
half. This was distant one-tenth the diameter of the Moon and
a bright thread-like line. (It was) at times very distinct, but
again undiscernable. * * * *
(Signed) Kate Ames,
School Superintendent
• Lick Astronomical Department of the University of California.
196 Publications of the
The Work of the Lick Observatory, 1888-1897.*
** In your letter of June 26th, you ask for some account of the
work in progress here for Popular Astronomy^ which I am very
glad to give. A report of the sort is annually made to the
Regents of the University of California, and from the forthcoming
report the following summary is made. It must be remembered
that the work of this year is in continuation of previous work, and
often in pursuance of plans laid down in 1874 — twenty-three
years ago. While the resources of the Lick Observatory are
large in comparison with those of many college observatories,
they are very small in relation to those of the great establishments
of Greenwich, Paris, Pulkova, Washington, and Harvard College.
For instance, the whole available income of the Lick Obser\'atory
for the coming fiscal year (exclusive of salaries) is $5145. This
sum must keep all the buildings painted and in repair; keep all
our reservoirs and some ^\^ miles of underground pipes in order;
provide for all painting, plumbing, brick-laying, pipe- fitting,
carpenter work, machine work, etc., etc., in the observatory and
in the houses of astronomers and workmen; buy all supplies,
such as lumber, hay, iron, brick, etc.; pay for all instrument
making not done in the observatory; pay all freight, express
and telegraph bills; maintain a telephone line seventeen miles
long in good order; pay for fuel; purchase books for the library;
provide any needed apparatus for all the instruments; and, this
year, buy much of the material needed for an eclipse expedition
to India. It is no small task to make the small income cover
the requirements. Every want that is felt in a large city is felt
here. The circumstances at Mount Hamilton are as different as
possible from those at eastern observatories. There each person
must provide for his own personal comfort; here the comfort of
each one must be secured by the expenditure of the annual
appropriation. If it is insufiicient, every person suffers in some
degree.
The astronomical efficiency of the Lick Observatory cannot be
properly estimated without taking such material and social con-
siderations into account. Under the circumstances, I do not
think it is too much to claim that its efficiency during the nine
years of its life has been satisfactory. This has only been
attained by good will and earnest effort on the part of all con-
• Reprinted from Popular Astronomy of Aufpist, 1897.
Astronomical Society of the Pacific. i97
cemed — regents, astronomers, mechanics, workmen. The sum-
mary of work for which you asked, is given below.
Double Stars have been measured here in past years in great
numbers by Professor Burnham, and at the present time Pro-
fessors ScHAEBERLE, HussEV and AiTKEN are engaged in such
work for parts of their time.
The Satellites of Mars, Jupiter, Uranus and Neptune have
been regularly observed here for the past nine years by Messrs.
ScHAEBERLE, Barnard, Campbell and HussEV. A fifth
satellite oi Jupiter was discovered by Professor Barnard in 1892.
The Planets, especially Mars, Jupiter, Saturn (and also Ve7ius
and Uranus), have been systematically observed for their physical
features at every opposition by Messrs. Holden, Schaeberle,
Keeler, Barnard and Hussev. For several oppositions of
Mars, the planet has been followed by Messrs. Holden, Schae-
berle and Campbell during every available hour.
Comets have been discovered here in great numbers. Ten
comets (seven unexpected) were discovered by Professor Bar-
nard from 1888 to 1892; ^v^ (four unexpected) by Mr. Perrine
from 1895 to date. The long series of observations of these and
other comets by Messrs. Barnard, Campbell, Hussey, Per-
rine and AiTKEN, are a contribution to science even more
important than the discoveries themselves.
Comet Orbits have been computed here by Messrs. Schae-
berle, Campbell, Hussey, Perrine and Aitken; and all
comets discovered at the observatory have had their first orbits
calculated by officers of the University. In this work, Professor
Leuschner, of Berkeley, a former student here, and his
assistant, Mr. F. H. Sears, have rendered assistance which is
much appreciated.
Meteors have been observed and photographed here (and
elsewhere) by all the astronomers, and their orbits calculated by
Messrs. Holden and Schaeberle.
Double-Star Orbits have also been computed by Professor
Schaeberle.
The Zodiacal Light was regularly observed (visually) by Pro-
fessor Barnard.
The Aurora has been regularly observed (spectroscopically)
by Professor Campbell.
Typical, or Remarkable Cloud-forms are regularly photo-
grraphed by Mr. Pauli, janitor of the observatory.
198 Publications of the
Nebulae have been observed (visually, photographically and
spectroscopically) by Messrs. Holden, Burnham, Schaeberle,
Barnard and Campbell.
Star Maps have been made and published by Mr. Tucker.
Photometry (photographic and visual): — of Eclipses and
Stars — has been attended to by Messrs. Holden, Schaeberle,
Campbell and Leuschner.
Solar Eclipses: — Those of January and December, 1889,
April, 1893, August, 1896, have been observed by Messrs.
Burnham, Schaeberle, Keeler, Barnard, Hill, Leusch-
ner and Campbell — and the latter will observe the eclipse of
January, 1898, in India.
Lunar Eclipses. — All lunar eclipses visible here have been
observed.
Occultations. — A series of occultations has been observed here
by Professor Leuschner.
Transits of Mercury, — Three transits of Mercury have been
observed (either visually or photographically).
Transits of Venus, — That of 1882 was successfully photo-
graphed here by Professor Todd.
Catalogues of Stars. — Two such are in progress of preparation.
I St. A Catalogue of Double Stars and Coast Survey Stars
from observations by Professor Schaeberle has been (pardy)
reduced, on lines laid down by myself, by Messrs. Schaeberle,
Campbell, Leuschner, Aitken and Professor Bigelow, and
Mrs. Updegraff. Professor Aitken has spent more than a
year on this work.
2d. A Catalogue of 38,000 Stars from Washington observa-
tions is well towards completion. The reductions have been made
chiefly by Messrs. Holden and Aitken. The original observa-
tions as printed were full of errors. The final places will be
considerably more precise in declination and somewhat less pre-
cise in right ascension than the southern zones of Argelander.
Solar Photography. — Some 1800 negatives of the Sun (taken
with the photoheliograph) have been secured by Mr. Perrine,
and since April, 1896, some 450 more by Mr. Colton. Excellent
experimental solar photographs on a large scale have been made
with the thirty-six- inch telescope, and it is hoped to go very
much further with this work during the summer of 1897.
Lunar Photography. — A very full series of focal negatives has
been made with the thirty-six-inch telescope, chiefly by Messrs.
Astronomical Society of the Pacific, i99
HoLDEN and Colton. An atlas on the scale of X-feet to the
Moon's diameter has been prepared from these by Professor
Weinek at Prague. Enlargements in the telescope have been
made by Messrs. Holden, Colton and Perrine, and five
plates of a Moon atlas on the scale of Ill-feet to the Moon*s
diameter have already been distributed. Twelve more plates are
now in the hands of the engraver and will soon be issued; and
about twenty more are ready to be published when the funds are
available. The atlas will be complete with about sixty plates.
All the work in the dark room is done by Mr. Colton.
Photographs of the Milky Way. — A great number of such
pictures has been obtained by Professor Barnard, who is pre-
paring them for publication.
Photographs of Planets (especially of Jupiter) have been
regularly made by Messrs. Holden, Schaeberle and Colton.
Photographs of Comets have been secured by Messrs. Bar-
nard, HussEY and Colton.
Visual Photometry. — Two fine photometers of Professor
Pickering's design have lately been given to us by Miss Bruce.
They will be used by Professor Aitken, chiefly on double stars
at present.
Spectroscopic Observations of nebulae, new stars, comets,
stars and planets, have been made by Messrs. Keeler and
Campbell. The chief problem of the great telescope is to
determine the motion of the solar system by spectroscopic
observations. It was first attacked here in 1888, and since
that time it has been considered as our most important work.
The results now attained by Professor Campbell are of unex-
ampled precision, and some of them will be published shortly.
Many unexpected delays have occurred in this research, which
has been under the charge of Messrs. Keeler, Crew and
Campbell.
Time-signals are sent out daily. Mr. Tucker is in charge of
our clocks.
Meridian-Circle Observations. — Mr. Tucker has completed a
fine series of observations of all stars contained in any of the
great Ephemerides and not contained in the Berliner Jahrbuch.
This work is all ready to print. He has also determined the
places of a long list of stars used by Professor Doolittle to
determine the latitude of Lehigh University. The division
errors of the one degree spaces of both circles of the instrument
200 Publications of the
have been determined by Mr. Tucker, with the assistance of
Mr. AlTKEN.
Meteorological Observations (tri- daily) have been regularly
made. They are now in charge of Professor Aitken. A sum-
mary of all meteorological observations made here from 1888 to
1897 is in course of preparation by Mr. Perrine.
Earthquake Observations are obtained on our two seismo-
graphs, which are in charge of Mr. Perrine. A complete list
of all recorded earthquakes on the Pacific Coast from 1769 to
1897, has just been prepared by Professor Holden.
Publications of the Observatory. — The observatory has already
issued three quarto volumes and five octavos, besides several
pamphlets and the Moon- Atlas. The Smithsonian Institution
has lately published an octavo prepared here by Professor
Holden — '* Mountain Observatories *' — and will probably print
his list of recorded earthquakes, just mentioned. Notices from
the Lick Observatory regularly appear in the Publications of the
Astronomical Society of the Pacific. More than 1200 contribu-
tions to astronomical and other journals have been made by the
officers of the observatory since 1888.
Trial of the Crosslev Reflector. — This fine instrument, which
has done such good work in the hands of Mr. Common, was
presented to the Lick Observatory by Mr. Crossley in 1895.
It was completely mounted in June, 1896, and given over to
Professor Hussey for trial. The work begun in 1896 is now
being prosecuted. Photography in the Newtonian and principal
foci will be tried by Professor Hussey, and Professor Campbell
has a programme of spectroscopic observations to be carried on
with the Bruce spectrograph (constructed here) in the principal
focus. A powerful driving-clock (the Bruce clock) has been
made here from drawings by Professor Hussey. It Is essentially
a copy, in litde, of the Warner & Swasey clock of the thirty-
six-inch equatorial. Its conical pendulum weighs about fifty-six
pounds.
The Schaeberle eighteen-inch Reflector has been used for
some years past in experiments in celestial photography by its
maker, Professor Schaeberle. Very interesting photographs
oi Jupiter have been obtained.
The Crocker Photographic Telescopes (a pair of Willard
portrait lenses) will soon be mounted in a new dome near the
Crossley reflector. A twelve-inch mirror (by Professor Schae-
Astronomical Society of the Pacific. 201
berle) of very short focus, is to be mounted on the same
stand.**
Edward S. Holden.
Lick Observatory, July 7, 1897.
Inventory, etc., of Lick Observatory Buildings and
Equipment, June 30, 1897.
Mr. Perrine, Secretary of the Lick Observatory, has prepared
a complete estimate of the cost of the buildings, instruments and
equipment of the Lick Observatory up to June 30, 1897, inclusive.
It is, summarized, as follows: —
Cost of buildings, permanent equipment, etc., paid
from the Lick Fund, 1 875-1 897 $609,981.84
(This leaves an endowment fund of $90,018. 16.)
Ditto, paid from the annual budgets of the Lick
Observatory, 1888-1897 11,767.10
Ditto, paid from special appropriations by the
Regents of the University, made to provide for
specific wants 2,278.00
Ditto, from gifts made by friends of the Lick
Observatory 35» 131-76
Total, $659,158.70
August 7, 1897. Edward S. Holden.
Cost of the Library of the Lick Observatory,
1875-1897.
The total cost of the Library (including buildings, etc.)
up to July I, 1889, was $5.235-50
Of this sum, the Lick Trustees expended $4837.36
previous to June i, 1888; and $398.14 was spent by
the University of California, mostly for periodicals
and binding.
Between July i, 1889 and July i, 1897, ^^ following
expenditures have been made: —
From the annual budgets of the Lick Observatory, 2,023.31
From gifts by Miss Bruce 22.50
From gifts by Mrs. Hearst 425.13
Total cost of the Library $7,706.44
The collection contains about 41 21 books and 3912
pamphlets, or about 8033 numbers. E. S. H.
202
Publications of the
Observatory Moon Atlas.
The following nineteen plates have been made by the New
York Photogravure and Color Company (No. 241 West Twenty-
third street), and will soon be distributed. Besides these, it is
proposed to reprint the heliogravure frontispiece to Volume
III of the quarto Publications of the Lick Observatory as
Plate A: 1891, October 12, 7^ 30" 54'. 5; Moon's Age^ 10 days,
3 hours (Moon in the focus of the 36-inch refractor). A number
of other negatives for the atlas are ready for printing as soon as
funds are available. Edward S. Holden.
Mt. Hamilton, September 9, 1897.
OBSERVATORY MOON ATLAS.
Date.
Nbgativk
TAKEN ON
Moons Age.
h. m. s. s.
I
1895, October 10,
16 49 10 — 17
22 days, 16 hours.
2
1895. ** 9.
165530 —40
21 *
* 16 *•
3
1895. " 8.
15 9 10 — 20
20
* 14 "
4
1895, " 9,
16 53 2 — 12
21
' 16 »*
5
1896, *' 18.
10 32 41 —47
12
* 8 **
6
1897, April 9,
9 8 21.5 — 285
8 *
i J .«
7
1895, October 7,
13 6 20 — 28
19 *
« 12 **
8
1895, " 8.
15 6 8 —18
20
* 14 **
9
1896, June 17,
942 —10
6 •
* 20 •*
10
1895, October 7,
12 57 18 — 24
19 '
i 12 *'
II
1895. " 8.
15 3 10 — 20
20 '
• 14 •*
12
1897, April 9,
8 55 25.5 — 315
8 *
i J i.
13
1896, October 18,
10 40 19 — 23
12 '
8 '*
14
1896, July 26,
12 59 25 — 33
16 •
* 13 **
15
1896, August 20,
11 57465 — 50.5
12 *
3 "
16
1896, July 26,
13 8 55 — 63
16 '
* 14 **
17
1897, April 13,
9 35 56.5 — 61.5
12 *
. I **
18
1897, *' 13.
9 42 29.5 — 35.5
12 '
1 J «(
1895, Aug:ust 30,
*% » *
10 *
* 16 **
19
9 *4
Albert Marth; born 1828, died 1897.
The death of Albert Marth, in September, 1897, takes
away the last astronomer who was a pupil of Bessel. Marth
was born in Colberg, May 5, 1828, and studied at the Universities
of Berlin and Koenigsberg. His first official position was that of
astronomical observer at the University of Durham. He was the
assistant of Mr. Bishop at Regent's Park and of Mr. Lassell
Astronomical Society of the Pacific. 203
in his Malta Expedition, and latterly the astronomer of Colonel
Cooper's Observatory at Markree. His published writings are in
many fields of astronomy, both theoretical and practical, though
his forte was calculation rather than observation. The asteroid
Amphitriie was discovered by him, as well as a long list of faint
nebulae at Malta. We owe to him calculations of the orbits of
many comets and asteroids. The orbits of satellites he took in
his especial charge, and for more than thirty years he provided
observers with ephemerides of these bodies, as well as with
ephemerides for the physical observation of the planets and the
Moon for a great part of this time. These ephemerides, regularly
issued on a uniform plan, have been of the greatest service to
astronomy. They encouraged the observation of satellites and
planets, and compelled a comparison of the results with theory.
Marth's writings on Theoretical Astronomy (theory of the
motions of satellites, Kepler's problem, orbits of binary stars,
etc.). and on Practical Astronomy (Theory of instruments, Divi-
sion Errors, Flexure, etc.) have been useful. His criticism of
the methods of reduction of the Greenwich observations was
well founded in several respects; but it naturally made him
no friends in official circles. He was a most useful aid to
Mr. Lassell, whose great talents lay rather in mechanics than
in the making and reduction of astronomical observations. ' The
Malta Expedition was a memorable event, and will remain a
lasting credit to England and to Lassell and his assistant,
Marth. Edward S. Holden.
Resignation of Mr. Colton.
On August 18, 1897, Mr. Colton, Assistant Astronomer in
the Lick Observatory, tendered his resignation, after a service of
a little over five years. E. S. H.
A New Celestial Atlas.
Atlas der Himmelskunde. — Atlas of Astronomy, based on
celestial photographs — with sixty-two plates containing 135
single astronomical objects, and text containing about 500
illustrations — by A. voN Schweiger-Lerchenfeld. Pub-
lished by A. Hartleben, Vienna, in thirty parts (issued
twice a month), at one German Mark ($0.25) per part.
On page 145 of the present volume, a notice of Baron von
Schweiger-Lerchenfeld's Celestial Atlas was printed under
/
204 Publications of the
an erroneous heading. The description given above is the correct
one, and it will be seen that the price of the Atlas is about $7.50
only. Some fourteen parts have already been issued, and the
rest are nearly ready for publication. E. S. H.
September 16, 1897.
Portraits of Astronomers and Others Belonging to
THE Lick Observatory.
The following names should be added to the list given on
page 95, to- wit: —
Caswell, A. Michie-Smith, C. Saegmiiller, G. M.
Edwards, G. C. Mitchell, O. M. Saxton. J. G.
Eichbaum, H. Peirce, C. S. Schumacher, H. C.
Faye, H. Porter, J. G. Stone, E. J.
Gibbes, L. R. Rogers, W. B. Thaw, A. B.
Jarboe, J. R.
Astronomical Society of the Pacific. 205
Minutes of a Special Meeting of the Board of Direc-
tors OF THE Astronomical Society of the Pacific,
held in the Rooms of the Society, on Satur-
day, August 14, 1897, at 2:00 p.m.
President Alvord presided. A quorum was present. The minutes
of the last meeting were approved.
The Bruce (Gold) Medal of the Astronomical Society of
the Pacific.
Mr. HoLDEN presented to the Board of Directors a communication
firom Miss Catherine Wolfe Bruce, of New York City, as follows:—
810 Fifth Avbnub, New York City, May 15, 1897.
To the Directors of the Astronomical Society of the Pacific : —
Gbktlembn: — It is my desire to found and endow a gold medal to be awarded by
the Astronomical Society of the Pacific, not oftener than annually, for distinguished
services to Astronomy. 1 desire that the medal shall be international in character, and
that persons of any country and of either sex may be eligible to receive it. I have taken
the counsel of competent advisers in the preparation of the accompanying statutes for
the bestowal of the medal. If your Board of Directors will undertake the administration
of the Trust, I shall be glad to turn over to your Treasurer the sum of I2750, which I
onderstand will be sufficient to carry it out. It is my hope, with your co-operation, to
establish a foundation which shall be useful to Astronomy now and always.
I am, Gentlemen,
Very respectfully and sincerely yours,
Catherine Wolfe Brucb.
This letter was accompanied by the statutes for the bestowal of the
Bruce Medal of the Astronomical Society of ihe Pacific, as printed in
the Publications^ No. 57.
After reading the foregoing, it was on motion.
Resolved^ That the Board of Directors of the Astronomical Society of the Pacific,
in its own behalf, and on behalf of the Society, accepts with gratitude Miss Krucb's
generous giA which, in connection with her many previous benefactions to the Astronomy
of America and Europe, will forever connect her name with the history of the Science.
Resolved^ That the conditions of the gift as expressed in the Statutes for the
bestowal of the Bruce Medal of the Astronomical Society of the Pacific are hereby
accepted by the Directors in their own behalf, and on behalf of the Society.
Resolved^ That the gift of Miss Bruce be divided into two portions, namely: I2500,
which constitutes the Bruce Medal Fund; and the residue, which is hereby placed at the
disposal of a Special Committee,* to consist of Messrs. Holdbn, St. Johk and Ziel,
who are authorized to procure the necessary dies and to strike off one gold medal and
nine bronze replicas. The gold medal is to serve for the first award; the bronze replicas
arc to be sent by the Secretaries of the Society as follows:—
The first to Miss Bruce ;
One to the Astronomical Society of the Pacific ;
One to the Smithsonian Institution ;
One to the Harvard College Observatory;
One to the Lick Observatory;
One to the Yerkes Observatory;
One to the Observatory of Paris ;
One to the Observatory of Greenwich ;
One to the Observatory of Berlin.
*The Committee suggested, consisted of Messrs. Alvord, Holden and Zieu
Mr. Alvord requested that his name be withdrawn and the name of Mr. St. John be
substituted in his stead, which was accordingly done.
2o6 Publications of the
The Treasurer is authorized to advance from the General Fund, whatever may be
necessary to carry out the foregoing:; all advances to be subsequently repaid from the
interest on the Brucu Medal Fund.
Resolved^ That the Bruce Medal Fund be placed under the immediate care of the
Finance Committee, which Committee shall, through the Treasurer, annually print a
separate account of this fund.
Resolved^ That the By-laws of the Society, the Statutes for the bestowal of the
Brucb Medal, and the Rules relating to the Comet Medal, be printed in an extra number
of the Publications t in an edition of 1500 copies.
In order to insure the prompt printing of the Publicatiofis^ it was
Resolved^ That the Committee on Publication is formally authorized to postpone the
printing of any manuscript received later than ten days before the stated dates of
issue of the regular numbers (namely: February i, April i, June i, August i, October i,
December i) when necessar>'.
The following members were duly elected:
List of Members Elected August 14, 1897.*
Miss Kate Ames Napa, Cal.
Mr. Walter C. Baker } '"^Ohia"''"'* ^''^" ^'^''^'^°'**
Mr. Charles R. Bishop Occidental Hotel, S. F.. Cal.
Mr. E. F. Coddington | Lick Observatory. Mt. Hamilton.
Mr. HENRV EiCHBAUM } ^ ^I^f 'vi^^h^^^^^^^^^^^
Mr. James Monroe GoEWEY . . . . Page and LagunaSts.. S. F.. Cal.
Mr. Charles C. Keeney* 2220 Clay St., S. F., Cal.
Mr. JOH. W. KHNOK,CK }%^otl^^St^M^nL5olirM?nt
Free Public Library Worcester. Mass.
(Puruatanga, Martinborough,
Wairarapa, Wellington, New
Zealand.
colonel C. McC. Rhbvh } ^^pou"" S' ''• ""■' '""""
Mr. Thos. VV. Stanford* {'"foria.^^" ^^" '^^"'°'"'"^' ^•''"
Secretary Perrine reported that sundry articles of bedding, etc.
(see Publications A. S. P., No. 54, page 49), had been disposed of for
the sum of twelve dollars. His report was accepted and filed.
Adjourned.
Meeting of the Board of Directors and of the
Society, September 4, 1897.
Saturday, September 4th. was the date for a regular meeting of the
Directors and of the Society at Mt. Hamilton. As no quorum for the
transaction of business (in either body) was present, no meetings were
held. The papers presented for reading will be printed in the Publica-
iions in due course.
•A star signifies Life Membership.
Astronomical Society of the Pacific. 207
Minutes of a Special Meeting of the Board of Direc-
tors OF the Astronomical Society of the Pacific;
HELD ON Saturday, September i8th, at 1:30 p.m.
President Alvord presided. A quorum was present. The minutes
of the last meeting were approved.
The following members were duly elected:
List of Members Elected September 18, 1897.*
Mr. John Bermingham* 330 Market St., S. F., Cal.
Mr. Thomas B. Bishop* 532 Market St., S. F., Cal.
Mr. George Crocker* Mills Building, New York, N. Y.
Mr. William H. Crocker* .... { ^ Bank^S^p!!^ CaL^ ^^^^"""^^
Mr. H. Dutard* 2616 Buchanan St., S. P., Cal.
Mr. Russell J. Wilson* 2027 California St., S. P., Cal.
Library of St. Gertrude's Academy. Rio Vista, Cal.
Adjourned.
* A star signifies Life Membership.
2o8 Publications of the Astronomical Society &c.
OFFICERS OF THE SOCIETY.
Mr. William Alvord Presidrmt
Mr. Edward S. Holdbn First Vice-Prtsident
Mr. Frbdbkick H. Sbarbs Second Vice-PresMdemt
Mr. Chauncbv M. St. John Third Vice-Prerident
ii;:R-£i:ir"-| ^'-"^
Mr. F. R. ZiBL Treasurer
Board of Directors- Mc^n. Alvoro, Holden, Molbra. Morsb, Miss O'Halloban,
Messrs. Pbkrinr, Pibrson, Sbarbs. St. John, von Gbloern, Ziel.
Finance Committee— iAcssn. William M. Pibrson, E. J. Molbra, and C. .VI. St. John.
Committee on Publication — Messrs. Holdbn. Babcock, Aitkbn.
Library Committee— l\^isx%. Hussbv and Sbarbs and Miss O'Halloran.
Committee on the Comet-Medal — Messrs. Holdbn (ex'officio)t Schabbbrlb, Campbbll.
OFFICERS OF THE CHICAGO SECTION.
Executive Committee— Uix. Ruthvbn W. Pikb.
OFFICERS OF THE MEXICAN SECTION.
Executive Committee— 'M., Francisco Rodrigubz Rbv.
NOTICE.
The attention of new members is called to Article VIII of the By-Laws, which provides that
the annual subscription, paid on election, covers the calendar year only. Subsequent annual
payments are due on January ist of each succeeding calendar year. This rule is necessary in
order to make our book-keeping as simple as possible. Dues sent by mail should be directed to
Astronomical Society of the Pacific S19 Market Street, San Francisco.
It is intended that each member of the Society shall receive a copy of each one of the PnS^
lications for the year in which he was elected to membership and for all subsequent years. If
there have been (unfortunately) any omissions in this matter, it is requested that the Secretaries
he at once notified, in order that the missing numbers may be supplied. Members are requested
to preserve the copies of the Publications of the Society as sent to them. Once each year a title-
page and contents of the preceding numbers will also be sent to the members, who can then bind
the numbers together into a volume. Complete volumes for past years will also be supplied, to
members onlv. so far as the stock in hand is sufficient, on the payment of two dollars per volume
to either of the Secretaries. Any non-resident member within the United States can obtain
books from the Society's library by sending his library card with ten cents in stamps to the
Secretary A. S. P., 819 Market Street, San Francisco, who will return the book and the card.
The Committee on Publication desires to say that the order in which papers are printed in
the Publications is decided simply by convenience. In a general way, those papers are printed
first which are earliest accepiecl for publication. It is not possible to send proof sheets of papers
to be printed to authors whose residence is not within the United States. The responsibility for
the views expressed in the papers printed rests with the writers, and is not assumed by the
Society itself.
The titles of papers for reading should be communicated to either of the Secretaries as early
as possible, as well as any changes in addresses. The Secretary in San Francisco will send to
any member of the Society suitable stationery, stamped with the seal of the Society, at cost price,
as follows: a block of letter paper, 40 cents; of note paper, 25 cents; a package of envelopes. 25
cents. These prices include postage, and should be remitted by money-order or in U. S. postage
stamps. The sendings are at the risk of the member.
Those members who propose to attend the meetings at Mount Hamilton during the summer
should communicate with "The Secretary Astronomical Society of the Pacific " at the rooms fk
the Society, 810 Market Street. San Francisco, in order that arrangements may be made for
transportation, lodging, etc.
PUBLICATIONS ISSUED BIMONTHLY.
( February f April, June, Aug-ust, October, December.)
^ORl
T^''=:v,^-'-
PUB LI CAT I O N S
AstroaomiGal Society of thpiiOTfeSwa
...■■■■'. m SU£ HBRA RV
Vol. IX. ' San Francisco, Cal.,. December i, ] 897. "No. 59.
M TOW , LbWOX A^ in
hm
TILDEN FOt/NC- \' J .^
THE YERKES OBSERVATORY.
By William j. Hussbv.
The Yerkes Observatory has been dedicated, and its active
exbtence as a, scientific institution commenced. On the 21st of
October, within the great dome, and. in the presence of a large
assemblage, the donor, Mr. Charles T. Yerkes, formally pre-
M»ced: the observatory and its great telescope to the University
of Chicago; and they were formally accepted for that institution
by Mr. Marti Jl A. Ryerson, the President of the Board of
Trustees.
The dedication of thfe observatory is an important scientific
event of the year, inaugurating, as it does^ the work of a great
institution devoted to the discovery and teaching of scientific
truth, and forming an epoch '. in its history by separating the
period of construction, which has extended over the past five
years, from the period of its scientific activity, which is just
beginnii^.. The dedication was made the occasion of a large
gathering of : astronomers and scientific men, and a series of
conferences on astronomical and astrophysical subjects, with
discussions and laboratory demonstrations of new and interesting
phenomena, was held at the observatory during the three days
preceding the formal exercises. These exercises were held in
the great dome of the observatory on October 21st, and were
continued in Chicago the following day. The leading address
at the observatory was by Professor James E. Keeler, on ** The
Importance of Astrophysical Research and the Relation of Astro-
physics to other Physical Sciences.*' Other addresses were
made at this time, by Mr. Yerkes, in presenting the observatory
2IO Publications of the
to the university; by Mr. Ryerson, in behalf of the l^oard of
Trustees in accepting it, and by President Harper, in b-half of
the faculty. In Chicago, Professors Michelson and Str atton
gave brilliant demonstrations with new forms of physki v r. tus.
having possible applications to the solution of cert; ■ . mintf
problems of astronomy. In the afternoon, Professor NeW( omb
delivered his address at Kent Theater, on * 'Aspects of American
Astronomy,** and that evening, in conclusion, Mr. Yerkes pro-
vided a banquet for the visiting scientists.
The Kenwood Observatory and the Yerkes Observatory are
so related, that an account of the latter would be incomplete
without some mention of the former, and in historical order the
former comes first.
The Kenwood Astrophysical Observatory had its beginning in
a spectroscopic laboratory, which Professor George E. Hale
erected in Chicago in the spring of 1888. In the winter of
1890-91, extensive additions were made to this, converting it
into an observatory proper, with an equipment designed especially
for the study of solar phenomena by spectroscopic and photo-
graphic methods. The observatory was provided with an equa-
torial telescope of 12.2 inches aperture. The mounting, which
was made by Messrs. Warner & Swasev, was large and heavy,
and was designed to carry a very large spectroscope. The
objective and the spectroscope were made by Mr. Brashear.
In connection with the observatory a workshop was fitted up,
supplied with such machinery and tools as were necessary for the
construction, repair, and modification of apparatus.
Professor Hale was not long in obtaining important results
with his new equipment. Early in April, 1891, soon after the tele-
scope had been set up, he succeeded in photographing the spectra
of the solar chromosphere and prominences for the first time with-
out an eclipse. Within a year or two, he had discovered new lines
in the spectra of the prominences, spots, and faculae; had obtained
photographs of the prominences with the H and K lines and an
open slit; had matured his invention of the spectroheliograph and
had one constructed by Mr. Brashear, and by its use had
secured photographs of all the prominences visible around the
entire circumference of the Sun at a single exposure, and then,
by a second exposure, had obtained on the same plate the forms
of the regions on the Sun*s disk, even in its brightest parts, over
which the H and K lines are reversed, and had shown that these
Astronomical Society of the Pacific. 211
forms are identical with the forms of the faculse obtained by photo-
graphs taken in the ordinary way.
At the time of its opening, in the fall of 1892, the University
of Chicago was entirely without facilities for research in astronomy
and astrophysics. Through the care of Professor Hale and
others, the matter received the immediate attention of President
Harper and the Board of Trustees, and in a very short time they
had obtained from Mr. Yerkes an expression of his willingness
to defray the entire cost of a large telescope.
Some years previously a large telescope was planned for the
University of Southern California. Large disks of glass for the
objective of this instrument were ordered from Mantois, of
Paris, and, when they were made, were forwarded to the
opticians, Messrs. Alvan Clark & Sons, Cambridgeport, Mass.
This is as far as the matter went. The order to finish the objec-
tive never came. In 1892 these disks still remained in the shops
of the opticians, and were then for sale. When Mr. Yerkes
was informed that these large disks of excellent glass could be
obtained immediately, he authorized their purchase for the Uni-
versity of Chicago, and entered into a contract with Messrs.
Alvan Clark & Sons for finishing an objective from them. He
also made a contract with Messrs. Warner & Swasey for an
equatorial mounting for the telescope that bears his name. It
thus came about that, within a few weeks from the time his gift
was announced, the orders for the objective and for the mounting
had been given. Mr. Yerkes then wrote to President Harper:
'* I have felt it proper that the telescope should have a home, to
be paid for by me ; and I have concluded to add to my gift an
observatory necessary to contain the instrument.*'
A site for the new observatory was not selected immediately.
Professor Hale was chosen Director, and the equipment of the
Kenwood Observatory was presented to the University of Chicago,
to become a part of the Yerkes Observator)\ It appeared to
Professor Hale that the exceptional instrumental advantages of
the new observatory should not be wasted by a mere duplication
of the work done equally well elsewhere, and that the large
telescope should not be employed in the observation of objects
within easy reach of smaller instruments. Notwithstanding the
number of observatories that had been established in various parts
of the world, and the importance of the subject, comparatively
little attention was being devoted to the phenomena presented by
212 Publications of the
the Sun. He accordingly outlined a plan of work, in which the
study of solar phenomena in all phases, and on a more extended
scale than had been possible with the equipment of the Kenwood
Observatory, formed an important part.
The great size of the telescope, its light-grasping power, and
long focal length make it especially suitable for the measurement
of faint and difficult objects, for the study of planetary markings,
and for the spectroscopic observ«ition of the stars. These con-
siderations led to the inclusion in the plan of work of micrometric
observation of difficult double stars, nebulae, planets, satellites,
comets, and stellar spectroscopy. Stellar and nebular photog-
raphy, meridian observations, and various kinds of laboratory
work of an astrophysical character were also included in the plan.
Professor Hale next considered the requirements of the
various kinds of work intended to be pursued as dependent upon
the quality of the seeing, the transparency of the atmosphere,
the blackness of the sky, and the steadiness of the instrument
used. After a study of the requirements, he wrote as follows
concerning the selection of the site: ** It is evident that in
these various classes of work, the greater part do not require
very good seeing; but on account of the importance of the
double -star observations, and those of planets, satellites, the
structure of the photosphere, etc., it was eminently desirable
to choose a site at which the seeing would be the best
attainable by night and by day. Some of the other
researches demand a dark sky and great transparency of the
atmosphere, while for still others the principal requisite is com-
plete protection of the instruments from vibration of any kind.
If there had been absolute freedom of choice, a site combining
the excellent conditions for night work enjoyed at Mt. Hamilton
with the good day seeing existing elsewhere would have been
sought far and wide, without regard to geographical boundaries."
From a consideration of the plan of work, and the conditions
necessary for the most successful prosecution of certain lines of
it, it was at once apparent that Chicago, or any place in its
immediate vicinity, would be an unsuitable location for the
observatory. When this became generally known, numerous
offers of land and other inducements to secure the observatory
were made by individuals and by towns in various parts of the
country. A practical consideration of no small weight in determin-
ing the location of the observatory was, that its value as a depart-
Astronomical Society of the Pacific. 213
ment of the university should not be materially affected. This
required that it be located within a reasonable distance of Chicago,
preferably within a hundred miles.
A committee of the Board of Trustees was appointed to select
a site. After visiting the most promising places proposed, this
committee reported in favor of accepting a tract of land offered
by Mr. John Johnson, Jr., of Chicago, situated on the northern
shore, near the western end of Lake Geneva, in Southern Wis-
consin. In speaking of this tract of land in its report, the com-
mittee says: ** It is conceded by all concerned that no site thus
fer suggested combines in itself so many requirements, or any of
the requirements, to so great a degree. The site is high and
beautifully located. The atmosphere is clear, without danger of
encroachments of manufactories, railroads, or electric lights.'*
The Board of Trustees adopted the report of the committee, and
the observatory has been built on the land given by Mr. Johnson.
This tract contains 53 acres. The observatory stands in the
midst of it. The center of motion of the great telescope is about
240 feet above the level of Lake Geneva, and about 1800 feet from
its shore. The elevation of the site above sea level is about 1200
feet It is 38 miles from Lake Michigan, and about 75 miles from
Chicago. The nearest town is Williams Bay, about a mile
distant This is the terminus of a branch of the Chicago and
Northwestern Railway. Lake Geneva, seven miles away, is the
nearest town having electric lights. The country round about is
woodland and cultivated fields, a beautiful region, already a favorite
summer- residence place for people of Chicago.
When the lines of work to be pursued by the new observatory
had been decided upon, and a site selected which, all requirements
considered, promised to be the best, the next problem that con-
Cronted Professor Hale was, the plan of an observatory building
suited to the scientific requirements and to its environment. To
plan such a building was not an easy task. The new observatory
was not to be one engaged predominantly with the astronomy of
position, nor was it to be merely a spectroscopic laboratory.
It was to combine both these lines of work on an extensive scale,
and besides to be prepared to meet the needs of such other
departments of research as might arise.
The subject was one of such importance that Professor Hale
visited and studied the most important observatories and spectro-
scopic laboratories of the United States and Europe in search of
214 Publications of the
ideas to enable him to formulate plans embodying the results of
experience and meeting the scientific requirements in the most
satisfactory manner. The preliminary plans were completed in
Berlin in February, 1894, and forwarded to the university
architect, Mr. Henry Ives Cobb, of Chicago. During the
following year, Mr. Cobb worked out the details of the plan
with great care, and without sacrificing architectural eflfect he
conserved the scientific requirements. The plans were finally
completed in February, 1895, and the work of construction,
beginning in April of that year, has since gone on, with some
interruptions, until the recent completion of the observatory.
The style of architecture adopted for the main building is
Romanesque, with somewhat Saracenic details. The foundation
is concrete, and the constructive materials are brown Roman
brick with terra-cotta ornaments of the same color. The parti-
tions are of hollow tile, the floors and roof are supported by steel
I-beams. The roof is of tile, the floor of the main hall is marble
mosaic, and those of the offices and laboratories are maple.
The doors and woodwork throughout the building are of antique
oak. The form of the building is that of the Latin cross, with
the longer axis (326 feet long) lying in an east and west direc-
tion, having the tower for the great dome (92 feet in diameter)
at the western extremity, and the room for the meridian-circle
(28 by 25 feet) at the eastern extremity. For the present, a
transit instrument will be used in this room, but it is intended
that this shall give place after a time to a large meridian circle.
Towers also rise at the ends of the shorter axis of the cross.
The northeast tower carries the dome (26 feet in diameter),
which was formerly a part of the Kenwood Observatory, and the
southeast tower is surmounted by a dome 30 feet in diameter.
The 12.2-inch telescope of the Kenwood Observatory is now
mounted in the northeast dome. A 24- inch reflecting telescope
for stellar spectrographic work is being constructed for use in the
southeast dome.
The main entrances to the observatory are on the north and
south sides of the building. They are exacdy alike, and both lead
to the central rotunda. A long hall divides the building centrally
lengthwise The rooms of the main floor have their entrances
into this hall or into the rotunda. The rooms on this floor are
those designed for offices, computing, reception, and lecture rooms,
library, chemical and spectroscopic laboratories, and those for
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Astronomical Society of the Pacific. 215
instruments and storage. The ground floor or basement affords
space at the western end for photographic dark rooms and enlarg-
ing room, emulsion room, constant temperature room (including
space for clocks), physical laboratory, and concave grating room;
and at the eastern end for optical, instrument, and pattern shops.
The attic between the two small towers is 104 feet long and
12 feet wide. It is fitted up as a heliostat room. A portion of
the roof near the northeast dome is mounted on wheels which run
on steel rails. By a windlass this portion of the roof can be
drawn to the southward far enough to allow the Sun's rays, at all
seasons of the year, to fall upon a heliostat placed near the north-
em end of the room. A heliostat having a mirror of 24 inches
aperture is being made in the shops of the observatory. The
large attic rooms along the main axis of the building are so
arranged that they can be used in conjunction with the heliostat
room for the use of apparatus having lenses or mirrors of great
focal length.
The spectroscopic laboratories have solid brick piers on con-
crete foundations. These are sp arranged, with reference to the
doors and windows, that the instruments mounted upon them can
be used in conjunction with each other, or with instruments in
the open air. One of these laboratories is especially arranged for
bolometric work. The apparatus for these laboratories includes
spectroscopes of various kinds, bolometers, galvanometers, inter-
ferential refractometers, induction coils, and a variety of subsidiary
apparatus.
The concave grating room is designed to contain a concave
grating of 21 feet radius, mounted in the usual manner. At pres-
ent there are mounted here a 4-inch grating of 10 feet focus and
a smaller one of 6 feet focus, both from the Kenwood Observa-
tory. The physical laboratory adjoins the concave grating room,
and the latter is so arranged that it can be used in conjunction
with apparatus in the former. Both are provided with rolling
wooden shutters so that the light can be effectually excluded.
At the Kenwood Observatory, Professor Hale found that
many of the problems with which he had to deal, involving, as
they did, new methods of research, required the construction of
instruments of new and special design. While the principal
instruments used there were obtained from Brashear and from
Warner & Swasey, it was found necessary to have a work-
shop in which nearly the entire time of an instrument maker was
2i6 Publications of the
employed in constructing pieces of apparatus required in the
solar and spectroscopic work. This shop proved so indispens-
able to the Kenwood Observatory that it was decided to provide
the Yerkes Observatory with the best facilities for mechanical and
optical work. A room, 1 8 by 54 feet, for metal working, was
selected on the ground floor of the observatory in the southeast
quarter of the building, with smaller adjacent rooms to the east
fitted up as a forge room and a pattern shop.
The machine tools used at Chicago were an engine lathe, a
shaper, a small speed lathe, an 8-inch Rivett ** Precision '* lathe,
and a Brown & Sharpe universal milling machine. These have
been transferred to the new shops, and a planer, a drill press, a
circular saw, and speed lathes added.
Two mechanicians are regularly employed in this shop. Sev-
eral important machines and various pieces of apparatus are in
process of construction. A friend of science in Chicago has pro-
vided the means of employing a third mechanician for the express
purpose of constructing a machine for ruling gratings, according
to plans by Professor Wadsworth.
The optical shop (20 by 70 feet), with rooms fitted up for grind-
ing, polishing and testing lenses and mirrors, is on the north side
of the building, just across the hall from the machine shop. The
walls of these rooms and the double windows are so constructed
as to maintain a nearly constant temperature, a condition neces-
sary for the most successful conduct of the work. Some large
pieces of optical work have already been completed in this shop,
and still more important ones are planned. A large grinding
machine has been constructed under the direction of the observa-
tory optician, Mr. G. W. Ritchey, for the purpose of grinding
and polishing a 60-inch mirror, to be used for stellar spectroscopic
work. The work of rough grinding has already been undertaken.
The 40- inch telescope, with its dome and elevating floor, are
the principal attractions of the Yerkes Observatory, viewed
from a popular standpoint. These are the largest in the world.
The dome is 90 feet in diameter, 60 feet high above the top of
the tower upon which it rests, or 1 12 feet above the ground. Its
framework is of steel, riveted together. This is covered, first,
with a sheathing of wood, and next with roofing tin. It is
supported upon 36 wheels, each 36 inches in diameter, and is
turned by an endless cable which passes around the dome and
is connected with the driving mechanism. The cable is driven
s \^^.
Astronomical Society of the Pacific. 217
by an electric motor, controlled by a switch on the observing
floor. Provision is also made for revolving the dome by hand.
The wheels upon which the dome revolves have journals with
roller bearings for relieving the friction, and are so constructed
as to adjust themselves to possible inequalities of the track.
The observing slit is 13 feet wide, and extends from the hori-
zon to a point 5 feet beyond the zenith. The shutters covering
this opening are arranged to open simultaneously on either side,
and remain parallel in all positions. Adjustable canvas curtains
are placed within the opening to protect the telescope, in whatever
direction it may be pointed, from the wind.
It is of interest to compare this dome with the one the next
largest; namely, that of the Lick Observatory. The large dome
at Mt Hamilton has an outside diameter of 74 feet 4 inches,
and an inside diameter of 71 feet, and weighs, including shutters
and live ring, 99^ tons. The live ring itself weighs 12^ tons.
This dome rises 41 feet 8 inches above the top of the supporting
tower, and 76 feet 10 inches above the ground. The dome is
supported on a live ring consisting of 21 conical rollers, each
roller having three wheels. The base plate of the dome rests on
the central wheel of each group, while the outside wheels rest
upon the lower track. The two rails of this track are a part of
a conical surface with its apex in the vertical axis of the dome,
and in the plane with the tops of the rollers. The upper track is a
plane surface. The outside wheels of the live ring are 30 inches
in diameter, and the inside ones 28^ inches. The three wheels
of each roller were pressed on a steel spindle 3^ inches in
diameter, and the journals at the extremities of these spindles
are provided with roller bearings for avoiding sliding friction.
The framework of the dome is of steel construction, and it is
covered with galvanized steel plates.
The observing slit is 9 feet 6^ inches in the clear, and extends
from near the horizon to a point 3 J^ feet beyond the zenith. This
opening is closed with double shutters, hinged at a point beyond
the zenith, and supported on wheels resting on a track below.
These shutters open simultaneously, but do not remain parallel.
The dome is turned by a cable, operated by an hydraulic engine.
It may also be turned by hand.
The elevating floor of the Yerkes Observatory is 75 feet in
diameter, and rises through 22 feet. It is supported by wire
cables, 90° apart. These cables pass over large drums, and are
2l8
Publications of the
attached to coupterweights. Gearing connects the four df urns,
causing them to operate simultaneously. The floor is operated
by an electric motor, controlled by a switch on the floor. The
rising floor of the Lick Observatory was the first one installed.
It is 6 1 >^ feet in diameter, and rises through i6>^ feet It is
operated by hydraulic rams placed 90° apart, and is provided with
gearing to keep the floor level in all positions. This method of
operation was out of the question at the Yerkes Observatory on
account of the danger of the water in the rams freezing in the
severe winter weather at Lake Geneva. At Mt. Hamilton the
temperature is usually above 32° Fahrenheit, even in winter, and
there is seldom any danger from freezing. *
The objective of the Yerkes telescope is 40 inches in diameter,
and has a focal length of 62 feet. The crown lens is 2>^ inches
thick at the center, and Y^ inch at the edge, and weighs 200
pounds. The flint lens is about i j4 inches thick at the center,
and 2 inches at the edge, and weighs more than 300 pounds*
The two lenses are mounted 8^ inches apart, upon aluminum
bearings in a cast-iron cell. The total weight of the objective in
its cell is about 1600 pounds.
The objective was completed in September, 1895, arid tested
in the following month at the Clarks* factory at Cambridgeport,
Mass., by Professors Hale and Keeler. Professor KeeLer
acted as ** expert agent " in making the test, and in his report
he states: —
** The expanded star disk was round inside and outside of
the focus, uniformly illuminated, and free from wings or other
appendages. Good images at the focus were obtained of stars at
widely different altitudes near the meridian, the definition being,
• The following table is derived from the record of the minimum thermometer at the
Lick Observatory. It gives a summary of the lowest temperatures for the past six years.
The months considered are from November to March, inclusive, the five coldest months
of the year.
MIN. TEMP.
AV. MIN.
NUMBKR OF DAYS WHKN TBMPBRATURB FBLL BELOW
WINTER.
20°
25°
30°
32V
1891-92
+ 17°
+38°
3
5
32
^
92-93
33
37
9
3a
59
93-94
16
36
4
16
45
56
94-95
22
39
4
24
40
95-96
18
39
I
7
38
36
96-97
18
34
3
14
42
52
THKjrORTV-INCH VKKKICS TKLKSCOPK. MAY n. 1897.
THE NEWYORK
Astronomical Society of the Pacific, 219
in my opinion, with due allowance for atmospheric disturbance,
equal to that of the Lick telescope, while the brightness of the
image was, of course, considerably greater than with the latter
instrument The color correction of the 40-inch objective
is, according to my best recollection, almost precisely the same
as that of the Lick telescope.'*
The tube of the telescope is 60 feet long. It has a diameter
of 52 inches at the center, 42 inches at the objective, and 38
inches at the eye-end. It is made of sheet steel, increasing in
thickness from ^ inch at the ends to 7/3, at the center. It
weighs 6 tons, and is so designed that it is in perfect balance
when a spectroscope weighing half a ton is attached to the eye-end.
When the spectroscope is removed, as for micrometer work, the
balance is restored by clamping weights near the eye-end.
The polar and declination axes are of hard forged steel. The
former is 13)^ feet long, 15 inches in diameter at the upper
bearing, and 12 inches at the lower bearing, and weighs 3^^ tons.
The latter is 11^ feet long, 12 inches in diameter, and weighs
1 54 tons. The bearings of these axes are relieved by live rings
of steel rolls, to reduce the friction.
The telescope is supported by a cast-iron column, made in
sections, bolted together, and firmly anchored to a massive brick
pier resting on a concrete foundation. The equatorial head at
the top of the column is cast in a single piece, and rises 43 feet
above the lowest position of the moving floor. The column and
head together weigh 50 tons. An iron balcony surrounds the
head. It is accessible from the floor by means of a spiral stair-
way at the south side of the column. The driving clock is placed
within the column, and is accessible by this stairway. An electric
motor automatically winds the clock when the weight reaches a
point near the limit of its run.
The clamps and slow motions can be operated by an observer
at the eye-end, or by an assistant on the balcony. Rapid
motions are abo provided, as well as a complete system of electric
motions, clamps, and illumination. The accessories are a filar
micrometer by Warner & Swasey, a solar spectroscope and
spectroheliograph from designs by Professors Hale and Wads-
woRTH, and a stellar spectroscope designed and constructed by
Brashear.
The objective of the Lick telescope is 36 inches in diameter,
and has a focal length of 57 feet 10 inches. The crown
220 Publications of the
lens is 1.96 inches thick at the center and 0.60 inch at the
edge. The flint lens is 0.93 inch thick at the center and
1.65 inches at the edge. The two lenses are mounted about
6^ inches apart, and the total weight of the objective in its
cell is 532 pounds.
The tube is 52 feet long, 48 inches in diameter at the center
and 38 inches at the ends. It is constructed of sheet steel, ^Uh
inch thick at the center and diminishing to ^ inch at the ends.
The tube has an extension at the eye-end of smaller diameter.
This is nearly 3 feet long, and is arranged to carry the sleeve
for supporting spectroscopes, photographic apparatus, and the
draw tube for the micrometer. The weight of the tube and
attachments is 5.3 tons.
The polar and declination axes are of steel; the former
is 10 feet long, 12 inches in diameter, and weighs with
its attachments 2j^ tons; the latter is 10 feet long, 10 inches
in diameter, and weighs, with its attachments, 2 tons. The
total weight that moves when turning in declination is 7^
tons, and when moving in right ascension is 14)^ tons (28,847
pounds).
The iron columns and heads of the Lick and Yerkes telescopes
are similar in design. The head and attachments of the former
weigh 6^ tons, the column 19 tons, and the driving clock i ton,
and total weight of its stationary parts 26^ tons. The driving
clock is wound by a water motor.
In considering the great telescopes of the Yerkes and Lick
Observatories, the large increase in the dimensions and massive-
ness of the former, as compared with the latter, stands in striking
contrast with the comparatively small increase in the diameter
and focal length of the objective. The objectives differ only 4
inches in diameter and about 4 feet in focal length; the Yerkes
telescope weighs 75 tons, and the Lick telescope 41 tons; the
elevating floor of the former is 75 feet in diameter and weighs
37^4 tons, that of the latter is 6i)4 feet in diameter and weighs
26 tons; the dome of the former is 90 feet in diameter and
weighs 140 tons, while that of the latter is 75 feet in diameter
and weighs 99^ tons. The principal reason that the differ-
ences are so great is, that the Yerkes telescope has been
designed to carry an exceedingly long and heavy solar spectro-
scope, and other large instruments at the eye-end. This
Astronomical Society of the Pacific. 221
made it necessary to increase the height and massiveness of the
mounting, the distance through which the moving floor rises and
falls, and the available floor space beyond what would otherwise
have been ample.
Leaving out of account the question of absorption as depen-
dent upon the thickness of the lenses, the perfection with which
they are polished, and the quality of the glass of which they are
made, in so far as it affects transparency, the light gathering
power of the Yerkes telescope is to that of the next largest tele-
scope in the ratio of 100 to 81, or very nearly in the ratio of
5 to 4. This is a difference which, other things being equal, will
give it a great advantage over all other instruments in many
kinds of work. The magnitudes of the faintest stars visible in
the Yerkes and Lick telescopes are (neglecting absorption)
respectively 17.21 and 16.98*, or the difference is less than a
quarter of a magnitude. In defining power, as exemplified in
the separation of close double stars, the two instruments stand
in the ratio of 10 to 9; the theoretical limit of separation for the
former is o".i2 and that for the latter o". 13!. These limits
differ so little, and are in themselves so small, that in defining
power the one telescope has scarcely any advantage over the
other for the work here considered. Besides, the practical real-
ization of these limits, aside from the skill of the observer, will
depend almost entirely upon atmospheric conditions, particularly
upon the steadiness of images and the excellence of the
seeing.
The Yerkes Observatory is valued at about $400,000. The
large objective cost $66,000; the mounting, $55,000; the dome
and elevating floor, $45,000; the stellar spectroscope, $3000;
the building, power house, engines, dynamos, etc. , more than
$145,000. These were the gifts of Mr. Yerkes. Mr. John-
son's gift of land is valued at $50,000; Mr. W. E. Hale's gift
of the Kenwood Observatory, $30,000; Miss Bruce has given
$7000 for a 10- inch photographic telescope.
The Lick Observatory cost nearly $600,000. The objective
of the 36-inch telescope cost $50,000; the third lens (photo-
graphic corrector), 33 inches in diameter, $13,000; the mount-
•This assumes that the faintest star visible in a i-inch telescope is 9.2 magnitude.
fThis assumes, as usual, that the spurious disk of a star in a i2-centimeter telescope
is i" in diameter.
222
Publications of the
ing, $42,000; the elevating floor, $13,000; and the large dome,
$54,000.*
In his address at the dedication, President Harper, quoting
the Director, said: '*The policy of the Yerkes Observatory
will be: (i) To derive the greatest possible return from the
use of the great telescope. It is evident that special attention
should be given to micrometrical observations of stars, satel-
lites, comets, nebulae, etc.; solar investigations, both visual and
photographic; and spectroscopic researches on the nature of
the stars and their motion in the line of sight. (2) To
provide for the investigation of any phase of an astronomical or
related physical problem. Most American observatories are
unprovided with the instruments and laboratories necessary for
the interpretation of the phenomena constantly encountered in
spectroscopic observations of the heavenly bodies. Spectroscopic
laboratories, on the other hand, are not equipped to carfy their
investigations beyond the artificial boundaries of physics into the
realm of astronomy. It is hoped that the Yerkes Observatory
may ultimately be in a position to represent both the astronomical
and physical sides of astrophysical work, and at the same time
provide the best facilities for research work in astronomy of
position.'*
The illustrations accompanying this article are from The Astro-
physical Journal, They were obtained through the courtesy
of Professor Hale.
Lick Observatory, Mt. Hamilton, Cal,
November 23, 1897.
*At the present time the prices of telescopes of various sizes, without their domes
and buildings, are roughly as follows, varying much, of course, with the style of mount-
ing, the accessories provided, and the quality of the workmanship. The accessories
here included are micrometer, spectroscope, finder, and eye pieces.
DIAMETER OF
OBJECTIVE.
PRICE OF
lOBJECTIVE.
PRICE OF
MOUNTING.
ACCESSORIES.
TOTAL.
45 inches
|8o,ooo
$65,000
$4,000
$149,000
40 ••
66,000
55.000
4,000
125,000
56 "
40.000
40,000
4,000
84,000
30 "
25,000
30,000
3,500
58.500
24 ••
14.000
20,000
3.000
37.000
20 ••
9,000
9,000
2.500
ao,50o
16 "
4.500
6,500
2,500
13.500
12 "
2,000
4.500
2,000
8.500
Astronomical Society of the Pacific.
223
CATALOGUES NOS. Ill AND IV, OF NEBULA DIS-
COVERED AT THE LOWE OBSERVATORY,
ECHO MOUNTAIN, CALIFORNIA.
By
Dr. Lewis Swift, Director.
LIST in.
6
Date
OF 1
R. A.
Dbc.
Dkscription.
2
Discovery.
FOR 1900.
1897
h m 9
I
Aug.
10.
46 45
— 35 43
pB eeS E. with 132 & 200 looks like a
nebulous D Uranus, •
2
Sept.
4.
55
— 40 53 51
vF. vS. R.
3
Sept.
4.
1 9 45
— 33 II 33
eeF. S. eeE. a ray no ♦ near.
4
Sept.
4.
I 23 35
— 36 17 3
eeF. pS. R. vdif.
5
Sept,
4.
I 33 10
— 34 29 45
vF. S. R. eF. * near nf.
6
Sept.
6.
I 46 45
— 30 26 20
pB. eS. IE. like a D nebulous ♦ with 132
& 200. See No. i.
7
Sept.
6,
I 53 45
— 33 4644
eeeF. ps. R. 7"* ♦ in field nf. another
suspected.
8
Sept.
4,
260
— 33 29 40
vF. S. vE. one ♦ nr.
9
Sept.
5.
2 II
— 31 41 30
pB. pS. IE.
10
Sept.
6.
2 34 3
— 27 52 25
pB. CS. R. 8™ * pretty close p.
II
Sept,
5,
2 44 30
— 31 42 30
vF. pS. R. I" of 3.
12
Sept.
5,
2 44 32
— 3T 36 32
vF. pS. R. 2<» of 3.
13
Sept
5,
2 45 4
- 3' 36 32
pF. pS. IE. 3** of 3.
U
July
22,
20 19 10
— 31 II 37
eF. pS. IE. wide D ♦ near s.
15
July
25.
20 20 50
— 36 20 57
pB. vS. eE.
16
Aug.
29.
20 22
— 36 22 19
eeS. eE. in meridian.
17
Aug.
29.
20 24 30
— 33 50 57
pF. pS. IE.
18
Aug.
29.
20 36 50
— 30 II 30
vF. pS. R. 2Fst. nr nf point to it. i»» of 3.
J9
Aug.
29.
20 37 5
— 30 II 30
eeF. CS. eE. nr the p * of several in seg-
20
Aug.
29.
20 37 30
— 30 I 30
ment of a circle. 2** of 3.
eeeF. pS. vE. eeedif. 3** of 3.
21
July
9»
21 26 5
- 37 9 9
eF. .pS. R. an e wide D ♦ f 30*.
22
Aug.
31.
22 3 5
— 28 21 II
eeF. vS. vE. forms right angle 2vF close
stars.
23
Aug.
8,
22 36
— 45 19 15
pF. pL. R. F ♦ nr sf.
24
Sept.
4,
22 51 10
— 37 7 5
eeF. vS. eeeE. a ray almost a line, np of
1459 Index Cat. Barnard.
25
S^pt.
4,
22 52 20
— 36 35 2
vF. vS. R. sfof 2.
26
Sept.
4,
22 52 30
— 36 24
pB. pS. R. np of 2.
27
Aug.
8,
23 13 50
— 42 49 45
eeF. S. CE. f of 3. f 7599-
28
Aug.
8.
23 16 15
— 43 3 20
eeeF. pLR. io°»»nr s. ii°» ♦f. eeedif.
29
Aug.
8,
23 23 8
— 42 2
pB. pS. R. 9« * closes.
30
Aug.
8.
23 26 59
- 45 36 18
vF. vS. R. bet 2 st. 8« ♦ sp.
224
Publications of the
NOTES.
List No. I, of fifty nebulae discovered here, was published in
the Astronomical /oumat o( November 13, 1896. Lkt No. 2, of
twenty- five, was recently published in Mottihly Notices, and Pub-
lications A. S. P. The present list, as will be seen, consists of
southern nebulae exclusively. It k a field rich in nebulae, which
that mighty Nimrod, Sir William Herschel, who hunted the
sky over, could not reach. Several are quite bright, and a few
are interesting. I have examined Gales* ring nebula, R. A.
21* 53" lo', Decl. — 39° 53' 42", and find it an interesting one,
increasing the number now known to seven. It bears consider-
able resemblance to the one in Lyra, but is not as bright, nor
will it bear magnifying like that celebrated one, though it is too
far south for me to do justice to it. Numbers i and 6 are
singular specimens of nebulae, perhaps deserving of a new classifi-
cation. I have lately seen three, all looking exactly alike.
N. G. C. 1288 is considerably elongated in 0°. It is not
round, as Sir John Herschel says.
N. G. C. 1340 must be struck out It is identical with 1344,
as has been suspected. I examined the locality thoroughly for
1340, and I am certain that it does not exist. Some time I
intend to take up thk matter of doubtful nebulae.
I am glad I have at length found in Barnard* s field a
nebula his keen eye failed to see. See No. 24.
LIST IV.
6
Datk of
DiSCOVKRV.
R. A.
Dkc.
KOR 1900.
Description.
h m s
/
I
Sept. 23/97
II
— 39 52 20
eeeF. vL eE. close f 55. See note.
2
Oct. 3. *
54 30
— 34 51 32
pB. vS. R. 2 St nf. & 2 np.
3
Sept. 29, *•
I 5
— 46 31 38
vF. S. R. No B ♦ near. vF one f.
4
Sept. 29, *'
I 53 4
— 33 31 27
pB. vS. R. BM. lo™ ♦ V close sp.
5
Sept. 29. **
250
- 33 25
vF. vS. eE. nearly o^ F ♦ p.
6
Sept. 29, "
2 59 28
— 39 52 38
eF. pS. R. F D ♦ sf points to it.
7
Sept. 26, "
3 31
- 34 46 55
pB. S. eeeE. a straight hair-like line 90".
See note.
8
Sept. 29. "
4 8 45
— 33 7 51
eF. vS. R. BM. 10™ * close s.
9
Sept. 29, *•
4 16 30
— 31 41 42
eeF. pL. R.
10
Aug. 10, •'
19 53 30
- 38 47 38
vF. S. R. 8"* » f 90^ pof 2. same parallel.
II
Aug. 10, **
19 54
- 38 47 38
vF. S. R. 8"**^ fof 2.
12
July 8. *•
20
— 48 35 50
B. CE. vS. stellar, f of 2.
13
Sept. 23, *•
20 10 59
— 41 53 24
vF. CS. R. no B * near.
Astronomical Society of the Pacific. 225
: Datb of
^ Discovery.
R.A.
Dec.
FOR 1900.
Description.
h m s
e 1 »
14 Sept 16. **
20 24 25
— 36 39 15
vF. CS. R. several p B st s & f.
15 Sept. 17, *'
20 40 25
— 38 50 35
eeF. pS. R.
16 Sept 15, "
21 I 31
— 30 26 30
eeF. pS. R. F»nearf9o^
17 Sept 17, "
21 41
— 35 21 58
vF. vS. R.
18
Sept 17. "
21 42
— 35 27
vF. pL. R. Not 7130, or 7135. sp of 2.
19
Sept 17. •*
21 43 30
— 35 22 10
eeF. pL. R. 3 B st p =» a. nf of 2.
20
Sept 27, "
21 49 46
— 49 31 52
eeF. pS. R. in line with 2 9" St sf. 7"» *
field sf.
Ill
21 Sept. 23, •'
22 51 30
— 43 59 27
pB. S. R. mbM.
22 Oct 3, •*
23 27 45
— 45 35 40
vF. S. R. bet 2 St. 8" ♦ sf. & a 7™ ♦ sp.
23 Sept 23, •'
23 39 25
— 43 29 15
vF. eS. R. stellar.
24 'Sept 25, **
23 42 40
— 37 36 53
eeF. CS. R. in vacancy.
25 Sept 25, "
23 52 25
— 37 34 52
pB. CS. eE. I ♦ near sf.
NOTES.
The nebulae in this list, the fourth issued from this observatory,
bringing the total to 130, are, as will be seen, all southern
nebulae. They are, with few exceptions, very faint, though some
are bright enough to come under Herschel's Class I. That
these have not been previously found, shows that the southern
sky, including that portion within the reach of Sir William
Herschel and Lord Rosse, has not been as thoroughly
searched over as has been the northern.
No. i = G. C. 27; also, N. G. C. 55, b, with its associated
companion, a very remarkable nebula. I am at a loss what to
think of it, whether it is all one; the preceding half very bright,
very large, exceedingly elongated, the following half exceedingly
feint, equally as large, and still more elongated; or, whether they
are two distinct nebulae, one partly overlapping the other. If single,
it is curved ; if double, they are inclined to each other. I am inclined
to think they are two distinct nebulae, one reason being that the
brighter one ends sharply, which would hardly be the case if the
brighter merged into the fainter. The brighter was discovered
by DuNLOP, but I doubt if he could have seen the fainter. That
Sir John Herschel does not mark it with a sign, as he often
has done, meaning a very remarkable or even a remarkable
object, lends plausibility to the idea that the fainter was not
even seen by him. As, however, it has been illustrated, a refer-
ence to that would decide the matter at once.
226 Publications of the
No. 7. This, in one respect at least, is the most remarkable
nebula I have ever seen. I doubt if the entire heavens afford a
similar example. If the reader will cut off a short piece of fine,
bright brass wire, and hold it up sidewise to the sky, he will
form, by looking at it, a very correct idea of how it appeared to
me. The line was certainly nebulous. It must be a thin nebulous
disk seen exactly edgewise.
G. C. 383 does not exist, and must be struck out. Sir John
Herschel makes both 380 and 383 of equal brightness, and the
places given would place both well within my field of 31' in
diameter, power 132. I made a long and thorough search
for 383, and would have found it if there, had it been three
times fainter than 380, which is an easy object.
PLANETARY PHENOMENA FOR JANUARY AND
FEBRUARY, 1898.
By Professor Malcolm McNeill.
January.
Eclipses. 1898 is richer in eclipses than was 1897. There
will be six in all, divided equally between those of the Sun and
those of the Moon, and one of each will occur in January.
The first will be a partial eclipse of the Moon, and will occur
on January 7th. It will be visible in the eastern hemisphere and
in the eastern part of the United States, but the Moon will have
passed out of the Earth's shadow before moonrise in the
western part of the United States. The maximum obscuration
is less than one sixth of the Moon's diameter.
The second will be a total eclipse of the Sun on the morning
of January 2 2d. No part of it will be visible in the western
hemisphere. The line of totality begins in Central Africa, and
passes through the Indian Ocean, India, and China. The most
accessible part of the Earth for observations is India, and the
weather conditions are usually favorable at that time of the year.
A large number of expeditions from various parts of the world
will be sent to make observations. The duration of the eclipse
will be about two minutes.
Astronomical Society of the Pacific, 227
OccultaHons, The Moon will pass over the Pleiades, and a
considerable number of occultations may be seen from almost any
part of the United States on the evening of January 30th.
Mercury is an evening star at the beginning of the month,
setting not quite an hour after sunset. It rapidly approaches the
Sun, passes inferior conjunction on January 6th, and becomes a
morning star. By the middle of the month, it rises early enough
to be seen in the morning twilight, and it reaches its greatest
west elongation on the morning of January 29th, when it rises
nearly an hour and a half before sunrise.
Vemts is a morning star, quite near the Sun throughout the
month, and cannot be seen, except, possibly, for a few days at
the beginning. On January 31st it rises only a few minutes
before sunrise.
Mars is also a morning star, very close to Venus at the begin-
ning of the month, less than one degree west and north; but
instead of getting nearer the Sun, as Venus does, it moves away
from it, and at the end of the month it rises about an hour
before sunrise. Its distance from the Earth has begun to
diminish slightly, but not enough to cause much increase in
brightness.
Jupiter rises at about midnight on January ist, and two hours
earlier on January 31st. It is a little east and south of the third
magnitude star y Virginis, and moves eastward about one degree
until January 24th, when it begins to retrograde.
Saturn is a morning star, rising somewhat earlier than Mars
and Venus, It is in the constellation Scorpio, about six degrees
north of the red first magnitude star, Antares, and during the
month moves about three degrees eastward.
Uranus precedes Saturti about six degrees, and is about one
degree south of fi Scorpii, It is also moving eastward, but less
than half as fast as Saturn,
Neptune is in the eastern part of Taurtis.
February.
Mercury is a morning star throughout the month, and during
the first half of the month rises early enough to be seen in the
morning twilight, if the atmospheric conditions are good. It
makes a very near approach to Mars on February nth. Mercury
passing to the north of Mars at a distance of only one minute of
arc. The Sun will have risen for all parts of the United States
228 Publications of the
before the time of the nearest approach, but the planets will be
near enough to be seen together in a telescope with a moderately
large field of view, on the morning of that date before sunrise.
Ventis is a morning star at the beginning of the month, but
passes superior conjunction on the morning of February 15th,
and becomes an evening star. It does not, however, reach a
distance from the Sun sufficient for naked-eye observation until
some time after the end of February.
Mars is also a morning star, rising a little earlier than during
January. It is slowly approaching the Earth, but it is still
distant from us more than double the Earth's mean distance from
the Sun, and it will not be conspicuous until nearly the dose of
the year.
Jupiter is rising about two hours earlier than during the
corresponding time in January, and by the end of the month is
up in time for late evening observations. It moves westward
during the month about two degrees from a position east of the
third magnitude star, y Virgmis, to a position about the same
distance west. At the time of nearest approach, the star is a
little more than one degree north of the planet.
Saturn is still a morning star, but rises earlier at the end of
the month, shortly after one o'clock. It moves about two
degrees eastward in the constellation Scorpio^ and is north and
east of the red star Antares, the brightest star of the constellation.
The apparent outer minor axis of the ring is nearly half the
major axis, not far from the widest opening the rings can have.
Uranus precedes Saturn about nine degrees, and is about
one degree east and south of ^ Scorpiu Its motion during the
month is small, about half a degree eastward, until February 28th;
then it begins to retrograde.
Neptune is in the eastern part of Taurus, and remains above
the horizon until after midnight.
Explanation of the Tables.
The phases of the Moon are given in Pacific Standard time.
In the tables for Sun and planets, the second and third columns
give the Right Ascension and Declination for Greenwich noon.
The fifth column gives the local mean time for transit over the
Greenwich meridian. To find the local mean time of transit for
any other meridian, the time given in the table must be corrected
by adding or subtracting the change per day, multiplied by
Astronomical Society of the Pacific. 229
the fraction whose numerator is the longitude from Greenwich
in hours, and whose denominator is 24. This correction is
seldom much more than i". To find the standard time for the
phenomenon, correct the local mean time by adding the differ-
ence between standard and local time if the place is west of the
standard meridian, and subtracting if east The same rules apply
to the fourth and sixth columns, which give the local mean times
of rising and setting for the meridian of Greenwich. They are
roughly computed for Lat. 40°, with the noon Declination and
time of meridian transit, and are intended as only a rough guide.
They may be in error by a minute or two for the given latitude,
and for latitudes differing much from 40** they may be several
minutes out.
Phases of the Moon, P. S. T.
Full
Moon
i,
Jan. 7,
H. M.
4 24 P. M.
Last
Quarter,
Jan. 15,
7 44 A.M.
New
Moor
1,
Jan. 21,
II 25 p. M.
First
Quarter,
Jan. 29,
6 33 A. M.
The Sun.
R.
. A.
Declination.
Rises.
Transits.
Sets.
189a.
H.
M.
c
/
H. H.
H.
M.
H.
M.
Jan.
I.
18
49
— 22
59
7 27 A.M,
. 12
4 P.M.
4 41 P.M.
II.
19 32
— 21
46
7 26
12
8
4
50
21.
20
15
-19
50
7 22
12
12
5
2
31-
20
57
- 17
17
7 14 ■
12
14
5
H
Mercury.
Jan.
I.
19
35
— 20
r6
8 2 A.M.
12
50 P.M.
5
38 P.M.
II.
18
45
- 19 40
6 31
II
21 A.M.
4
rr
21.
18
36
— 20
51
5 48
10
33
3
18
31.
19
12
— 21
47
5 47
Venus.
10
29
3
It
Jan.
I.
r8
I
-23
27
6 41 A.M.
II
16 A.M.
3
51 P.M.
II.
18
56
-23
13
6 56
II
32
4
8
21.
19
50
— 21
49
7 4
II
46
4
28
31.
20
43
-19
19
7 8
Mars.
12
M.
4
52
Jan.
I.
17
58
-24
4
6 41 A.M.
II
13 A.M.
3
45 PM.
II.
18
31
-23
58
6 35
II
7
3
39
21.
19
4
-23
27
6 25
II
3
35
31.
19 37
— 22
29
6 15
10
54
3
33
230
Publications of the
1898. H. M.
Jan. I. 12 37
II. 12 39
21. 12 40
31- 12 40
Jan.
I. 16 24
II. 16 29
21. 16 32
31- 16 36
Jan. I. 15 59
II. 16 I
21. 16 2
31. 16 4
Jan. I. 5 19
II. 5 19
21. 5 17
31. 5 17
Jupiter,
Declination. Rises.
*» ' H. M.
— 2 32 12 2 A.M.
— 2 43 II 25 P.M.
— 2 47 10 47
— 2 43 10 7
Sa turn.
Transits.
H. M.
Sets.
H. M.
5 53 A.M.
5 16
4 38
3 58
II 44 A. M.
II 7
10 29
9 49
~ 19 53 4 51 A.M. 9 40 A.M. 2 29 P.M.
20 2 4 16
20 10 3 41
20 16 36
Uranus,
9 5
8 30
7 54
I 54
I 19
12 42
— 20 21 4 26 A.M. 9 14 A.M.
2 P.M.
20 27
20 32
20 36
3 50
3 13
2 35
8 37
8 o
7 22
I 24
12 47
12 9
Neptune,
+ 21 44 3 15 P.M.
+ 21 43 2 35
+ 21 42 I 55
+ 21 42 I 14
10 33 P.M. 5 51 A.M.
9 53 5 II
9 13 4 31
8 32 3 50
Eclipses of Jupiter's Satellites, P. S.
(Off left-hand limb, as seen in an inverting telescope.)
H. M. •
H.
M.
II, D, Jan.
2.
10 16 P. M.
II, D, Jan.
17.
3
26 A. M.
I.D,
3.
5 13 A.M.
I,D,
19.
3
27 A. M.
I,D,
4-
II 41 P. M.
I.D,
20.
9
55 P. M.
III, R,
7.
9 2 P. M.
III, D,
22.
2
10 A. M.
II, D,
10.
12 51 A. M.
III, R,
22.
4
56 A. M.
IV, D,
10.
12 51 A. M.
II, D,
24.
6
2 A. M.
IV, R,
10.
2 39 A. M.
I, D,
26.
5
20 A. M.
I, D,
12.
I 34 A.M.
IV, R.
26.
8
25 P. M.
III, D,
14.
10 12 P. M.
I, D,
27.
II
48 P. M.
III, R,
15.
12 59 A. M.
III, D,
29.
6
8 A.M.
Minima of Algol, P. S. T.
H. M.
H.
M.
Jan. 3.
7 43 A.M.
Jan. 20.
12
36 P. M.
6.
4 32 A.M.
23.
9
25 A. M.
9-
I 21 A. M.
26.
6
14 A. M.
II.
10 10 P. M.
29.
3
3 A. M.
14.
6 59 P. M.
31.
II
52 P. M.
17.
3 47 P.M.
Astronomical Society of the Pacific, 231
Phases of the Moon, P. S. T.
H. M.
Full Moon, Feb. 6, 10 24 a. m.
Last Quarter, Feb. 13, 4 35 p. m.
New Moon, Feb. 20, 11 41 a. m.
First Quarter, Feb. 28, 3 13 a. m.
The Sun.
R. A.
Declination.
Rises.
Transits.
Sets.
I89S.
H.
M.
'
H. M.
H. M.
H. M.
Feb.
I.
21
I
-17
7 13 A.M.
12 14 P.M.
5 I5P-M.
II.
21
41
- 13 55
7 2
12 14
5 26
21.
22
19
— 10 26
6 50
12 14
5 38
Mar.
3.
22
57
— 6 42
6 35
12 12
5 49
Mercury.
Feb.
I.
19
17
— 21 48
5 48 A.M.
10 30 A.M.
3 12 P.M.
II.
20
12
-20 57
6
10 45
3 30
21.
21
13
-18 I
6 10
II 7
4 4
Mar.
3-
22
18
-12 53
6 18
Venus,
II 33
4 48
Feb.
I.
20
48
- 19 I
7 8 A.M.
12 I P.M.
4 54 P.M.
II.
21
38
- 15 30
7 6
12 12
5 18
21.
22
27
— II 16
7
12 21
5 42
Mar.
3-
23
14
- 6 33
6 50
Mars,
12 28
6 6
Feb.
I.
19 40
— 22 22
6 13 A.M.
10 53 A.M.
3 33 P.M.
II.
20
12
— 20 58
6 I
10 46
3 31
21.
20
44
— 19 10
5 47 .
10 39
3 31
Mar.
3-
21
16
-17 3
5 30
10 31
3 32
Jupiter,
Feb.
I.
12
40
— 2 42
10 3 P.M.
3 54 A.M.
9 45 A.M.
II.
12
38
— 2 30
9 22
3 13
9 4
21.
12
36
— 2 II
8 39
2 32
8 25
Mar.
3-
12
32
- I 47
7 55
I 49
7 43
Sa turn.
Feb.
I.
16
36
— 20 17
3 2 A. M.
7 50 A. M.
12 38P.M.
II.
16
39
— 20 21
2 26
7 14
12 2
21.
16
41
— 20 25
I 49
6 36
II 23A.M.
Mar.
3-
16
43
— 20 26
I 12
5 59
10 46
Uranus,
Feb.
I.
16
4
- 20 36
2 31 A.M.
7 18A.M.
12 5 P.M.
II.
16
5
-20 39
I 53
6 40 ,
II 27 A.M.
21.
16
6
— 20 41
I 14
6 I
10 49
Mar.
3-
16
6
— 20 42
12 35
5 22
10 9
232 Publications of the
Neptune.
1898.
R.
A.
Declination. Rises.
Transits.
Sets.
H.
M.
„
M.
H.
M.
H. H.
Feb. I.
5
17
+ 21 42 I
ID P.M.
8
28 P.M.
3 46A-M
ri.
5
16
+ 21 42 12
30
7
48
3 6
21.
5
16
4- 21 42 II
51 A.M.
7
9
2 27
Mar. 3.
5
16
+ 21 43 II
II
6
29
I 47
Eclipses
OF Jupiter *s
Satellites,
P. S.
T.
(Off left hand limb, as seen
in an inverting: telescope.)
H. M.
H. M.
II, D.
Feb.
3-
9 56 P. M.
III. R,
Feb. 19.
8 42 P. M.
I.D,
4.
I 41 A. M.
I.D.
19-
II 56 p. M.
I. D,
5.
8 10 p. M.
I.D,
21.
6 24 p. M.
II. D,
II.
12 32 A. M.
II, D.
25-
5 44A- M.
I. D,
II.
3 34 A.M.
III. D.
26.
9 58 P. M.
I.D.
12.
10 3 P, M.
I.D,
27.
I 49 A. M.
II. D.
18.
.3 8 A. M.
II. D,
28.
7 2 p. M.
I.D,
18.
5 28 A. M.
I.D,
28.
8 17 P. M.
Minima of Algol, P. S. T
H. M.
H. U.
Feb. 3.
8 41 P. M.
Feb. 18.
4 45 A. M.
6.
5 30 P.M.
21.
I 34 AM.
9-
2 19 P. M.
23-
10 23 p. M.
12.
II 8 A. M.
26.
7 12 P.M.
15-
7 56 A.M.
COMET
b, 1897.
By C. D.
Pbrrinb.
This comet, the second of the year, was discovered by the
writer on the evening of October i6th. It was then in the con-
stellation Camelapardalis, in R. A. 3* 36" 7'. 58, Decl. + 66°
46' 43". 6, at 17** 45" 22', Greenwich M. T. It was then moving
north at the rate of about one and a half degrees per day, and
west 6* On October 29th it passed within about eight degrees
of the pole, and is now moving southward.
The following elements have been deduced from the Mt.
Hamilton observations of October i6th, 24th, and 31st: —
T = 1897 J^ec. 8.84714
a) = 66° 5'42".2 It:.,..- a
^ I Echptic and mean equmox
= 32 4 4.9 > of ,8
» = 69 37 40 .9 )
log q = 0.132056.
Astronomical Society of the Pacific, 233
The residuals for the middle place being: —
Observed — computed, AV cos P^ + 4''.!
A)3' 4 4 .3.
From these elements it will be seen that the comet will make
its closest approach to the Sun on December 8th, at a distance
of one hundred and twenty-five million miles. Owing to the
positions of the Earth and comet in their respective orbits, the
comet slowly approached the Earth for about two weeks after its
discovery, until it was only about seventy-five million miles away.
The distance is now increasing slowly.
At discovery the comet had a clearly-defined stellar nucleus,
resembling a twelfth-magnitude star. This nucleus was in and
very near the north following end of a well-marked, elongated
condensation. Continuing in the same direction as this con-
densation, /. e. s. p., was a narrow streamer of a tail, which
could be traced for a distance of 3' from the head. Around the
whole could be seen a faint nebulosity for a distance of probably
i'. In a week's time the star-like nucleus had disappeared, and
even the condensation about it had lost much of its light. The
changes continued, until by October 31st it was not an easy
object to observe with the 12- inch refractor, owing to its blurred
appearance — there being no well-marked condensation upon
which to set the micrometer wires. At discovery it was quite
bright, even in the moonlight, giving as much light as an eighth-
magnitude star. On October 31st it was carefully examined with
the 36-inch telescope, but no indications of a nucleus were to be
seen; there was a long streak of nebulosity in the head, which
dwindled into a fainter, streamer-like tail. The size of the comet
had changed but little, but instead of being brighter, as it should
be, on the assumption that a comet's light is principally reflected
sunlight, it was actually very much fainter. Comets frequently
show increased activity as they approach the Sun, the nucleus
(should the comet show one) becoming much brighter, and in
some cases even developing one; but here is a case where the
reverse has occurred — the comet losing all signs of the one it
had, and losing much of its light, with no sensible change of
size. So great has been the loss of light, that it was not found
on November 7th (in the moonlight), although the sky for some
distance around its place was carefully examined with the 36-inch
telescope, using the lowest power available — 270. The orbit of
this comet docs not resemble that of any known one.
Lick Observatory, University of California,
November 8. 1897.
234 Publications of the
ELEMENTS OF COMET b, 1897.
By R. Tracy Crau-ford.
From observations made at the Lick Observatory and tele-
graphed to the Students* Observatory by Professor J. M. Schae-
BERLE, Acting Director, I have computed the following sets of
parabolic elements for Comet b, 1897. The first set, from observa-
tions by Mr. Ferrine on October i6th and 17th, and by
Professor Hussey on October i8th, is: —
T= 1897 Dec. 8.86570 G. M. T.
^ = 69- 35' 39".5^ Mean Equinox
a> = 66 6 41 .4 1
q= 1. 355513
Representation of middle place —
A X cos i8 = - o".3 A iS = — i".o
Cot J = 9. 8 1 8048^ Cot Jo = 9. 8 1 8044,
The second set, from observations by Mr. Perrine on
October i6th, and by Professor Hussey on October 31st and
November 15th, is: —
T= 1897 E>ec. 8.550029 G. M. T.
^=69- 35' 5i".0 Mean Equinox
0) = 65 48 38 .0 ) ^'
^=1.357331
Representation of middle place —
AXcos)3=+ ii".7 Ai8=+ i9".6
Cot J = 9- 238929n Cot Jo == 9- 238926„
The value of log M used in determining the second set of
elements was derived from the first set, as follows: —
log M = 0.06462 [
which agrees exactly with the value of
log M = 0.064621
resulting from the second set, so that the second set of elements
must be considered as the best parabolic orbit which can be
passed through the given observations.
University of California, Students* Observatory,
December 13, 1897.
Astronomical Society of the Pacific, 235
NOTICES FROM THE LICK OBSERVATORY.*
Prepared by Members of the Staff.
Resignation of Professor E. S. Holden as Director
OF THE Lick Observatory.
At a meeting of the Board of Regents of the University of
California, held in San Francisco on Tuesday, October 12, 1897,
Professor E. S. Holden* s resignation as Director of the Lick
Observatory was presented and accepted, to take effect January
I, 1898.
At the same meeting Professor J. M. Schaeberle was
appointed Acting Director during the absence of Dr. Holden.
Professor Holden' s letter was as follows: —
** Lick Observatory, University of California, |
Mt. Hamilton, October i, 1897. )
To the Honarabte the Board of Regents of the University
of California: —
Gentlemen: — I beg to tender my resignation as Director of
the Lick Observatory, to take effect at the expiration of my
present leave of absence.
In severing my connection with an institution with which I
have been intimately connected since the year 1874 (under the
direction of the Regents since 1885), ^ wish to express my
obligations to the Board, to the members of the Standing
Committees on the Observatory, on Internal Administration,
and on Finance, and more especially to the Chairmen of these
Committees, for their support, by which alone it has been possible
to bring the establishment to its present high state of efficiency.
In the summer of 1874 the President of the first Board of
* Lick Astronomical Department of the University of California.
236 Publications of the
Lick Trustees visited Washington to consult with Professor
Newcomb and myself upon the plans for the observatory founded
by Mr. Lick. In October of that year I prepared the plans and
programme upon which the Lick Observatory has been built,
organized, and is now administered. A detailed memorandum
on thb subject may be found in the Publications of the Astro-
nomical Society of the Pacific, Vol. IV, page 139 (1892). The
position of Director was offered to me in 1874, and accepted.
The plans of the first Board of Lick Trustees were not carried
out, for reasons which it is not necessary to state here.
In 1876 I became the adviser of the President of the third
Board, and from that time until 1887 all the plans of the build-
ings were made by me, all the instruments ordered from my
specifications (excepting the visual object-glass of the great
telescope, with which Professor Newcomb was alone concerned),
and most of the instruments were mounted and used by me
personally during official visits to Mt. Hamilton in the years
1881, 1883, 1885, and 1886. Correspondence on file at the
Lick Observatory and in the records of the Lick Trust will
exhibit my share in this work.
In December, 1885, I was appointed to be President of the
University of California, and Director of the Lick Observatory,
and I held the former office until 1888. In June of that year
the observatory was formally transferred by the Lick Trustees as
the Lick Astronomical Department of the University, and from
this time onward its scientific history is known to your Board.
The regular annual income of the observatory has been very
small in relation to the wants of the establishment. It has been
used to supply these wants so far as possible, and the whole
observatory — buildings, instruments, and equipment — is now in
excellent condition. Since 1888 the reservoir capacity has been
doubled; the buildings have been made water-tight and much
improved in many respects; the instruments have been consider-
ably increased in number, and they have been provided with
subsidiary apparatus which was lacking; the library has doubled
in size; the area of the reservation has been increased by one
thousand acres, and the whole establishment and equipment is
far more efficient in 1897 than it was in 1888. Only those who
have visited the observatory can appreciate the full force of
these statements.
A considerable number of graduate students have received
Astronomical Society of the Pacific. 237
training here, and have been fitted for responsible positions here
and elsewhere. Some 50,000 visitors have been received and
cared for, and a contribution of importance to the intellectual
advancement of the State has thus been made.
A very large part of the strictly scientific work of the observa-
tory has been accomplished by virtue of subsidies received from
its friends. Most of its apparatus has been presented to us
outright. All of its foreign eclipse expeditions have been sent at
the expense of wellwishers of the institution. The expensive
plates of the Observatory Moon- Atlas, of Vol. III. of our quarto
Publications, etc., have been provided at private cost. The
names of Messrs. D. O. Mills, C. F. Crocker, Walter W.
Law, of Mrs. Phcebe Hearst, Miss Catherine Wolfe
Bruce, among others, are gratefully remembered in this con-
nection. The money value of these gifts is over $47,000.
Mr. Edward Crossley, an English member of Parliament and
amateur of astronomy, presented to the University in 1895 a
three- foot reflecting telescope. Its performance from the year
1879 onwards has shown that it has no superior in the world at
present It is fitted to supplement the work of the three- foot
refractor in an important way. This instrument was established
in its place by the gifts of many citizens of California. Its dome
and mounting were nearly complete in July, 1896. If it is
diligently used, other gifts of like nature will come to the
observatory as they are needed — and such gifts will be required
if the observatory is to maintain its present standing, unless
larger provision is made by the State, or unless a subsidy is
received from the general government.
The observatory has published three quarto and five octavo
volumes, besides an Atlas of the Moon, and two volumes
printed for us by the Smithsonian Institution, and very many
separate articles published in scientific journals. Some perma-
nent provision should be made for the publication of its
work.
In the years which are to come, I wish for the observatory
the fullest measure of brilliant success. Its equipment, situation,
and its personnel will command this, if it is adequately supported.
I am proud to have been connected with the observatory from
its inception, and during its early and formative period, and to
have done my part towards the creation and maintenance of the
spirit which has characterized its own researches and its relations
238 Publications of the
to other scientific establishments throughout the world. I have
given my best endeavors to these ends for twenty-three years.
I am, gentlemen,
Very respectfully and truly yours,
Edward S. Holden.*'
List of Recorded Earthquakes on the Pacific Coast,
1769-1897, BY Edward S. Holden; Illustrated.
The Smithsonian Institution is about to print, in its Miscel-
laneous Contributions, a work with the above title. The data
are derived from a similar list of recorded earthquakes, 1 769-1888
(with a very considerable number of additions and a few correc-
tions), which was issued by the University of California in 1888,
and from the annual publications of the Lick Observatory (printed
in the American Journal of Science, the Publications of the
Astronomical Society of the Pacific, the Bulletins of the U. S.
Geological Survey) since that date. The annual records referred
to have been compiled by Messrs. Holden, Keeler, and
Perrine from observations at Mt. Hamilton, and from miscel-
laneous reports of earthquake shocks. They have been
thoroughly sifted and revised in the present work, which is
believed to contain all trustworthy data on the subject of Pacific
Coast earthquakes since 1769. E. S. H.
Mt. Hamilton, September i, 1897.
Measures of the Companion of Sirius. and of /3 883.
I have obtained measures of the companion of Sirius on two
nights, September 23d and October 2d. On the former date the
companion was readily seen for at least teir minutes after sunrise.
The measures are: —
K Po Weight.
1897-731 i75''-9 3"-92 5
1897.756 174 .4 4 .04 3
Another binary star of considerable interest is fi 883. It was
discovered by Mr. Burnham in 1879, and was soon found to be in
rapid motion. Dr. See {Monthly Notices R. A. S., June, 1897),
in a recent investigation, found the period to be only five and
a half years. If this result is even approximately correct, the star
is by far the most rapid visible binary known.
I have secured three measures recently with the 36-inch
Astronomical Society of the Pcccific. 239
telescope. The two components are of nearly the same magnitude,
and the angles may need to be increased by 180°.
«o Po Weight.
1897-715 3o''.6 o".23 3
.731 29 .9 o .26 4
.797 28 .4 o .28 2
R. G. AlTKEN.
October 23, 1897.
The Leonids in 1897.
The Leonids were watched for from November 13th to
November i8th, inclusive, but no unusual shower was seen. In
fact, the displays were very meager, the greatest number being
observed on the morning of November 17th, when nine Leonids
were counted from 3** 40" to 4** 30" a.m. As the Moon was in
this region of the heavens and near the time of last quarter, the
conditions were not the best. C. D. P.
Comets Due to Return in 1898.
In the year 1898 there are no less than ^vt, periodic comets
due to return to perihelion: —
Winnecke, March 20th; Encke, May 26th; Swift, 1889 VI;
Wolf, June 30th; Temple's first periodic comet.
Of these comets, Winnecke* s, Encke* s, and Wolfs are
well determined and should be found, except, perhaps, Wolfs
which is so situated that it does not become very bright — only
about two and a half times as bright as at the time of its redis-
covery in 1891, when Professor Barnard estimated it at thirteen
and a half magnitude.
In the case of Swift's comet, there is an uncertainty of 0.9
year .in the time of perihelion passage, which precludes any
accurate prediction of its place, and hence renders impracticable
any extended search with large telescopes. Those having small
and moderate-sized telescopes will do well to devote some of their
time to sweeping, with the chance of picking up this comet, and
thereby save another from being added to the already long list of
missing ones.
Temple's first periodic comet was observed at the returns of
1873 and 1879. subsequent to its discovery in 1867, but at the
last two apparitions it was not seen. It is to be hoped that it may
be rediscovered at the coming apparition.
240 Publications of the
The Temple-Swift comet (1869 HI, 1880 IV, 1891 V) was
due to pass perihelion on June 4th of the present year, but owing
to the unfavorable situation of the Earth, the comet was always
in the twilight, and being on the opposite side of the Sun
from the Elarth, its brightness was small, and hence was not
found. Its next return should be more favorable. C. D. P.
Mt. Hamilton, November 20, 1897.
Photograph of the Spectrum of a Meteor.
In Harvard College Observatory Circular No. 20, dated
November 8, 1897, Professor E. C. Pickering states that the
spectrum of a meteor has been photographed for the first time.
At about II P.M. on June 18, 1897, when the eight-inch Bache
telescope (provided with a large objective prism) at Arequipa,
Peru, was directed towards the constellation Telescopium, a
bright meteor appeared in Right Ascension 18** 19"*, Declination
— 47° 10', and passed out of the field of view at Right Ascension
18*' 29", Declination — 50° 30'.
Mrs. Fleming's examination of the photographic plate shows
that the spectrum consists of six bright lines, whose intensity
varies in different positions of the photograph, thereby showing
that the light of the meteor changed as its image passed across
the plate. The intensities of these lines are estimated at 40, 100,
2, 13, 10, and 10, respectively, and their wave lengths show that
the first, second, fourth, and sixth lines are probably identical
with the hydrogen lines H„ Ha, Hy, and H/^. The fifth line is
probably identical with the band which forms the distinctive
feature of the spectra of stars of the third class of the fifth type,
and the third line, which is barely visible, is perhaps identical
with another band contained in these stars.
The Ha line is the most intense of the four hydrogen lines in
the spectrum of the meteor. This is also the case in the spectrum
of o Ceti, and of many other variable stars of long period. The
relations between the other hydrogen lines also indicate an
important resemblance between meteors and stars having bright
lines in their spectra. These results may aid in determining the
conditions of temperature and pressure in these bodies.
Professor Pickering adds that special efforts will be made to
photograph meteor * trails and spectra during the November
meteoric shower of this year. R. G. Aitken.
Astronomical Society of the Pacific. 241
Dimensions of the Planets and Satellites.
In Poptdar Astronomy for October, 1897, Professor E. E.
Barnard gives the results of * * A Micrometrical Determination 01
the Dimensions of the Planets and Satellites of the Solar System,
Made with the 36-inch Refractor of the Lick Observatory."
Below are given Professor Barnard's results in English
miles, and for comparison the values given in Young's General
Astronomy (second issue, 1889).
Barnard.
Miles.
Mer^ry* 2,765
Venus
Mars[^
Pol.
Ceres .
Pallas
Juno .
Vesta.
. 7,826
• 4,352
4,312
485
304
118
243
>^r{Eq- 90,190
IPol 84,570
. 2,452
. 2,045
. 3,558
. 3,345
. 76,470
. 69,780
. 172,610
. 150,480
Jupiter's Satellites
I"
nil
IV
Satuml^'^:
I Pol
Saturn* s
Rings
f Outer diameter, outer ring .
Inner
Center Cassini Division 148,260
Outer diameter, inner ring . . . 145,990
Inner '* " "... 110,070
*' *' crape ring . . . 88,190
Width Cassini Division 2,220
^ Diameter satellite Titan 2,720
l^anus, mean diameter 34,900
Neptune, " ** 32,900
Young's General
Astronomy.
Miles.
3,030
7.700
I 4,230
J (mean diam.)
!No previous
micrometric
measures.
88,200
83,000
2,400 +
2,100 +
3,600
3,000
75,ooo±
68,ooo±
168,000
148,000
144,800
111,800
9i,8oo±
I 6ooi
3,000 or 4,000
(Probably.)
31.900
34,800
R. G. AlTKEN.
Changes in the U. S. Coast and Geodetic Survey.
Mr. Henry S. Pritchett, Ph. D. (Munich), professor of
physics and astronomy in Washington University, St Louis, has
been ap()ointed by the President, Superintendent of the United
States Coast and Geodetic Survey in the place of General
•Professor Barnard states that his measures of Mercury were made with the
12-inch telescope at the transits of 1891 and 1894.
242 Publications of the
W. W. DuFFiELD, resigned. Professor Pritchett was Assistant
Astronomer at the Naval Observatory, Washington, from 1878 to
1880. He has engaged in work for the survey in China and
Japan, as well as in the United States.
The Telegraphic Longitude Net of the United States.
In the Astronomical Journal, No. 412, Professor Charles A.
ScHOTT, of the United States Coast and Geodetic Survey, pub-
lishes a brief summary of the longitude work done by the Survey
between 1866 and 1896. From this paper, the following extracts
are taken: —
In 1851, S. C. Walker, Assistant, reported the following
values for the longitude of the Cambridge Observatory: —
West of Greenwich,
h m s
From Moon culminations, 4 44 28.42
From eclipses, transits, and occultations, 4 44 29.64
By chronometric expeditions, 4 44 30.10
In the autumn of 1845, Superintendent Bache instructed
Assistant Walker to devise practical means for the employment
of the electric telegraph (publicly tested by Morse in May,
1844) for longitude work. With the co-operation of the United
States Naval Observatory, the cities of Washington and Phila-
delphia were connected on October 10, 1846, and their differ-
ence of longitude was found to be 7" 34V 3. After Professor
Walker's retirement in 1852, Dr. B. A. Gould took charge
of the longitude work of the Survey up to 1867; the Coast Survey
Report of that year contains his report ' ' On the Longitude
between America and Europe from Signals through the Atlantic
Cable." The resulting longitude of the Cambridge Observatory
was 4** 44" 30«.85.
Other cable determinations were secured by the Coast Survey
in 1870 and 1872, but the latest determination, in 1892, is due
to the co-operation of the McGill College Observatory at Montreal,
Canada, with the Greenwich Observatory.
The final value for the longitude of the Harvard Observatory
at Cambridge, as adjusted in June, 1897, *s, —
4*^ 44" 3 1 '.046 ±: o*.048.
The longitude net as developed during thirty years, including
some European stations, is composed of forty-five stations, con-
nected by seventy-two links. Practically, three lines cross the
continent, one near our nothern boundary, one near the southern,
Astronomical Society of the Pacific, 243
and an intermediate one and the three are connected by cross lines.
The smallness of the probable errors of measure shows the satis-
factory character of the obser\'ations.
The table of final resulting longitudes west of Greenwich is as
follows: — 1, ^
Greenwich, England (Transit circle) 00 0.000
Paris, France (Meridian of France) o 9 20.968 E.
Brest, France (Tower of St. Louis) 017 57.597
Foilhommerum, Ireland (Transit) 041 33.409
He«rt*s Content, Newfoundland (Transit) 3 33 29.788
St. Pierre Island, Miquelon Group (Transit) 3 44 42.427
Calais, Maine (Transit) 4 29 7.857
Duxbury, Ma.ss. (Transit) 4 42 40.858
Cambridge, Mass. (Dome, Harvard College Obs'y) . . 4 44 31.046
Montreal, Canada (Transit McGill College Obs'y). . . 4 54 18.634
Albany, N. Y. (Dome, Dudley Obs'y; old site) 4 34 59.992
Cape May, N. J. (Transit) 4 59 43.045
Washington, D. C. (Dome U. S. N. Obs'y; old site) ... 5 8 12.153
Charleston. S. C. (Transit) 5 19 44.076
Key West, F*la. (Transit) 5 27 13.579
Detroit, Mich. (Transit of 1891) 5 32 11.830
Atlanta, Ga. (Transit of 1896) 5 37 33.338
Cincinnati, O. (Dome, Mt. Lookout Obs'y) 5 37 41.398
Louisville, Ky. (Transit) 5 43 3.636
Nashville, Tenn. ^Transit) 5 47 8.083
Chicago, 111. (Transit of 1891) 5 50 29.446
New Orleans. La. (Transit of 1895) 6 o 16.763
St Louis, Mo. (Transit, 1882, of Washington Univ.) ..60 49.256
Liule Rock, Ark. (Transit) 69 5.727
Minneapolis, Minn. (Transit) 6 12 56.845
Kansas City, Mo. (Transit) 6 18 21.404
Galveston Tex. (Transit of 1895) 6 19 9.928
Omaha, Neb. (Transit) 6 23 46.087
Austin, Tex. (Transit) 6 30 57.024
Bismarck, N. D. (Transit) 6 43 7.938
Colorado Springs, Colo. (Transit of i886j 6 59 16.710
Santa Fe, N. M. (Transit) 7 3 46.805
El Paso, Tex. (Transit) 7 5 57.386
Nogales, Ariz. (Transit) 7 23 45.912
Salt Lake City, Utah (Transit) 7 27 35.173
Helena, Mont. (Transit) 7 28 8.789
Needles, Cal. (Transit) 7 38 24.836
Yuma, Ariz. (Transit) 7 38 29.608
San Diego, Cal. (Transit of 1892) 7 48 38.748
Los Angeles, Cal. (Transit of 1892) 7 53 1.561
Walla Walla, Wash. (Transit) 7 53 23.331
Sacramento, Cal. (Transit) 8 5 5^.387
Seattle, Wash. (Transit) 8 9 20.358
San Francisco, Cal. (Transit, Lafayette Park) 8 9 42.861
Portland, Oregon (Transit) 8 10 42.838
244 Publications of the
The paper also contains the longitudes of a few prominent
observatories directly connected with the Coast and Geodetic
Survey system. From these we take the longitude of
U. S. Naval Observatory — new ^\\jt\ meridian of clock room: —
h m s s
5 8 15.784 ±0.050
Lick Observatory, Mt. Hamilton — meridian of transit house: —
h m s s
8 6 34.895 i 0.057
Observations of the Companion to Procyon.
The following observations of Procyon' s companion were
made with our great refractor. For the purpose of showing the
orbital motion, the discovery position is also given: —
Date.
1897.
October 8.
Position
Angle.
324°. I
Distance.
4". 70
17.
18.
323 -o
323.8
4.76
29.
30.
November i.
324.2
326 .2
324 .3
4.51
4.59
4 .67
15-
325 .2
4 .71
Mean position for 1897.821
Discovery position 1896 812
324 .40
318.8
4.66
4 .59
. Procyon' s companion has finally been seen at two other observa-
tories. Dr. See of the Lowell Observatory informs me that he
and his assistant, Mr. Boothroyd, saw and measured the com-
panion on the ist of the present month. Professor Barnard writes
that on the 3d, during a few moments of steadiness, the companion
was * * clearly and distinctly seen ' ' with the great refractor of the
Yerkes Observatory. So far as I know, these are the only
observations made away from Mt. Hamilton. J. M. S.
Lick Observatory, November 18, 1897.
Lick Observatory Eclipse Expedition.
The Crocker eclipse expedition from the Lick Observatory, to
observe the total solar eclipse of January 21-22, 1898, sailed from
San Francisco on the steamship "China*' on October 21st,
going via Hongkong to Bombay. From this point it is expected
to move inland some 150 or 200 miles, to a station near Karad.
The expedition is in charge of Professor W. W. Campbell.
Astronomical Society of the Pacific. 245
He is accompanied by Mrs. Campbell and Miss Rowena Beans
as volunteer assistants, traveling at private expense.
Professor Campbell takes with him a number of instruments
for the observation of the eclipse, and expects to secure the
needed assistance in India. Besides the 40-foot telescope for
large-scale photographs of the corona on Professor Schaeberle's
plan, he has several spectroscopes for special observations. An
effort will be made to photograph the changes in the spectrum
due to the ** reversing layer," which have been noticed visually
at previous eclipses, and also to secure photographs of the 1474
K line, for the purpose of determining the question of rotation
of the corona.
The funds to defray the expenses of the expedition were pro-
vided by the late Colonel C. F. Crocker, who had provided
for two previous eclipse parties from the Lick Observatory.
A private cablegram from the party at Hongkong advises their
safe arrival at that port aiid their close connection with the steamer
for Bombay. The latter port should be reached about December
5th. C. D. P.
The Chabot Observatory Eclipse Expedition.
Professor Charles Burckhalter, Director of the Chabot
Observatory, Oakland, Cal., sailed for Hongkong on Saturday,
October 30th, and will proceed to India for the purpose of
observing photographically the total solar echpse of January 22,
1898. The exact location of his station will not be decided until
he reaches Bombay. Probably it will be somewhere near one of
the railroads, a short distance from that city.
Professor Burckhalter*s apparatus is essentially the same
as that he took to Japan in 1896, an account of which may be
found on page 157, Vol. VII, of these Publications,
The equipment described therein has been augmented by
another lens of the same diameter and focal length, which is the
gift of Dr. George C. Pardee. It will be packed separately
from the other, so that in the event of the loss, damage, or delay
of any of the baggage, he will be reasonably sure of having one
lens. It is his intention to use both lenses, one with his shutter,
the other in the usual manner. The two tubes will be mounted
together, one above the other, and the exposures will be coin-
cident, both as to duration and period.
A new mounting was necessary, on account of the additional
246 Publications of the
load. It is constructed almost entirely of heavy gaspipe, and is
extremely rigid. The polar axis is hollow, and is fitted with an
eyepiece, as an aid in adjusting. The automatic arrangements
for securing certainty in exposing have been elaborated upon to
such an extent that the inventor now feels certain that nothing
can go wrong, at least with this part of the expedition.
Professor Burckhalter*s parting injunction to his friends
was not to wish him a good time or a pleasant journey, but that
he might have two minutes of clear sky at the right time. Those
of us who have heard him describe the disappointing day in
Japan in 1896, and who realize what the success of this expedi-
tion means, will be certain to remember him on the eventful day.
If friendly good wishes can insure success, he will have it.
Allen H. Babcock.
Elements of Comet b, 1897 (Perrine).
From Mt. Hamilton observations, made on October i6th,
1 8th, and 20th, we have computed the following elements of the
orbit of this comet: —
T r= 1897 Dec. 9.89171 G. M. T.
0, = 67° 6' 55". 2 ) . , . ^ ,. ,•
' ^^ \ Mean equmox and ecliptic
n ^ 32 8 37 .4 \ ,s97.o
/ = 69 45 43 .2 )
log ^ = o. 1 29500.
Residuals for the middle place (O — C): —
AX cos /3 = + 2".8, A^ = +2".4.
A comparison of observations made on November ist with
the ephemeris positions computed from these elements shows a
satisfactory agreement. W. J. Hussey and R. G. Aitken.
November 3, 1897.
Astronomical Telegrams (Translations),
Lick Observatory, Oct. 17, 1897.
To Harvard College Observatory: ; ^5^^^ ^ .^ ^ ^^
To Students' Observatory, Berkeley:^
A comet was discovered by C. D. Perrine, October 16.7398,
G. M. T.; R. A. 3* 36" 7'.6; N. P. D. 23° 13' 16". The comet
is about 2' in diameter, is as bright as an eighth magnitude star,
has a well-defined nucleus and a tail less than 30' long.
Astronomical Society of the Pacific. 247
Lick Observatory, Oct. 18, 1897.
To Harvard College Observatory: ) ^3^^^ ^ .^^ ^^^^
To Students' Observatory, Berkeley: )
Comet b, 1897 (Perrine), was observed by C D. Perrine,
October 17.7121, G. M. T.; R. A. 7^" ^d^ 2^\^\ N. P. D. 21°
42' 47''.
Lick Observatory, Oct. 18, 1897.
To Harvard College Observatory: y ^^^^^ ^^^
To Students' Observatory, Berkeley:)
Comet ^, 1897 (Perrine), was observed by W. J. Hussey,
October 18.6498. G. M. T.; R. A. 3*' 24'° 2'. 2; N. P. D. 20°
16' 06''.
Lick Observatory, Oct. 19, 1897.
To Harvard College Observatory: (Sent 5:10 p.m.)
Comet b, 1897, was observed with the Meridian Circle by
R. H. Tucker, October 18.901 1, G. M. T.; R. A. 3*' 22° 5'. 5;
N. P. D. 19° 52' 49".
Lick Observatory, Oct. 19, 1897.
To Harvard College Observatory: (Sent 9:15 a.m.)
Elements and ephemeris of Comet b, 1897, were computed by
W. J. Hussey and R. G. Aitken.
ELEMENTS.
T = G. M. T. 1897, ^^^' 9.2300.
0) = 66° 28' \
O = 32 5 VMean equinox of 1897.0
z = 69 38 )
q = 1.3525-
[The ephemeris at four-day intervals, from October 20th to
November i, 1897, is here omitted.]
248 Publications of the
Minutes of the Meeting of the Board of Directors,
held in the rooms of the society,
November 27, 1897.
Mr. PiERsoN presided. A quorum was present. The minutes of
the last meeting were approved. The following members were duly
elected: —
List of Members Elected November 27, 1897.
r American Museum of Natural
Prof Albert S. Bickmore ....-! History, Central Park, New
I York, N. Y.
Miss GEAKON {"^tScrffiand:"'*'''""'''
Mr. A. Perrenod Saint- Pierre, Martinique.
The following letter was presented to the Directors: —
Mount Hamilton. October i, 1897.
The Board of Directors^ Astronomicnl Society 0/ iht Pacific.
Gentlbmen: — I beg to tender my resignation as a member of the Directors A. S. P.,
and as one of the Committee on Publication, to take effect on December 1, 1897. I shall
hope to retain my connection with the Society during my lifetime. I have the pleasure oC
thinking that the situation of our Society is much improved since the early days of its
formation, and that our power and influence for good is now well established, thanks to the
unwearied efforts of some of the members. In spite of some obstacles which have had to be
overct me, it would seem that we are now firmly established as a veritable force for advancing
Science in the United States and elsewhere.
I wish for the Society continued success and usefulness, and it will be my effort, in the
future as well as in the past, to contribute to these ends to the best of my ability.
With my personal good wishes to each one of your Board, and my thanks for your friendship
during the years of our pleasant association, believe me. Gentlemen,
Very cordially yours,
Edward S. Holdbn.
Upon motion by Mr. Pierson, the following resolutions were
adopted: —
Whfrkas', Dr. Edward S. Holdbn has tendered his resignation as a member of the
Board of Directors of this Society, and the Board is now called upon to act on the same, be it
Resolvedy That it is with sincere regret that the Board accepts said resignation, which it
does solely for the reason that Dr. Holdbn's absence from the State prevents him from attend-
ing to the duties of the ofhce;
Rcsoh'edt That as the founder of this Society, as its First President, as a continuing member
of its Board of Directors, and as the able editor of the Publications of the Society, Dr. Holdbn
is entitled to the gratitude of all its members, and deserving of such marks of esteem as this
Board has the power to grant; and it is therefore further
Resol7'ed, That Dr. Holdfn be, and he is hereby elected a life Member of this Society; —
and the Secretary is instructed to forward a copy of these resolutions to him.
The following members were appointed to fill the vacancies caused
by Dr. Holden's resignation; to date from December i, 1897: —
As First Vice-President Mr. E. J. Molera.
As a Director Mr. R. H. Tucker.
As a member of the Committee }
on Publication. f • • • Mr. F. H. Shares.
Adjourned.
Astronomical Society of the Pacific. 249
Minutes of the Meeting of the Astronomical Society
OF THE Pacific, held in the Lecture Hall of
THE California Academy of Sciences,
November 27, 1897.
The meeting was called to order by Mr. William S. Moses. The
minutes of the last meeting, as printed in the PublicaiionSy were
approved.
The Secretary read the names of new members duly elected at the
Directors' meeting.
The following papers were presented: —
1. Dedication of the Yerkes Observatory, by Mr. Frederick H.
Seares.
2. Planetary Phenomena for January and February, 1898. by Professor
M. McNeill, of Lake Forest.
3. Catalogues 111 and IV of New Nebulae discpvered at the Lowe
Observatory, by Dr. Lewis Swift.
4. The Yerkes Observatory, by Professor W. J. Hussey.
5. Comet b, 1897, by Mr. C. D. Perrine.
Mr. Seares delivered an address upon the dedication of the Yerkes
Observatory, giving a description of the equipment of this institution,
and an account of the opening exercises, which he attended in person.
Adjourned.
250 Publications of the Astronomical Society &c.
OFFICERS OF THE SOCIETY.
Mr. William Alvord Pr^sidemt
Mr. E. J. MoLSRA Ftrst I'lce-Preiidrnt
Mr. Frederick H. Skakks Second VLe-Preademt
Mr. Chaun'Cky M. St. John Third Vi-.t-Presiacni
Mr. C. D. PbRRINK ( K^rr^t^r^,^
Mr. F. R. Z.KL i i^ccretartex
Mr. F. R. ZiKL Treasurer
Board of Directors- Messrs. Alvoru, Mulkra, Morse, Miss O'Hallokan, Messrs.
Pkrrink, PiKRSON, Skakes. St. John, Tucker, von Geldekn, Ziel.
Finance Committee — Messrs. William M. Pibrson, E. J. Molbra, and C. M. St. Juhn.
I Committee on Publication — Messrs. Aitken, Babcock, Seares.
Library Committee— "SitssTt. HussEY and Sbarbs and Miss O'Halloran.
Committee OH the Comet- Afeda/^S\essTs. Holden (ex-ojicio), Schabbbrle, Camfbell.
OFFICERS OF THE CHICAGO SECTION.
Executive Committee — .Mr. Ruthven W. Pike.
OFFICERS OF THE MEXICAN SECTION.
Executix'e Committee— lA. Francisco Rodriguez Rev.
NOTICE.
The attention of new members is called to Article VIII of the By-Laws, which provides that
the annual subscription, paid on election, covers the calendar year only. Subsequent annual
payments are due on January ist of each succeeding calendar year. 1 his rule is necessary in
order lo make our book-keeping as simple as possible. Dues sent by mail should be directed to
Astronomical Society of the Pacific S19 Market Street, San Francisco.
It is intended that each member of the Society shall receive a copy of each one of the Pub-
lications for the year in which he was elected to membership and for all subsequent years. If
there have been (unfortunately) any omissions in this matter, it is requested that the Secretaries
he at once notified, in order that the missing numbers may be supplied. Members are requested
to preserve the copies of the Publications of the Society as sent to them. Once each year a title*
page and contents of the preceding numbers will also be sent to the members, who can then bind
the numbers together into a volume. Complete volumes for past years will also be supplied, to
members only, so far as the stock in hand is sufficient, on the payment of two dollars per volume
to either of the Secretaries. Any non-resident member within the United States can obtain
books from the Society's library by sending his library card with ten cents in stamps to the
Secretary A.S. P., 819 Market Street, San Francisco, who will return the book and the card.
The Committee on Publication desires to say that the order in which papers are printed in
the Publications is decided simply by convenience. In a general way, those papers are printed
first which are earliest accepted for publication. It is not possible to send proof sheets of papers
to be printed to authors whose residence is not within the United States, llie responsibility for
the views expressed in the papers printed rests with the writers, and is not assumed by the
Society itself.
The titles of papers for reading should be communicated to either of the Secretaries as early
as possible, as well as any changes in addresses. The Secretary in San V rancisco will send to
any member of the Society suitable stationery, stamped with the seal of the Society, at cost price,
as follows: a block of letter paper, 40 cents; of note paper, 35 cents; a package of envelopes, 95
cents. These prices include postage, and should be remitted by money-order or in U. S. postage
stamps. The sendings are at the risk of the member.
Those members who propose to attend the meetings at Mount Hamilton during the summer
should communicate with "The Secretary Astronomical Society of the Pacific *' at the rooms of
the Society, 810 Market Street, San Francisco, in order that arrangements may be made for
transportation, lodging, etc.
PUBLICATIONS ISSUED BIMONTHLY.
( February t April, June, August, October, December. f
GENERAL INDEX TO VOL. IX.
Page
Abjuratio Galilei 30
Asirono mische Gesellscha/t Zon^, — 9® 50' to — 14° 10' (note) . ... 40
AiTKEN, R. G., Elements of Comet by 1897, with W. J. Hussey, 246;
Dimensions of Planets and Satellites, 241; Light Absorption as a
Factor in Determining the Size of Objectives (note), 98; Measures
of the Companion to Proycon, 47; Measures of ^ Delphini, 93;
Measures of Sirius, 10 1; Measures of Sirius and ^ 883. 238;
Observation of the Solar Eclipse of July 29, 1897, 195; Statistics
of the Lick Observatory Library, 150; Weather at Mt. Hamilton
in Winter of 1896-97, 103; The Bruce Photometers of the Lick
Observatory, 184; The Great Sun-Spot of January, 1897 (note), 43;
Photograph of the Spectrum of a Meteor (note) 240
Ames, Kate, Unusual Lunar Halo, August 5, 1897 195
Arrhenius, S., Influence of Carbonic Acid in the Air on the Earth's
Temperature 14
Astronomical Society of the Pacific, By-Laws of 163
Bruce Medal of, 104, 168; Comet-Medal of, 170; Corresponding
Institutions of, 12; Exchanges of, 13; Members of, i; Minutes of
Meeting of Board of Directors of. 49, 113. 118, 160, 205. 206,
207, 248; Minutes of Meetings of Society, 50, 114, 160, 206, 249;
Officers of, 51, 119, 161, 171, 208, 250; Report of Committee on
Comet-Medal, 115; Report of Treasurer 116
Astrographic Charts 102
Astronomical Telegrams 47, 155, 246
A«itronomy and Astronomers in Their Relations to the Public, by
W. J. Hussey 53
Atlas der Himmelskunde 145, 203
Awards of the Donohoe Comet-Medal 36, 38, 99
Babcock, a. H., Earthquake at Oakland, January 17, 1897 .... 45
Earthquake of June 20, 1897 135
Chabot Observatory Eclipse Expedition 245
Barnard, E. E., Honor Conferred on (note) 44
Bond, W. C. and G. P., Memorials of (note) 100
W. C, Portrait of, to face 89; note 91
Bruce, Gift to Prague Observatory loi
Medal for Astronomical Society of the Pacific, 104, 168; Pho-
tometers of Lick Observatory, 184; Photographic telescope, ist
results of (note) 93
Burton-Brown, A. Col., Total Eclipse of Sun, January 22, 1898 . . 189
Campbell, W. W., Recent Observations of the Spectrum of Mars . 109
Carbonic Add in the Air, Its Influence on the Temperature of the
Earth, by Prof. S. Arrhenius 14
252 Publications of the
Pack
Chabot Observatory Eclipse Expedition 245
Clark, Alvan G., Death of (note) 152
Coast and Geodetic Survey, Longitude Net of, 242; Change in (note) 241
CoDDiNGTON, E. F., The Cause of Gravitation (translation) .... igo
CoLTON, A. L.. The Great Sun-Spot of January, 1897, with Photo-
graphs 42
Photograph of the Solar Surface, with C. D. Perrinb, Frontispiece
Resignation of 203
Comets, Due to Return in 1898 239
Comet, DoNATi's, Photograpli of (note) 89
Reported by Swift, Search for (note) 89
g 1896, Perrine, Discovery, 39; Elements by Seares and Craw-
ford, 36; Elements by Hussev and Perrine, 40; Elliptic
Elements by Hussev and Perrine. 46; Telegrams 47. 48
D'Arrest's, Rediscovery by Perrine 155
Comet b, 1897 (Perrine), Elements by W. J. Hussev and R. G.
AlTKEN 246
Note on, by C. D. Perrine, 232; Telegrams on 246
Medal, Awards of, 36, 38, 99; Rules of 170
CoMSTOCK, George C, The Washburn Observatory 31
Corresponding Institutions of the Astronomical Society of the Pacific 12
Crawford, R.T.. Elements of Comet ^, 1896; Comet h, 1897 . . 36, 234
Crocker, C. P., Death of (note) 160
Crossley Reflector, Trial of (note) 159
DooLiTTLE, C. L., The Sayre Observatory 130
Double Stars, Measures of. See Aitken, Lehman; Procyon, Sirtus,
Eclipse of Sun, July 29, 1897, by D. E. Hadden 188
Observations of, by R. G. Aitken, 195; Predictions for, by C. D.
Perrine 85
January 22, 1898, by E. W. Maunder 131
By Col. A. Burton-Brown, 189; Expedition to, from Lick
Observatory (notes), 155, 244; from Chabot Observatory (note) 245
Earthquakes in California in 1896. by C. D. Perrine 37
At Oakland, January 17, 1897, by A. H. Babcock, 45; Of June
20. 1897, by A. H. Babcock, 135; by S. C. Lillis, 135; On Pacific
Coast, Catalogue of (note) 238
Errata in Publications Astronomical Society of the Pacific . . . . 47. 90
Exchanges, Astronomical Society of the Pacific 13
Gravitation, The Cause of, by V. Wellman 190
Hadden, David E., Eclipse of Sun, January 29, 1897 188
Review of Solar Observations for 1895-96 77
Hagen, J. G, A New Observatory 121
Heliocentric Theory and the University of Cambridge in 1669 (note) 43
Holden, E. S., a New Celestial Atlas (review) 145
Albert Marth (biographical notice), 202; Appointments in the
Lick Observatory (note), 160; Atlas der Himmelskunde (note),
203; Bruce Medal, 105; Catalogue of Pacific Coast Earthquakes
from 1767 to 1897, 238; Cost of Lick Observatory Library (note),
201; Death of Alvan G. Clark (note), 152; Death of Chas. F.
Astronomical Society of the Pacific. 253
Pack
Crocker (note), i6o; Experiments with the Moving Floor of the
Large Dome, 148; First Results from the Bruce Photographic
Telescope (note), 93; HoenA Wronski (note), 90; Howe's Ele-
ments of Astronomy (review), 94; Inventory of Lick Observatory,
Buildings and Equipment, 201; Lick Observatory Eclipse Expe-
dition to India (note), 155; Lowell's Observations of Mercury
and V^enus^ 92; Memorials of W. C. and G. P. Bond (note), 100;
Notice to Members A. S. P., 41; Observatory Moon Atlas, 202;
Photographs of Donati's Comet (note), 89; Photograph of
Solar Surface (note), 39; Portrait of W. C. Bond (note), 91; Por-
traits of Astronomers (list), 95; Mt. Hamilton Post Office, 151;
Probable Errors of Some Star Catalogues, 107; Reflector and
Portrait Lens in Celestial Photography (note), 147; Relief Map
of Lick Observatory Reservation, 40; Resignation of, 235;
Reversing-Layer of the Corona (note), 100; Small Telescope
for Sale (note), 160; Stability of the Great Equatorial, 147 ; Trial
of the Crosslev Reflector (note), 159; The Work of the Lick
Observatory 196
Howe's Astronomy (review) 94
Hussev, W. J., Astronomy and Astronomers in Their Relations to
the Public 53
Elements of Comet ^, 1897, with R. G. Aitken, 246; Elements
of Comet ^, 1896, 40; Elliptic Elements of Comet ;f, 1896, with
C. D. Perrine, 46; Measures of Procyon, 147; Search for Comets
Reported by Swift, September 20, 1896 (note), 89; The Yerkes
Observatory 209
Instrument Making at Alleghany (note) 151
yi#/i/^. Photographs of, by J. M. Schaeberle 173
Kohl, Torvald, Astronomical Observations in 1896 65
Ladd Observatory, The (note) 47
Lehman, D. A., Measures of Double Stars 141
Leonids^ See Meteors.
Lick Observatory, Appointments in 151, i6t\ 235
Bruce Photometers of, 184; Eclipse Expedition to India, 155,
244; Experiments with the Moving Floor of the Great Dome,
148; Graduate Students at, 151; Inventory of, 201; Latitude of,
loi; Library, Cost of, 201; Statistics of, 150; Moon Atlas, 202;
Post Office at, 151; Relief Map of Reservation, 40; Resignation
of Director of, 235; Stability of the Great Equatorial of, 147;
Weather at, 103; Work of 196
Light Absorption as a Factor in Determining the Size of Objectives. 98
LiLLis, S. C, Earthquake of June 20, 1897 135
Longitude Net of the United States Coast and Geodetic Survey . 242
Lowell Observatory, Return to Arizona (note) 105
Luminous Appearances in the Sky, Sqme, by W. H. S. Monck . . 33
Lunar Halo, Unusual (note) 195
Mars, Rift in the Polar Cap of 48
Mars, Spectrum of, by W. W. Campbell 109
Marth, a., Biographical Notice of 202
254 Publications of the
Page
Ephemeris for Physical Observations of the Moon 76, 108
Maunder, E. W., English Preparations for Total Eclipse of January
22, 1898 131
McNeill, Malcolm, Planetary Phenomena .... 24, 70, 136, 174, 226
Members of Astronomical Society of the Pacific, List of i
Mercury and Venus, Lowell's Observations of 92
Meteors of November 15, 1896 (note) 41
A Brilliant (note), 44; Of January 24, 1897 (note), 91; Of January
26, 1897 (note), 90; Of May 5, 1897 (note), 146; The Leonids (note),
41; Leonids in 1897, The, 239; Photograph of the Spectrum of . 240
Metric System (note) 90
MoNCK, VV. H. S., Some Luminous Appearances in the Sky .... 33
The Spectra and Proper Motions of Stars 123
Moon, Atlas of 202
Ephemeris for the Physical Observations of, by A. Marth, 76, loS
Weinek's Photographic Atlas of 156
Moses, Wm. S., A Brilliant Meteor (note) 44
Nebulae, Lowe Observatory Catalogues of, by Lewis Swift . . 186. 223
Notice to Members of ihe Astronomical Society of the Pacific . . 41, 108
Observatory, Dedication of Flower 148
Ladd. 47; Washburn, 31; Royal, at Greenwich, 152; The
Savre, 130; Valkenburg, 121; Yerkes 209
Observations, Astronomical, in 1896, by Torvald Kohl 65
O'Halloran, Miss Rose, Maximum of o Ceti 86
Perrine, C. D., Comet b, 1897 232
Discovery of Comet g, 1896, 39; Elements of Comet g, 1896, 40;
Elliptic Elements of Comet g^ 1896, with W. J. Hussev, 46;
Earthquakes in California in 1896, 37; Fireball of January 26,
1897 (note), 90; Lick Observatory Eclipse Expedition, 244;
Photograph of Solar Surface, with A. L. Colton, Frontispiece;
Predictions for Solar Eclipse of July 29, 1897, 85; Comets Due
to Return in 1898, 239; The Leonids in 1897, 239; Rediscovery
of D'Arrest's Comet • 155
Photograph of Solar Surface (note) 39
Frontispiece, by A. L. Colton and C. D. Perrine
Photographic Durchmusierung ^ Cape 105
Photometers, The Bruce, by R. G. Aitken 184
Planetary Phenomena, by Malcolm McNeill ... 24, 70. 136, 174, 226
Planets and Satellite*^, Dimensions of 241
Portraits of Astronomers 95, 204
Prague Observatory, Gift of Miss Bruce to 107
pRiCHETT, H. S., Appointed Superintendent of United States Coast
and Geodetic Survey 241
Observations of the Companion of Sirius 104
Procyon, Measures of the Companion to 46, 47, 147, 244
Proper Motions of Stars, by W. H. S. Monck 123
Reese, S. J., Meteor of January 24, 1897 (note) 91
Reflecting Telescopes, Prices of (note) 44
Reflector and Portrait Lens in Celestial Photography (note) .... 147
Astronomical Society of the Pacific. 255
Pack
Royal Astronomical Society, American Foreign Associates .... 45
Americans Who Have Received the Medal of 45
ScHAEBERLE, J. M., Measures of the Companion to Procyon .... 244
Meteor of May 5, 1897, 146; Observations of the Companions of
Procyon ?ixv^ Sirius^ ^^\V\\o\o%x?i^\i%o{ Jupiter 173
Searle, Arthur, A. G., Zone, —9° 50' to — 14° lo^^(note) .... 40
Seares, F. H.. and Crawford, R. T., Elements of Comet ^, 1896. 36
SiriuSf Measures of 46, loi, 104, 238
Solar Observations, by David E. Hadden . . 77
Spectra and Proper Motion ot Stars, by W. H. S. Monck 123
Stars, Catalogue of Fundamental ic6
Probable Errors of Catalogues of, 107; Spectra and Proper
Motions of 123
Sun, Photograph of (note), 39 Frontispiece
Eclipse of July 29, 1897 188
Reversing Layer of Corona (note), 100; The Great Sun-Spot
of January, 1897, with Photographs, by A. L. Colton 42
Swift, Lewis, Catalogues of Nebulae Discovered at the Lowe
Observatory, 186, 223; Honor Conferred on (note) 47
Telescope for Sale (note) 160
Tucker, R. H., Latitude of Lick Observatory 10 1
Upham, Mrs. F. K., Meteors of November 15, 1896 (note) .... 41
Vaikenburg, A New Observatory at, by John G. Hagen 122
Variable Star, Maximum of o Ceii 86
Venus and Mercury ^ Lowell's Observations of 92
Washburn Observatory, The, by G. C. Comstock 31
Weinek, L., Photographic Atlas of the Moon 156
Wellm AN, v., The Cause of Gravitation 190
VVronski, HoENfe (note) 90
Yates, William, The A^i7«/V/ Meteors (note) 41
Yerkes Observatory, The, by W. J. Hussev 209
I
J
/
'/ ■/' >->
'^
Aflov
V,
PUBLICATIONS
>^^^
^-.-^> :<<•..
ASTRONOMICAL SOCIETY
OF THE PACIFIC.
VOLUME X.
i8g8.
SAN FRANCISCO
PRINTED FOR THE SOCIETY,
1898.
THE NEW YORK
PUBLIC LIBRARY
A8TOR, LENOX AND
TIL DEN FOUNDATIONS.
R 1901 L.
TABLE OF CONTENTS.*
Publications No. 60, February i, 1898.
Pagb
The Great Nebula in Andromeda^ from a Photograph by E. F.
CoDDiNGTON FrontispUcf
List of Members of the Society, January I, 1898 i
List of Corresponding Observatories and Institutions 11
A Series of Six Star Maps, by C. D. Per R I NE ......... 15
Map I to face page 15
Maps II, III, IV, V, VI .to face page 16
Planetary Phenomena, for March and April, 1898, by Professor
Malcolm McNeill 16
Twenty-eighth Award of the Donohoe Comet-Medal to Mr. C. D.
Perrinb . 22
Astronomical Observations in 1897, by Torvald Kohl 22
First Award of the Bruce Medal to Professor Simon Newcomb . . 26
Spectroscopic Binary Stars, by R. G. Aitken . . . . . ... . . 26
Notices from the Lick Observatory 35
Rediscovery of Winnecke's Periodic Comet = <x 1897. C.*D. P. . 35
The Probable State of the Sky along the Path of Total Eclipse of
the Sun, May 28, 1900. Abstract of Report by Professor F. H.
BiGELOW in Monthly Weather Review for September, 1897 . 35
Eclipses of Jupiter's Satellite IV. C. B. Hill 36
The Star with the Largest Known Proper Motion. R. G. A. . 37
Astronomical Telegram : Observation of Winnecke's Comet
byC. D. Perrine 37
Observational Astronomy: A Practical Book for Amateurs, by
Arthur Mee, F. R. A. S 37
Some Interesting Double Stars. R. G. A 38
Errata in Star Catalogues. R. G. A 39
Award of the Lalande Gold Medal to Assistant Astronomer
C. D. Perrine of the Lick Observatory. J. M. S 40
Belopolskv's Researches on 17 Aquilce. W. J. H 41
Meteors Visible in Full Daylight. E. F. C 41
Report on the Teaching of Astronomy in the United States.
R. G.A 42
Success of the CROCKER-Lick Observatory Eclipse Expedition.
J.M.S 43
Death, of Dr. Winnecke 43
Success of the PiERsoN-Chabot Observatory Eclipse Expedition.
J.M.S 44
The Great Nebula in Andromeda, E. F. C 45
• To the Binder : This should precede page i, Volume X.
IV Publications of the
Pack
Minules of the Meeting of ihe Directors, January 2g, i8g8 46
List of Members Elected 46
Minutes of the Meeting of the Society, January 2g, 1898 46
Officers of the Society, etc 47
Publications No. 61, April 2, 1898.
A Lunar Landscape cut to face page 49
Address of the Retiring President of the Society, in Awarding the
Bruce Gold Medal to Professor Simon Newcomb, by William
Alvord • 49
Planetary Phenomena, forMay and June, 1898, by Professor Malcolm
McNeill 59
List of Earthquakes in California for the year 1897, compiled by
C. D. Perrine. d4
Latitude Work with the Fauth Transit Instrument of the Lick
Observatory, by H. D. Curtis 67
The Royal Observatory, Edinburgh, Scotland, from the Southwest
cut to face page 69
The Royal Observatory, Edinburgh. Scotland, by R. G. Aitken . 69
The 15-inch Equatorial Refractor, Royal Observatory, Edinburgh .
. , . . ' cut to face page 70
A New Variable Star, by Torvald Kohl 72
Magnifying Ratios of Ewing Seismographs of Three Components,
and of the Duplex-Pendulum Seismographs, by C. D. Perrine . 7a
The 24-inch Newtonian Reflecting Telescope. Royal Observatory,
Edinburgh cut to face page 72
The Transit Circle, Royal Observatory, Edinburgh . cut to face page 74
The Experimenting Room, Royal Observatory, Edinburgh ....
cut to face page 76
Very Bright Meteor, March 4, 1898, by H. D. Curtis 79
Elements and Ephemeris of Comet b 1898 (Perrine), by R. T.
Crawford and H. K. Palmer 79
North Front of the Royal Observatory, Edinburgh . cut to face page 81
Notices from the Lick Observatory 8r
A Lunar Landscape, photographed at the Lick Observatory.
J. M. S. and C. D. P 81
The Lick Observatory Eclipse Expedition, from letter by
W. W. Campbell 8r
The Companions to Atdebaran, R. G. A 85
A Remarkable Object. T. E. Espin 85
Request for Observations of Comet 1896 L C. D. P 83
A Dayhght Meteor. Chas. Pixlev 84
Missing Books. Library Committee 84
Election of Professor James E. Keeler as Director of the Lick
Observatory. R. G. A 85
Library Notice. Publication Committee 85
Discovery of Cometh 1898 (Perrine). C. D. P 85
Elements of Comet* 1898 (Perrine). W. J. H 86
Astronomical Society of the Pacific. v
Pagh
Astronomical Teleg:ram : Discovery and Observation of Comet
b 1898, by C. D. Perrine 86
Astronomical Telegram : Observation of Comet b 1898, by
W.J. HussEY 86
Astronomical Telegram: Observation of Comet b 1898, by
C. D. Perrine 87
Astronomical Telegram : Elements and Ephemeris of Comet b
1898, by W.J. HussEY and C. D. Perrine 87
Erratum 87
The Crawford Library, Royal Observatory, Edinburgh . . .
cut to face page 89
Minutes of the Special Meeting of the Directors, November 27^ i8g8. 89
First Award of the Bruce Medal 89
Minutes of the Meeting of the Directors^ March 26 ^ j8g8 90
List of Members Elected . 90
Report of Committee on the Library 90
Minutes of the AnnucU Meeting (Adjourned) of the Society, April 2,
1898 91
Directors Elected 91
Report of Committee on Comet-Medal, March 26, 1898 .... 91
Annual Report of Treasurer, March a6, 1898 92
Minutes of the Meeting of the Directors, April 2, i8g8 94
Officers Elected 94
Appointment of Standing Committees 94
Officers of the Society, etc 95
The Spectroscope Attached to the 15-inch Refractor of the Royal
Observatory, Edinburgh cut to face page 96
Publications No. 62, June i, 1898.
The Solar Corona of January 22, 1898 cut to face page 97
On the Causes of the Sun's Equatorial Acceleration and the Sun-Spot
Period, by E. J. Wilczvnski 97
The New Atlas of Variable Stars, by the Rev. Father J. G. Hagen.
S.J 100
Observations of o Ceti (Mira), 1897-98, by Rose O'Halloran ... 103
Honor Conferred on Professor Schaeberle 104
The Red Stars V Hydra and 277 of Birmingham's Catalogue, by
Rose 0*Halloran 105
A New Astronomy for Beginners, by David P. Todd. Review by
W. J. HussBY 106
Planetary Phenomena, for July and August, 1898, by Professor Mal-
colm McNeill 108
Twenty-ninth Award of the Donohoe Comet-Medal to Mr. C. D.
Perrine in
Notices from the Lick Observatory 113
Photograph of the Total Eclipse of the Sun, January 22, 189S . 113
Changes in the Staff of the Lick Observatory 113
vi Publications of the
Pack
Electric Illumination of the Micrometer at the Lick Observatory.
W.J. H 113.
The Lowell Observatory Catalogue of Double Stars. R. G. A. 114
Changes in the American Ephemeris. R. G. A 115
Solar Observations in 1897. R. G. A 116
New Elements of Comet ^ 1898. C. D. P 116
Elliptic Elements of Comet b 1898, and a Certain Similarity to
the Comets of 1684 and 1785 L C. D. P 117
Cometary Discoveries. W. F. Denning 11&
The Variable Stars Z Ceniauri and the Nebula N. G. C. 5253.
W.J. H 119
"A Remarkable Object in /Vr^^w^.'* E. F. C 120
A Correction. J. M. Schaebbrlb 120
Recent Changes in the Double Star 02 341. W. J. H 121
New Elements of Cometh 1898! Perrine). W.J. H 122
A New Large Nebula in Ursa Major, E. F. C 123.
The Rumford Medal. From Science 123
Stellar Parallax. R. G. A 124
Erratum ^ 124
Minutes of the Meeting of the Directors, June tt, j6g8 125
List of Members Elected 125
Minutes of the Meeting of the Society, June J t^ iSgS 125
Officers of the Society, etc. 1 26
Publications No. 63, August i, 1898.
General View of the Lick Observatory Eclipse Camp, near Jeur,
India, January 22, 1898 cut to face page 127
A General Account of the Lick Observatory-C rocker Eclipse Expe-
dition to India, by W. W. Campbell 127
The Lick Observatory Eclipse Station. Half an Hour After To-
tality cut to face page 134
The Influence of Physiological Phenomena on Visual Observations
of the Spectrum of the Nebulae, by James E. Keeler 141
Wolf's Periodic Comet, by W. J. Hussey 144
Comet c 1898 (CoDDiNGTON), by E. F. Coddington 146
Discovery Plate of Comet Coddington cut to face page 146
Planetary Phenomena, for September and October, 1898, by Profes-
sor Malcolm McNeill 149
Notices from the Lick Observatory 153
The November Meteors, from H. C. O. Circular No. 31 ... . 153
Discovery of Comet e 1898 (Perrine). C. D. P 155
Errata in Star Catalogues. C. D. P 155
Two Bright Meteors, June 24 and June 29, 1898. C. D. P. . . . 156
Comet c 1898 (Coddington) 157
Elements of Comet e 1898. C. D. P. and R. G. A 157
Elements of Comet ^ 1898 (GiACOBiNi). W. J. H 157
Elements of Comet ^ 1898 (Perrine). C. D. P 158
Fellowships at the Lick Observatory 158
Astronomical Society of the Pcuific. vii
Page
The Large Refractors of the World, from The Observatory . . 158
Astronomical Telegrams : Discovery and Observations of
Comet c 1898 (Coddington) 160
Astronomical Telegram: Ritchie. Discovery of Enckb's
Comet by; Tbbbutt . * 160
Astronomical Telegrams : Discovery and Observations of
Cometh 1898 (Pbrrinb) 160
Astronomical Telegram : Discovery of Wolf's Comet by
W. J. HussEV 161
Astronomical Telegrams : Elements and Ephemeris of Comets
e 1898 (Pbrrine), and c 1898 (Coddington) 161
Astronomical Telegram : Ritchie. Observation of Comet /
1898 (GiACOBiNi) 162
Astronomical Telegram : Ritchie. Elements and Ephemeris
of Comet g 1898 (GiACOBiNi), by Krbutz 162
Independent Discovery of Comet r 1898 162
Conference of Astronomers and Physicists 162
Obituary Notice of William Augustus Rogers, by Arthur
Searlb, from Astronomische Nachrichten^ No. 3499 163
Officers of the Society, etc 165
Publications No, 64. October i, 1898.
The Temperature of the Sun (I), by Professor Dr. J. Scheinbr.
Translated from the German, in Himmel und Erde, by Fred-
erick H. Seares 167
New Observations of the Otto Struve Double Stars, by W. J.
HussEV 180
Motion of 1; Cephei in the Line of Sight, by W. W. Campbell ... 184
Thirtieth, Thirty-first, and Thirty-second Awards of the Donohoe
Comet-Medal to Messrs. E. F. Coddington, C. D. Pbrrine, and
E. Giacobini 185
Planetary Phenomena, for November and December, 1898, by Pro-
fessor Malcolm McNeill 186
Notices from the Lick Observatory 191
New Gases in the Earth's Atmosphere. R. G. A. . . . . 191
The Minor Planet (334) Chicago, W. J. H. . . 192
The New Minor Planet, 1898 D Q. W. J. H 194
Discovery and Orbit of Comet A 1898 (Pbrrine). C. D. P. . . 194
New Elements of Comet h 1898. C. D. P 195
Elements of the Minor Planet, 1898 D Q. W. J. H 196
Astronomical Telegram : Ritchie. Orbit of Minor Planet, 1898
DQ 197
Astronomical Telegrams : Discovery and Observations of
Comet b 1898 (Pbrrine) 197
Astronomical Telegram : Ritchie. Discovery of a Comet by
Pbchulb 197
Astronomical Telegram : Ritchie. Pbchule*s Comet is
Wolf's 198
viii Publications of the
Astroaotnical Telegram : Ritchie. Uacertatnty in L. O. tele-
gram, September 14, 1898 198
Astronomical Telegrams : Observation, Elements, and Epbem-
eris. Comet b 1897 (Perrine) 198
The Perseid Shower of 189a C. D..I* 198
Elemehtsof Cometh 1898 (Perrine). C. D. P 199
Obituary Notice of Dr. Hermann Romberg aoo
Minutes of the Meeting of t9u Directors, Septemifer j, 1898 k>i
List of Members Elected 201
Minutes 0/ the Meeting 0/ the Society, Septemtfer J, £898 aoi
Officers of the Society, etc 20a
Ptibluations No. 65, December i, 1898.
The Bruce Gold Medal cut to face page J03
A General Acc6unt of the Chabot Observatory-PiERSON Edipse
Expedition to India, by Charles Burckhalter 203
Camp PiERtoN, near Wangi, India cut to face page 206
The PiERsoN Photographic Telescope, as mounted in India ....
cut to face page 208
The PiERSON Telescope; with the Pardee Lens and Tube Attached
cut to face page 21a
The '* Eye-End ** of the Pierson Telescope .... cut to Dace page 212
The Development of Photography in Astronomy, by Edward E.
Barnard (Abstract) 213
The Surface of the Sun, by Rose 0*Hallor AN 222
The Temperature of the Sun (U), by Professor Dr. J. Scheiner
(translated from the German, in Himmel und Erde, by Fred-
erick H. Seares) ... 224
Planetary Phenomena for January and February, 1899, by Professor
Malcolm McNeill 235
Notices frofn ike Ltc/i Observatory 239
The Leonids of 1898. C. D. P . . 239
The Leonid S\\oyN^x in 1898. R. G. A 241
The Leonids in 1898. H. D. Curtis 242
Family Likeness of the Comets 1 1898 (Brooks) and 1881 IV
(Schaeberle). W. J. H 243
The Small Bright Nebula near Merope. J. E. K. 245
The Motion of the Pole. R. G. A 246
Tiajeclory of the Pole (from A stronomicat Journal, No. 446) . . 247
The Harvard Conference of Astronomers and Physicists . . . 249
Helium in the Earth's Atmosphere. R. G. A 249
The Telescope for the Paris Exhibition of 1900 249
A New Algol Variable (from Science Observer, Specigl Circular,
No. 122) 249
Resemblance of the Orbit of Brooks's Comet (j 1898) to that of
ScHAEBERLE'sCometof 1881 (1881 IV). C. D. P. 250
. Astronomical Telegram: Ritchie, Discovery of Brooks's Comet 250
Astroiiomical Telegrams: Observations and Elements of
Bkooks's Comet 250
Astronomical Society of the Pacific. ix
Page
Astronomical Telegram: Perrinb finds Resemblance between
Elements of Brooks's Comet and those of 1881 IV .... 351
A New Gas. R. G. A 251
Photographs of Comet t' 1898 (Brooks). J. E. K 353
Erratum 353
Minutes of the Meeting of the Director Sy November 26^ iSg8 354
List of Members Elected 354
Report of the Special Committee on the Bruce Medal 354
Minutes of the Meeting of the Society^ November 26^ iSg8 356
Officers of the Society, etc 357
General Index to Volume X 359
PUBLICATIONS
OF TH B
Astronomical Society of the Pacific.
Vol. X. San Francisco, California, February i, 1898. No. 60.
LIST OF MEMBERS
OP THE
ASTRONOMICAL SOCIETY OF THE PACIFIC.
January i, 1898.
OFFICERS OF THE SOCIETY.
Mr. William Alvord (Bank of CaUfornia, S. F.) Prtiident
Mr. E. J. MoLSRA <6o6 Clay Street, S. F.) v
Mr. Frbdbrick H. Sbakbs (Berkeley, Cal.) ..... > Vice-Prtxidenti
Mr. C. M. St. John (IJ. S. Custom Hou&e, S. F.) '
Mr. C. D. Pbrrinb (Lick Observatory) Secretary
Mr. F. R. ZiBL (301 California Street, S. F.) . . Secretary and Treasurer
Board of Directors— Messn. Alvord, Molbra, Morke, Miss O'Halloran, Messrs.
Pbrrinb, Pibrson, Skarbs, St. John, Tuckrm, von Gbluern, Zibl.
Ftmamce Committee— Kessn. Wm. M. Pibrson, £. J. Molbra, and C. M. St. John.
Committee oh Publication — Messrs. Aitkbn. Babcock, Searbs.
Li^ary Committee— MessTt. Hvsany and Sbarbs and Miss O'Halloran.
Committee on the Comet^Afedai—Mtssn. Schabhbrlb and Campbbi.l.
OFFICERS OP THE CHICAGO SECTION.
Executive Committee— Mr. Ruthvhn W. Pikb.
OFFICERS OF THE MEXICAN SECTION.
Executive Committee— Hit, Francisco Rodriguez Rbv.
LIST OP MEMBERS.*
Mr. Carl H. Abbott 118 nth St., Oakland, Cal.
Prof. R. G. AiTKEN {^^tiS'''^''''^' ^'' """""■
Mr. J. H. Albert Salem, Oregon.
Prof. W. Steadman Alois, *f.r.a.s. . { ^^^^S^^"' near Oxford, Eng-
Prof. W. D. Alexander Honolulu, Hawaiian Islands.
Mr. Richard H. Alle.n* Chatham, Morris Co., N. J.
Mr. CHAKLHS A UTSCHUL { Xt"' s'T Cal/"'"""
* A star signifies Life Membership. Total membership, 349 (75 life members. )
y
2 Publications of the
Hon. Henry B. Alvord* San Jos^, Cal.
Hon. William Alvord* 2200 Broadway, S. F., Cal.
Mrs. William Alvord* 2200 Broadway, S. F., Cal.
Miss Kate Ames Napa, Cal.
Mr. W. S. Andrews Schenectady, N. Y.
Mr. F. S. AKCHSSHCO { ^TB^erirG^rany.
Mrs. Wm. Ashburner 1014 Pine St., S. F., Cal.
Mr. J. J. A.B«T.N.. P.K.X.S { ''^^^^^)-^^T' ^- ^-
Mr. Allen h. Babcock 12 14 Webster St., Oakland, Cal.
Mr. Walter C. Baker { '"^Ohio."''^*'^ ^^""^ Cleveland.
Mr. N. A. Baldwin New Haven, Conn.
Mr T Racssktt i ^^ ^*^^ ^^^ ^^^^^ Newington,
Mr. J. BASSETT j j^ England.
Miss Frances L. Beans 489 N. First St., San Jos^, Cal.
Mr. Henry Berger { Oteervatory Hill, Allegheny.
Mr. John Bermingham* 330 Market St., S. F., Cal.
f American Museum of Natural
Prof. Albert S. Bickmore -! History, Central Park, New
I York. N. Y.
Prof. Frank H. Bigelow { ^ington? D^ C. ^"'''^"' ^^^^^
Mr. Wilbert M. Birge Davenport, Neb.
Mr. R. L. Bischoffsheim,* F.R.A.s. . . 3 Rue Taitbout, Paris, France.
Mr. Charles R. Bishop Occidental Hotel, S. F., Cal.
Mr. Thomas B. Bishop* 532 Market St., S. F., Cal.
Mr. Anson Stiles Blake Berkeley, Cal.
Mr. Charles T. Blake Berkeley, Cal.
%jf- u„^.«,, T ^«^ D^.t.^^v, T.. «. » A o (Caracas, Venezuela, or Box
Mr. Henry Lord Boulton, Jr.,*F.R.A.s. | ^^^^^ ^^^^ york, N. Y.
Dr. J. T. Boyd i 76 E. Ohio St., Indianapolis,
Colonel E. D. Boyle Gold Hill, Storey Co., Nev.
Mr. Frederick E. Brasch Stanford University, Cal.
Mr. J. A. Brashear, f.r.a.s Allegheny City, Pa.
1?*., VI c n».^i^.^AK, J St. Lawrence's Church, St.
Rev. M. S. Brennan j ^ouis. Mo.
Rev. A. L. Brewer San Mateo, Cal.
Mr. Edward M. Brewer 27 Kilby St , Boston, Mass.
f Hope Bank, Nelson St., Wool-
Mr. Joseph Brooks, f.r.a.s., f.r.g.s. -{ lahra, via Sydney, New South
I Wales,
col. ALEX. BUKTON-BROWS.R.A....R.A.S. {^^eoj-ge^s^^Club.^^^^^^^^^^
Miss E. Brown* { ^ England"'*""' *='''^"*=*''*''-
Miss C. W. Bruce* 8to 5th Ave., New York, N.Y.
Mr. Charles Burckhalter, f.r.a.s. {^^^^^ c^h'"'''"'**"'^' ^''^'
Astronomical Society of the Pacific. 3
Miss MXKV E. BvK. {■'^e^S'KrptotMaS:*'-
Dr. J. Callandreau* 114 Montgomery St., S.F ,Cal.
Prof. W. W. Campbell -f Li^rk Observatory. Mt. Hamil-
( ton, Cal.
Mr. Andrew Carnegie* 5 West 51st St., New York, N.Y.
Mr. J. C. Cebrian* { ^ Cal^""^ '^^'''^'^ ^^" ^' ^"
Dr. V. Cerulli | Observatorio Privato, Teramo,
Mr. B. G. Clapp The Academy. Fulton, N. Y.
Dr. E. S. Clark 16 Geary St.. S. F., Cal.
Miss Isabella D. Clakk Sanjos^, Cal.
Mr. Mateo Clark* {"^ESnd." ^''*^' ^"*^°"'
Miss Agnes M. Clerke {^E^|faid^* ^"''"'' ^°"*'''"'
Mr. Ernest A. Cleveland Vancouver, B. C.
Mr. E. F. CoDDiNGTON {^to^n^C^''''''^^ ^^' "''"'*'"
Mr. A. L. CoLTON* Box 1314, Ann Arbor. Mich.
Mr. J. Costa 1 14 Montgomery St., S.F., Cal.
Mr. Henry CowELL* 413 Hyde St., S. F., Cal.
Mr. Hugh Craig 312 California St., S. F., Cal.
Mr. Walter Cramp j "delK^'pa."'''''^ ^^" ^*'"^"
Mr. George Crocker* Mills Building:, New York, N.Y.
Mr. Henry J. Crocker 508 California St., S. F., Cal.
Mr. William H. Crocker* j ^'g^Jj^y'^^'ll^cT ^^''''"''^
Mr. Edward Crossley,*f.r.a.s. . . { ^^f^^g^Ja^^'^^^^^
Miss's. J. Cunningham { ^ w^'reTo^, Pa."''^''' ^^^''"
Mr. Chas. S. Cushing 920 Linden St.. Oakland. Cal.
TM^ T i7««f.7i^ rkAif.r.c^xT* 3 Alexandra Plantation, Brans-
Mr. J. EwEN Davidson* ^ combe, Mackay, Queensland.
Mr. Joseph E. Davis 154 Beacon St.. Boston, Mass.
Mr. William T. Dawson Etna, Siskiyou Co., Cal.
Mr. C. W. Dearborn { "^'ilSfn^ar' ''^""^'
Mrs. John H. Devereux { ^^hfo"''"** ^''*' ^'*''^'*"*''
Mr. W. H. Devinb* Nagasaki, Japan.
Miss Grace H. Dodge { '^YoK*"y. ^"^""^^ ^**
Mr. John Dolbeer lo California St., S. F., Cal.
Mr. W. E. Downs Sutter Creek, Amador Co., Cal.
Mrs. Anna Palmer Draper* .... | ^ri^Madison Ave.. New York,
Rev. W. Arthur Duckworth, j. p. . { ^STEnJland!'''*""*' ^'"*"
4 Publications of the
Mr. Francis G. Du Pont Wilmington, Del.
Mr. H. DuTARD* 2616 Buchanan St., S. F., Cal.
Mr. Earnest I. Dyer 1383 Alice St., Oakland, Cal.
Miss S. J. Eastman Ogontz School, Pa.
Mr. GEO. M. EDGAR ^SrALb^n,?.- """"''"^
Mr. Geo. W. Edwardes {"k^'"'' °'^"^* ^'" ^^"^
Prof. George C. Edwards Berkeley, Cal.
Mr. HENRV EICHBAUM {3 ^I'^^flt^-^^l^l
Capt. Oliver Eldridge 615 Sutter Si., S. F., Cal.
Mr. J. W. Erwin C'c^l.^"'*"' ^''*- ^^^'^^'^y-
{Puisne Judge, Supreme Court,
Pietermaritzburg, Natal,
South Africa.
Mr. S. Wilson Fisher 1502 Pine St., Philadelphia, Pa.
Mr. Andrew B. Forbes* 401 California St., S. F., Cal.
Mr. GEO. STUART FORBES j ^„^k^;"/-„S"l,L^°y,I„^!
Mr. Arthur W. Foster* 322 Pine St., S. F., Cal.
Mr. C. L. Foster 601 Polk St.. S. F., Cal.
Mr. H. C. Frick* 42 5th Ave., Pittsburgh. Pa.
Prof. Chas. W. Friend Observatory, Carson, Nev.
Mr. Robert D. Fry* 1812 Jackson St., S. F., Cal.
Mr. Walter F. Gale, f.r.a.s Paddington, Sydney, N. S. W.
Mr. Jos. F. Gassmann 318 Montgomery St., S. F., Cal.
Miss GEAROK {"'ko^l.^lSjk.'l^S!''
Mr. Otto von Geudern | Room 56. 819 Market St., S.F.,
Mr. Louis Gex Santos, Brazil.
T^^ TA»,r.r. r-,, , ^« «. n * o /Royal Astrouomer, Cape of
Dr. David Gill, c.b., f.r.a.s | J^^^ ^ope, Africa.
Mr. Allen F. Gillihan 2420 Fulton St., Berkeley, Cal.
Mr. George Gleason, j. p { ^°Ca . Cat**'"''' ^' "^"^^'^
Mr. James Monroe Goewev { ^^^|,.*"** ^^"» ^'^- ^- ''••
Capt. Charles Goodall* {^fts^S.'R.'^cS'''*"**^*"*
xA^ Ar..., nr..^.^ /N- E. cor. Bush and Sansome
Mr. Adam Grant* j gts., S. F., Cal.
x>T* T^^^«., rk ^oAi.*^* i N- E. cor. Bush and Sansome
Mr. Joseph D. Grant* j gts., S. F., Cal.
Mr. Albert Edward Gray Lasata,Oroville, Butte Co., Cal.
%# A.,^««,., i-„„.^» f 3 Duntrune Terrace, Broughty
Mr. Andrew Greig* |^ p^^y^ Dundee, Scotland.
Sir George Grey,* k.c.b Auckland, New Zealand.
Mr. C. P. Grimwood 214 Pine St., S. F., Cal.
r> u i-« ..^»., i-.»,.,^r»oo ^ « - - . o i Cliff House, Curbar, via Shef-
Rev. H. Grattan Guinness, d.d., f.r.a.s. j ^^j^^ England.
Astronomical Society of the Pacific. 5
Mr. J. O'B. GuNN Box 2128, S. F., Cal.
Miss EsTELLA L. Guppv San Jos^, Cal.
Mr. W. C. GuRLKY Marietta, Ohio.
Mr. David E. Hadden Alta, Iowa.
-M^ \M vk Uai^%</m^ /U. S. Weather Bureau, Mills
Mr. W. H. Hammon | Building, S. F., Cal.
Mr Hfvrv Harrison f Maudeville Ave.. Jersey City
Mr. HENRY HARRISON | Heights. New J crsey.
Mr. Jackson Hatch Porter Building, San Jos^, Cal.
Mr. L. L. Hawkins 268 Oak St., Portland, Oregon.
Mr. Robert Y. Haynb, Jr San Mateo, Cal.
Mrs. Phebe Hearst f Room 33. 9th floor. Mills BuUd-
i ing, S. F., Cal.
Mr. ANDKBW p. HKNKEL { ^'^iSatf OhS^'""* ""''•
Mr. David Hewes Occidental Hotel, S. F., Cal.
Mr. George V. Hicks 532 California St., S. F., Cal.
Prof. Alfred Higbie | S.W.wr^Kerce and Pine Sts..
Hon. Henrv E. Highton 1 4th,floor, Mills Building, S. F.,
Mr. Chas. B. Hill 212 Pine St., S. F., Cal.
Mr. Horace L. Hill* 124 Sansome St., S. F., Cal.
Mr. Samuel V. Hoffman,* f.r.a.s. . { "^jjf "^'""^ A*«- Mo"«stown,
Mr. Charles W. Holden 30 Congress St., Boston, Mass.
Dr. E. S. Holden,* Foreign A.soc.R.A.s.{Sm^JhsonianI^nstitution,^^^
Mr. S. E. Holden Napa, Cal.
Hon. Jambs F. Houghton 223 Mission St., S. F., Cal.
Hon. C. Webb Howard* Pacific-Union Club, S. F., Cal.
Mr. Wm. Howat* {^'vicSi*!" ^'■* ^*"'°"™*'
Mr. Wm. Rumford Howell .... J43^^WaInut St. Philadelphia,
Prof. W. J. HussEY {^to^n^fih"''''*''^' ^*- "*""""
Mrs. M. H. HUTTON \ '* ""'»" ^t- New Brunswick,
< New Jersey.
Imperial Observatory {"ruISI? ""' ^'" ^^'*'^''"'^'
Mr. O. H. Ingram Eau Claire, Wisconsin.
Mr. Frank Jaynes {W^U; Telegraph Co.. S. F.,
Mr. Nels Johnson Manistee, Mich.
Prof T E Kerler f r a s \ Director Allegheny Observa-
rrot. j. li. KEBLER, F.R.A.S ^ ^^^^ Allegheny City, Pa.
Mr. Charles C. Keeney* 2220 Clay St, S. F., Cal.
Prof. JosiAH Keep j Mi^s College, Alameda Co.,
Mr. A. Keith Riverside, Cal.
Mr. James R. Kelly 309 Leavenworth St., S.F., Cal.
6 Publications of the
Mr. JOH« W. KB..K.CK j ^a?ov^?,.'irnL%rMS
Mr. DONALD K..O { « ^^l E^aid."""^'''
Mr. SvoNKV T. KLH.N.- P.K.X.S. . . . { Ote^,S: inTunr"*"*'
Dr. Dorothea Klumpke jr NaUona^ Observatory. Paris.
Mr. ToRVALD KoHt* Odder, Denmark.
Mr. Fr. Koeppbn {^'^TOfny*!^* '' ^''''"' ^^'
Prof. H. Kreutz Stemwarte. Kiel, Germany.
Mr. C. F. DE LANDERO- {P-^^^- ^,P-h-. state
Mr. Walter W. Law Briar Cliff. Scarborough, N.Y.
Miss Hannah Townsbnd Lawrence . Bayside, Long Island, N. Y.
Hon. MANUEL FERNANDEZ LeAL . . . j ^'^^^^l, '^^^^:^^,^^^ 3.
Prof. F. P. Leavenworth { ^ n^^lU, MiSIil""^^' ^'^
Prof. Joseph Lb Conte, ll. d Berkeley, Cal.
Rev. Edmund Ledger, m.a., f.r.a.s. . Claydon, Ipswich, England.
Prof. D. A. Lehman Berea, Ohio.
Mr. Clarence Mackenzie Lewis* . . 104 E. 37th St., New York, N.Y.
^'TAT^Jor. ^I" ^"l"^" .""^ E;^"-} Washington, D. C.
California State Library Sacramento, Cal.
Library of the Chabot Observatory . Oakland, Cal.
The City Library Lowell, Mass.
Free Public Library Newark, New Jersey.
Free Public Library Worcester, Mass.
Library OF THE LELi»ND Stanford Jr. / c*o«f,>^^ tt«:..^«,u„ n^\
University [Stanford University, Cal.
Library of the Lick Observatory . Mount Hamilton, Cal.
Library OF THE Mechanics* Institute . 31 Post St., S. F., Cal.
The Newberry Library Chicago, 111.
New York Public Library j 40 Lafayette Place, New York,
Library of the Observatory .... Georgetown College, D. C.
Library of Princeton University . . Princeton, New Jersey.
The Public Library Boston, Mass.
Library of St. Gertrude's Academy . Rio Vista, Cal.
Library of the University of Cali- \ o^^i,^i^ ^ •
fornia [Berkeley, Cal.
Library of the University of)^.^^^,.^ fii:„^:^
Illinois | Champaign, Illmois.
Library of the University ofXr. ^^. .^„ t«^;««,
Indiana / Bloomington, Indiana.
Library of the University of Penn- 1
sylvania
' I Philadelphia, Pa.
Astronomical Society of the Pacific. 7
Library of Yale University .... New Haven, Conn.
Mr. Adolph Lietz 422 Sacramento St., S. F., Cal.
Mr. J. A. LiCHTHiPE . 15 First St., S. F., Cal.
Mr. John D. Locke Haverhill, New Hampshire.
Mr. Henry B. Loomis Seattle, Washington.
{Director of the McMillin Ob-
servatory, Ohio State Uni-
versity, Columbus, Ohio.
Mr. Edward G. Lukens -200 Market St., S. F., Cal.
Mr. Geo. Russell Lukens 1350 Madison St., Oakland, Cal.
Mr. Frank E. Lunt | Ca^eR. G. Lunt, Los Angeles,
Miss Agnes M. Manning 12 15 Suiter Street, S. F.,Cal.
Mr. Marsden Manson, c.e., ph.d. . { ^So^ c"!^*''^^^'' ^'''''^'
Mr. F. Martens {^^li^eTvo^k!'* ^"'^"'' ^''"
Mr. Camilo Martin { S^^.^S.fI.^Si^
Hon. E. S. Martin P. O. Box 75, Wilmington, N.C.
{Puruatanga, Martinborough,
Wairarapa, Welhngton, New
Zealand.
Mr. Louis C. Masten 2218 Clay St., S. F., Cal.
D-^r A \n iLf..n^^^i.T ) Scott Observatory, Parkville,
Prof. A. M. Mattoon j Missouri.
m>r. \ir u vr.,.,« » » ^ o i i8 Addison Road, Kensington,
Mr. W. H. Maw,* f.r.a.s ] London, England.
ilm i7«.^,^ iLT^i-. ».^, » w . »o * o f Rusthall House, Tunbridge
Mr. Frank McClean.* m.a.. f.r.a.s. | ^^,jg^ England.
Mr. F. H. McCoNNELL 19 Montgomery St., S. F., Cal.
Mr. John McDonough 193 28th St, Brooklyn, N. Y.
r South Alabama Baptist In-
Prof. J. M. McIvER \ stitute, Thomasville, Ala-
( bama.
Prof. Malcolm McNeill Lake Forest, 111.
Hon. Albert Miller* 532 California St., S. F., Cal.
r^ e ^ X* .« /University of Kansas, Law-
Prof. E. Miller | ^^^^^ ^Kansas.
Hon. D O. Mills* 15 Broad St., New York, N.Y.
Dr. Lewis F. Mizzi Constantinople. Turkey.
Mr. James K. Moffitt First National Bank, S. F.,Cal.
Mr. E. J. Molera.* c.e 606 Clay St.. S. F., Cal.
^m iir u o xn^^.r.^ «. « * ^ J i^ Earlsfort Terrace, Dublin,
Mr. W. H. S. MoNCK, f.r.a.s { Ireland.
-^ . ^ , , _„ i Quezaltenango, Guatemala,
Dr. Jorge C Monzon {'' Central America.
Mr. Beverly K. Moore . . 56 Bedford St., Boston, Mass.
Mr. Fremont Morse, u.s.c.&g.survev . P. O. Box 2512, S. F., Cal.
-, -,, c? m# /Turk St., bet. Masonic and
Mr. William S. Moses | Parker A ves., S. F., Cal.
Mr. C. A. MuRDOCK 2710 Scott St., S. F., Cal
8 Publications of the
Hon. B. D. Murphy* San Jos^, Cal.
Mr. Charles Nelson 6 California St., S. F., Cal.
Mr. H. F. NKWALL.. P.R.X.S { °Sb^S^e? 'SnT"'*^'
Mr. G. W. NicoLLS. f.r.a.s. . . . . { ^^^l^^' **'** ''* J""'*"*'
Mr. P. NooRDHOFF Groeningen, Holland.
Mr. Charles Nordhoff Coronado, Cal.
Miss Rose O'Halloran 2610 Bush St., S. F., Cal.
Miss M. A. Orr j "fngfJnd.^'*^''' Camberley.
Mr. T. S. PALMER {''ifSio.^^t'^'''''^^
General W. J. Palmer Colorado Springs, Colo.
Dr. George C. Pardee 526 Montgomery St., S. F., Cal.
Dr. S. C. Passavant 200 Post St., S. F., Cal.
Mr. Edward Payson San Mateo, Cal.
Miss Clara A. Pease High School, Hartford, Conn.
Mr. George W. Percy { ^'LTc^^'"* ^^^''^' ^^^'
Hon. Geo. C. Perkins* Oakland, Cal.
Prof. H. B. Perkins Box 240, Pasadena, Cal.
Mr. A. Perrenod Saint-Pierre, Martinique.
Mr. C. D. PBKK.NH {^e'r^:^forM;:Hlllit2l:
Hon. T. Guy Phelps Belmont. Cal.
Mr. Henry Phipps. Jr.* |Camegie,^Phipps & Co., Pitt^
Mr. Sam C. Phipps Irvington, Alameda Co., Cal.
Mr. John Jay Pierrepont { ^ K^n"^ C^o.! R Y.' ^''^^^^'''
Mr. Lawrence H. Pierson jPacHic Pine Lumber Co., S.F..
Hon. Wm. M. Pierson, f.r.a.s. . . . j ^^^^J^^''' Mills Building, S. F.,
Mr. RuTHVEN W. Pike* 166 La Salle St., Chicago, III.
Mr. Fred. G. Plummer Tacoma, Washington.
Dr. Charles Lane Poor, f.r.a.s. . . {J'^Baltimo^e^'' M^^ University,
Miss Juliet Porter* 37 Dean St., Worcester, Mass.
Mr. Charles A. Post Bay port, Long Island, N. Y.
Mr. Walter A. Post Newport News, Va.
Mr. Wm. Appleton Potter 39 W. 27th St, New York, N.Y.
Mr. Enos Putman* Grand Rapids, Michigan.
Mr. J. C. RABE ) ^v^ile^orc^al." ^"* '"'"*''
Mr. F. B. Randall, u.s.r.m | " Cal!^^^' ^*''- "R'«h."S.F..
Sister Anna Raphael { ^ jUsf cil.^"''* °^"*' ^"
Mr. Albert Raymond ao2 Sansome St., S. P., Cal.
Mr. NoKMAN B. Ream 1901 Prairie Ave., Chicago, III.
Astronomical Society of the Pacific. 9
Prof T K Rrr<; F R A «5 I Observatory of Columbia Col-
Frof. J. K. KEBS, F.R.A.s I ,^g^ ^^^ y^^^^^ ^ Y
Colonel C. McC. Reeve {^'rpS"S^ ^' ^" ^*""''"
Mr. M. Rbiman {4325 Drexel Boulevard, Chi-
l cago, HI.
Mr. Francisco Rodriguez Rev . . . { ^ bay"? Mexfc^^^^ ^''''""
Rev. J. L. RiCARD, s. J Sania Clara, Cal.
Mrs. William Gorham Rice Washington, D. C.
Mr. DAMEU S. R.CHARr«ON j ^"SasVoatunSf !r™'^^'
Mr. A1.EXANDBR W. Roberts .... { '"i^^jd.*^^*'' "**^' ^*'*' ^*'°*"
Hon. Arthur Rodgers Nevada Block, S. F., Cal.
Mrs. Arthur Rodgers* | Leavenworth and VallejoSts.,
Dr. W. H. RoLpiNS 350 Marlboro St., Boston.Mass.
Mr. Geo. A. Ross { '"find!' Cal.^''*" ^**' ^''^'
The Earl of Rossb, f.r.a.s {^'ia„d.^"^' P"'***"*'"*'"' ^'«-
Baron Albert von Rothschild* . . . Vienna, Austria.
Mr. John R. Ruckstell 182 Croclcer Bld'g, S. F., Cal.
Mr. Alexander Rvdzewsk, {''^6%^k"?sburgtR^£^
Mr. G. N. Saeomuller { ^Tv^'^I^J^shlnSn. W'
Mr. Joseph C. Sala 429 Montgomery St., S. F., Cal.
Mr. John W. Salsbury Clear Water Harbor, Florida.
Prof. J. M. Schaeberle* { ^t'o^^^CaT''''''''^' ^^' """""'
Mr. Jacob H. Schiff* 932Fifth Ave., New York, N.Y.
Mr. Herman Schussler. ...... . Pacific-Union Club, S. F., Cal.
Baron A. v. Schweiger-Lbrchenfeld { ^^1^"^^^^^^^^ ^3, Vienna,
Mr. Henry T. Scott Box 2128, S. F., Cal.
Mr. JAHES L. Scorr, P.R.A.S { ^¥at"chi!?a°*'* ^ ^°'
Rev. GEORGE M. SEARLE {"^t^^^^^T' '^''''''
Mr. Frederick H. Seares Berkeley, Cal.
Dr. J. M. Sblfridgb Box 37, Oakland, Cal.
Mr. Garrett P. Serviss 8 Middagh St., Brooklyn, N.Y.
Dr. T. STEELE Sheldon, F.R.A.S. . . {^Y^n^j^^' Macclesfield. Eng-
I>r. G. E. Shuey { ^akian'S^Car ^' ^'' "^"^
Mr. D. P. Simons Los Gatos, Cal.
Mr Fr ANri*; Sinplair / ^""^ °^G. S. Gay, Crafton, San
Mr. FRANCIS biNCLAiR | Bernardino Co., Cal.
Mr. Chas. S. Smith* 25 W. 47thSt.,New York,N.Y.
Mr. SoMMBRS N. Smith Newport News, Virginia.
lo Publications of the
Mr. Wm. F. Smith 206 Sansome St.. S. F., Cal.
Mr. C. A. Spreckbls* San Mateo, Cal.
Mrs. C. A. Sprkckels* San Mateo. Cal
Mr. Rudolph Spreckels 2000 Gough St., S. F., Cal.
Miss Gertrude Stanford 1218 Oak St., Oakland, Cal.
Mr. Thos. W. Stanford* { '^^jft^^^^" ^^^ Melbourne,
Dr. Hezekiah Starr {^Md!"^^^"^ ^^" Baltimore,
Mr. John W. Stetson 906 Broadway, Oakland, Cal.
Mr. Robert Stevenson P. O. Box 2214. S. F., Cal.
Mr. H. F. Stivers Hunters, Tehama Co.. Cal.
Mr. Chauncev M. St. John U. S. Custom House, S.F.,CaL
Mr. jcuus STONE. rro.rSnPb'Js^Shr''^"^*
Prof. W. H. VON Streeruwitz . . . . P. O. Box 465, Austin, Texas.
Prof. I. Stringham, ph. d Berkeley, Cal.
Mile. Le Brun DB SuRviLLE 3242 Sacramento St, S.F., Cal.
Mr. Daniel Suter { ^ s! R.^'Sil.^'''''^^" ^"'''*'"^'
Hon. A. Sutro*. j So^Montgomery Block, S. F.,
Mr. C. F. A. Talbot 204 California St., S. F., Cal.
Mrs. Louis Taussig 2127 California St., S. F., Cal.
Mr. Charles Tousey Taylor Kamela, Oregon.
Mr. George Taylor Walnut St., Brookline, Mass.
Dr. Horace H. Taylor Los Angeles, Cal.
Prof. J. M. Taylor State University, Seattle, Wash.
Dr. Jesus Muf5os Tebar Cardcas. Venezuela. S. A.
Mr. JOHN TEBBUTT. F.R.A.S T^S' VaW"""''^ "^'^
Dr. A. Blair Thaw | M on tecito, Santa Barbara Co.,
Mr. L E. Thayer 28 California St.. S. F., Cal.
T\^ T^«i., M Tu^wo* i National Observatory, Cordo-
Dr. John M. Thome* j ^ Argentine Republic.
Mr. D. F. Tillinghast 315 Montgomery Si., S. F., Cal.
Mr Q n TnwNTipv (Astronomical Observatory,
Mr. S. D. Townley j ^„„ ^^.j^^^^ Michigan.
«« t o 1'^...^.^,,^,^ S Stamford Lodge, St. Johns.
Mr. John S. Townsend \ g^^.^^ q^^^^k .£^^,Jj =».
Mr. R. H. Tucker. Jr j ^'fo^„^cir''°'^' ^^ """""'
Mr. Henrv J. Turner* j WoodVjIle, Rappahannock Co..
Miss SARA C.RR UPTON | "^ash^iS'T "c'''*""**
Mr. Edward H. Van Ingen 9 East 71st St., New York, N.Y.
Rev. Jacob Voorsanger 432 Montgomery St, S. F., Cal.
Mr. W. P. Wallheiser Bedford, Indiana.
vr. T \\i WAor. ^ 271 Bourke St.. Sydney. New
Mr. J. W. Ward . . . ^ 'gouth Wales.
Astronomical Society of the Pacific. 1 1
{Care of Warner & Swasey,
East Prospect St., Cleve-
land, Ohio.
Mrs. W. Seward Webb ] ^^.^Y^'^ ^''^""''' New York,
Prof Dr L Weinek ^ Imperial Observatory, Prague,
rroi. i^r. l. weinek ^ Austro- Hungary.
Mr. Chas. J. Welch 1090 Eddy St., S. F., Cal.
President Andrew D. White* Ithaca, N. Y.
ui^ IT. o.B. Uatm^^ ufuf-ro. i Stale Normal School, Valley
Mre. Elsie Hadlev White ] ^j^^^ ^^^^y^ ly^\ioxL
Mr. E. J. White, f.r.a.s ) ^^^^^^^^"""^^ Melbourne, Vic-
Mr. Ralph Radcliffe-Whitehead . . Santa Barbara, Cal.
M, A c^A,.T. »%r \)ir„ « «Aw<, ^ n . o J Bella Vista, Hove Park Villas,
Mr. A. Stanley Williams, f.r.a.s. . \ ^^^ Brighton, England.
Mrs. Mary H. Willmarth* 222 Michigan Ave., Chicago.Ill.
Mr. Russell J. Wilson* 2027 California St., S. F., Cal.
Colonel B. Witkovsky* j ^^44^^^^^' ^' ^' ^
Rev. Henry Woods St. Ignatius College, S F., Cal.
Mr. William Yates j ^^^^ellsi^'cfl'^^''" ^' ^^ ^"'
Mr. Frederick W. Zeile* i Room 26. 5th floor. Mills Build-
\ ing, S. F., Cal.
Prof. C. V. Zenger, f.r.a.s Smichow, Prague, Bohemia.
Mr. F. R. ZiEL 301 California St., S. F., Cal.
LIST OF CORRESPONDING INSTITUTIONS.
Albany, New York, Dudley Observatory.
Allegheny, Pennsylvania, Allegheny Observatory.
Armagh, Ireland, Armagh Observatory.
Berlin, Germany, Redaction des Berliner Jahrbuchs.
Berlin, Germany, Royal Observatory.
Cambridge, England, University Observatory.
Cambridge, Massachusetts, Harvard College Observatory.
Cape Town, Africa, Royal Observatory.
Christiania, Norway, University Observatory.
Cincinnati, Ohio, University Observatory.
Cordoba, Argentine Republic, National Observatory.
Dorpat, Russia, University Observatory.
Dublin, Ireland, Dunsink Observatory.
Dublin, Ireland, Royal Dublin Society.
Edinburgh, Scotland, Royal Observatory.
Geneva, Switzerland, Observatory.
Glasgow, Scotland, University Observatory.
Gotha, Germany, Ducal Observatory.
Goettingen^ Germany, Royal Observatory.
Greenwich, England, Royal Observatory.
12 Publications of the
Hamburg, Germany, Hamburger Stemwarte.
Helsingfors, Russia, University Observatory.
Kasan, Russia, University Observatory.
Kiel, Germany. University Observatory.
Koenigsberg. Germany, University Observatory.
La Plata, Argentine Republic, Observatory.
Leipzig, Germany, University Observatory.
Leyden, Holland, University Observatory.
Lisbon (Tapada), Portugal, Royal Observatory.
London, England, 26 Martin's Lane, British Astronomical Association.
London, England, British Museum.
London, England, Royal Astronomical Society.
London, England, 3 Verulam Bldgs., Gray's Inn, The Nautical Almanac
Lund, Sweden, University Observatory.
Madison, Wisconsin, Washburn Observatory.
Madras, India, Observatory.
Madrid, Spain, Royal Observatory.
Marseilles, France, Observatory.
Melbourne, Victoria, Observatory.
Mexico, Mexico, Sociedad Cientifica **Antonio Alzate."
Milan, Italy, Royal Observatory.
Moscow, Russia, University Observatory.
Munich, Germany, Royal Observatory.
Naples, Italy, Royal Observatory.
New Haven, Connecticut, Yale University Observatory.
New York, New York, American Mathematical Society.
New York, New York, Columbia University Observatory.
Nice, France. Observatory.
Northfield, Minnesota, Carleton College Observatory.
Oxford, England, Radcliffe Observatory.
Oxford, England, University Observatory.
Paris, France, Bureau of Longitudes.
Paris, France, National Observatory.
Potsdam. Germany, Astrophysical Observatory.
Prague, Austro-Hungary, University Observatory.
Pulkowa, Russia, Imperial Observatory.
Rio de Janeiro, Brazil, Observatory.
Rome, Italy, Observatory of the Roman College.
Rome, Italy, Italian Spectroscopic Society.
Rome, Italy, Specula Vaticana.
San Francisco, California, California Academy of Sciences.
San Francisco, California, Technical Society of the Pacific Coast.
Stockholm, .Sweden, University Observatory.
Strassburg, Germany, University Observatory.
Sydney, New South Wales, Observatory.
Tacubaya, Mexico, National Observatory.
Tokio, Japan, University Observatory.
Toronto, Canada. Astronomical and Physical Society of Toronto.
Toulouse, France, Observatory.
Astronomical Society of the Pacific. 13
Turin, Italy, Observatory.
University Park, Colorado, Chamberlin Observatory.
University of Virginia. Virginia, McCormick Observatory.
Upsala, Sweden, University Observatory.
Vienna, Austria, Imperial Observatory.
Vienna (Ottakring), Austria, Von Kuffner*s Observatory.
Washington, District of Columbia, Library of Congress.
Washington, District of Columbia, National Academy of Sciences.
Washington, District of Columbia, Naval Observatory.
Washington, District of Columbia, Smithsonian Institution.
Washington, District of Columbia, The American Ephemeris.
Washington, District of Columbia, U. S. Coast and Geodetic Survey.
William's Bay, Wisconsin, Yerkes Observatory.
Zurich, Switzerland, Observatory.
BXCHANOES.
Adrophysical Journal^ William's Bay, Wisconsin.
Sirius, Cologne, Germany.
The Observatory ^ Greenwich, England.
FOR REVIEW.
[See Publications A. S. P., Vol. VIII, p. loi.J
The CcUly San Francisco, California.
The Chronicle^ San Francisco, California.
The Examiner^ San Francisco, California.
The Mercury^ San Jos6, California.
The Overland^ Monthly y Si^n Francisco, California.
The Record- Union, ^acramento, California.
The Times, Los Angeles, California.
The Tribune, Oakland, California.
MAP I.
i>
f' n
f*.«oj
.0'
J> V
<•>
V
-•»to=
..**•"%'-
«? V
v^
:^
>V^ 9
.(v^^
■r:-:..;:%
■•^.:;-$'.-
M ^
^i
^M^
^y
•ven ■'-?"■:
^ o^
y »
u.
/■■ -^L f^ M*"" i^...i.i i >-<^
/^^/V/^,
^5 "^
y ^
'"^•(/i
^t#
£? f
iT^
.^"i.
''?*/]'«
71*"
-1«»
:•. <
0«i
JS^^i
l.'V-V-^^p
/••
•••i>
•^-f^.-
^/ftI>ANI/A^^
"•'^i.c
The sky on November 22, at 12 o'clock.
December 6, at 11 o'clock.
December 21, at 10 o'clock.
January 5, at 9 o'clock.
January 20, at 8 o'clock.
WM* 31
The sky on January 20, at 12 o'clock.
February 4, at 11 o'clock.
February 19, at 10 o'clock.
March 6, at 9 o'clock.
March 21, at 8 o'clock.
n '
&^
Astronomical Society of the Pacific. 15
A SERIES OF SIX STAR MAPS.
The star maps in this series have been drawn, using those in
Proctor's ^'Half Hours with the Stars'' as a basis. The scale
has been somewhat reduced, in order to accommodate a map to
a page of the Society's Publications,
The making of these maps was originally undertaken by
Professor D. A. Lehman, at Professor Holden's suggestion.
A portion of them remained unfinished at the time of Professor
Lehman's departure from the Lick Observatory, in July, 1897,
and these I have completed.
The maps were originally adapted to a north latitude of about
52°, so that, for the latitudes of the United States, they will be
somewhat in error, but not so much, however, as to cause
serious inconvenience. Under each map will be found the date
and time at which the sky will be as represented in the accom-
panying map; e, g. Map No. i shows the sky as it appears on
November 22d at midnight, December 5th at 11 o'clock, Decem-
ber 2 1 St at ID o'clock, January 5th at 9 o'clock, and January
20th at 8 o'clock. It is presumed that the maps will be used
for observations principally between the hours of 8 o'clock in
the evening and midnight. It should be borne in mind, how-
ever, that the same map represents the aspect of the constella-
tions on other dates than those given, but at a different hour of
the night. Map No. i, which we have been considering, shows
the sky's aspect on October 23d at 2 a. m., September 23d at
4 A. M., and also on February 20th at 6 p. m., as well as on the
dates and at the hours given in the map. The same is true of
all the other maps in the series. For any date between those
given, the map will represent the sky at a time between the hours
given; for instance, on November 26th, Map No. i will represent
the sky at 11:45 o'clock, on November 30th at 11:30 o'clock,
and on December 2d at 11:15 o'clock.
If the maps are held with the center exactly overhead and
the top pointing to the north, the lower part of the map will be
south, the right-hand portion will be to the west, and the left-
hand to the east, the circle bounding the map representing the
horizon. It will be seen from this that each map shows the whole
of the sky visible at these times.
It will be noted that a number of the constellations about the
pole never set, but are always visible in some part of the northern
1 6 Publications of the
sky. As the maps are the projections of a curved surface upon
a plane, there is, of course, considerable distortion, but this will
hardly be confusing.
The names of the constellations are inserted in capitals to dis-
tinguish them, while the names of stars and other data are in
small letters.
The planets are continually changing their places, and hence
are not inserted on the maps which represent the stars for one
year as well as another.
From the Planetary Notes it can readily be told if the brighter
planets — Venus, Jupiter, and Mars (when at his brightest) —
are visible, and in what part of the sky. Saturn can almost
always be told by its steady yellowish light. If it is desired to
locate a planet accurately, a star map giving circles of Right
Ascension and parallels of Declination should be used, and the
place of the planet ascertained from the tables accompanying the
Planetary Notes in these Publications or from any of the nautical
almanacs. It may assist in identifying a planet, to remember
that the planets do not depart widely, north or south, from the
Sun's path — the ecliptic. C. D. Perrine.
Mt. Hamilton, January 7, 1898.
PLANETARY PHENOMENA FOR MARCH AND
APRIL, 1898.
By Professor Malcolm McNeill.
March.
The Sun reaches the vernal equinox and crosses the equator
from south to north on the morning of March 20th, at 6 o'clock,
P. S. T.
Mercury is too near the Sun to be easily seen until near the
close of the month. It is a morning star until March i6th, when
it passes superior conjunction and becomes an evening star. It
moves rapidly away from the Sun, and by the end of the month
sets about an hour and a quarter after sunset. It is quite near
Venus near the close of the month, and passes that planet about
two diameters of the Moon to the north on March 26ih. The two
planets will not be far apart during the last ten days of the
month.
snH*)JkO
%rt..
Air A
ri A«-
,.i-*^
V\M> HI
'ui K
''^Jyr
^^
■:.*.V<'
>.r*.
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-^ V
4^
^» - . - -
0'5>I>L<I.
^ w*
.•--•
••>.."^-*-i
"> <.
i4^
Ik V*^
^•^.
,< \
V
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^l
s^'
p f
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,v^\*.
■■•■<\
<!(?<, H-
V t\
.^^
% >
-V >
^''»...'i^-.
^^*^'
>"
"iV.
The sky on March 21, at 12 o'clock.
April 5, at 11 o'clock.
April 20, at 10 o'clock.
May 5, at 9 o'clock.
May 21, at 8 o'clock.
MM> TV
The sky on May 21, at 12 o'clock.
June 5, at 11 o'clock.
June 21, at 10 o'clock.
July 7, at 9 o'clock.
July 22, at 8 o'clock.
Astronomical Society of the Pacific. 17
Venus is also an evening star near the Sun, too near to be
easily seen until after the middle of the month.
Mars is a morning star, rising about an hour before sunrise.
It has begun to approach the Earth, but will not be near enough
until autumn to be at all conspicuous.
Jupiter is in good position for observation, and is above the
horizon during nearly the entire night. It comes to opposition
with the Sun on March 25th. It retrogrades (moves westward),
about three degrees in the western part of the constellation VirgOy
and at the beginning of the month it is about one degree south
and west of the third magnitude star y Virginis.
Saturn rises earlier than during February, but is not high
enough to be easily seen until some time after midnight. It is in
quadrature with the Sun, that is six hours behind it, on March 2d.
It is nearly stationary, moving very slowly eastward until March
21st, and then a little westward in the constellation Scorpio, north
and east of the first magnitude star Aniares^ aScorpii, and about
eight degrees distant from it. The minor axis of the rings is a
little less than the polar diameter of the planet.
Uranus precedes Saturn about half an hour, and is about
two degrees east and one degree south of the third magnitude
star j8 Scorpii,
Neptune is in the eastern part of Taurus.
April.
Mercury comes to greatest eastern elongation on April loth,
and then sets nearly an hour and three quarters after sunset. It
will be far enough away from the Sun to be easily seen in the
evening twilight until the last week of the month. April is, for
this year, the best month for seeing Mercury as an evening star.
Toward the close of the month it rapidly approaches the Sun,
and comes to inferior conjunction on the morning of May ist.
Venus is also an evening star, somewhat farther from the Sun
than it was in March. It is in the same region as Mercuiy,
somewhat to the west of it, until April i8th, when the planets are
in conjunction again, with Mercury three degrees to the north.
Their distance apart increases rapidly after this.
Mars rises a little earlier in the morning; by the end of the
month about an hour and a half before the Sun. It increases its
apparent distance from the Sun about ^v^ degrees during the
month. On April 30th it passes perihelion.
1 8 Publications of the
Jupiter is still in fine position for observation, rather better
for evening observation than it was during March, as it is well
above the horizon at sunset. It moves westward about three
degrees in the constellation Virgo, and during the middle of the
month is very near the fourth magnitude star 17 Virginis. On
April 1 2th, the time of nearest approach, the planet is only about
half of the Moon's diameter north of the star.
Saturn rises earlier — by the end of the month at a little after
9 o'clock. It is in the constellation Scorpio, and moves about
one degree westward. The rings are about as in March.
Uranus precedes Saturn about half an hour and moves about
the same amount westward. By the end of the month it is about
one degree south and east of the third magnitude star /3 Scorpii.
Neptune is in the eastern part of Taurus.
Explanation of the Tables.
The phases of the Moon are given in Pacific Standard time.
In the tables for Sun and planets, the second and third columns
give the Right Ascension and Declination for Greenwich noon.
The fifth column gives the local mean time for transit over the
Greenwich meridian. To find the local mean time of transit for
any other meridian, the time given in the table must be corrected
by adding or subtracting the change per day, multiplied by
the fraction whose numerator is the longitude from Greenwich
in hours, and whose denominator is 24. This correction is
seldom much more than i". To find the standard time for the
phenomenon, correct the local mean time by adding the differ-
ence between standard and local time if the place is west of the
standard meridian, and subtracting if east. The same rules apply
to the fourth and sixth columns, which give the local mean times
of rising and setting for the meridian of Greenwich. They are
roughly computed for Lat. 40°, with the noon Declination and
time of meridian transit, and are intended as only a rough guide.
They may be in error by a minute or two for the given latitude,
and for latitudes differing much from 40® they may be several
minutes out.
Phases of the Moon, P. S. T.
H. M.
Full Moon, Mar. 8, i 29 a. m.
Last Quarter, Mar. 14, 11 48 P. M.
New Moon, Mar. 22, 12 37 A. m.
First Quarter, Mar. 29, 11 40 p. M.
MM> ^
^>i«>\^nv
ho
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. ^ y
./.'
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.1''
9 ^Qua^
^\^
.<> ^
^ ^.
^A?X|
^IC01\
^•^US ^y.^«^^^
K-^^^
VN>^
The sky on July 22, at 12 o'clock.
Aug^ust 7, at II o'clock.
August 23, at 10 o'clock.
September 8, at 9 o'clock.
September 23, at 8 o'clock.
H^T'\^
'•^
•-••--.
^<i^(\
-f«-
•' '^^V^
\\-
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A«
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>--*
-^o
The sky on September 23, at 12 o'clock.
October 8, at 11 o'clock.
October 23, at 10 o'clock.
November 7, at 9 o'clock.
November 22, at 8 o'clock.
Astronomical Society of the Pacific. 19
T
HE Sun.
1898.
R. A.
Declination.
Rises.
Transits.
Sets.
H. M.
/
H. M.
H.
M.
H.
M.
Mar. I.
22 50
—
7 28
6 37 A.M.
12
12 P.M.
5 47P-M
II.
23 27
—
3 35
6 22 ,
12
10
5
58
21.
3
+
22
6 6
12
7
6
8
31.
40
+
4 17
5 50
12
4
6
18
Mercury.
Mar. I .
22 5
—
14 5
6 16 A.M.
II
28 A.M.
4
38 P.M.
II.
23 12
—
7 13
6 19
II
55
5
31
21.
22
+
I 34
6 21
12
26 P.M.
6
31
31.
I 33
+
10 48
6 20
Venus,
12
57
7
34
Mar. I.
23 4
—
7 31
6 53 A.M.
12
27 P.M.
6
I P.M.
II.
23 50
—
2 33
6 43
12
34
6
25
21.
36
+
2 33
6 31
12
40
6
49
31. I 21 + 7 34 6 20 12 46 7 12
Mars,
Mar. I.
21
10
- 17
30 5 33 A.M.
10 32 A.M.
3 31 P-M
II.
21
41
-15
8 5 16
10 24
3 32
21.
22
II
— 12
31 4 58
10 15
3 32
31.
22
40
- 9 42 4 38
10 5
3 32
Jupiter,
Mar. I.
12
33
— I
52 8 5 P.M.
I 58 A.M.
7 51A.M
II.
12
29
— I
25 7 19
I 14
7 9
21.
12
24
—
54 6 33
12 30
6 27
31.
12
20
—
24 5 43
Saturn.
II 42 P.M.
5 41
Mar. I.
16
43
— 20
26 I 19 A.M.
6 6 a.m.
10 53 A.M.
II.
16
44
— 20
27 12 41
5 28
10 15
21.
16
44
— 20
26 12 2
4 49
9 36
31.
16
44
— 20
24 II 23 P.M.
Uranus,
4 10
857
Mar. I.
16
6
— 20
42 12 44 A.M.
5 30 a.m.
10 16A.M.
II.
16
6
— 20
42 12 5
4 51
9 37
21.
16
6
— 20
41 II 25 P.M.
4 II
8 57
31.
16
5
— 20
40 10 45
3 31
8 17
20 Publications of the
Neptune.
1898.
R. A.
Declination. Rises.
Transits. Sets.
H. M.
*» ' H. M.
H. M. H. M.
lar. I.
5 16
-f 21 43 II 19 A.M.
6 37 P.M. I 55A.M.
II.
5 16
+ 21 43 10 40
5 58 I 16
21.
5 16
+ 21 44 10 I
5 19 12 37
31.
5 17
+ 21 45 9 22
4 40 II 58 P.M.
Eclipses of Jupiter's Satellites, P. S. T.
(Off left-hand limb, as seen in an inverting telescope before opposition, March 2stb,
afterward off right.)
Ill, D,
Mar. 6.
H. M.
I 56 A.
M. I, D,
Mar. 16.
H. M.
6 33 P. M.
I,D,
6.
3 42 A.
M. I, D,
22.
I 58 A. M.
II, D,
7.
9 38 P.
M. II, D,
22.
2 51 A. M.
I. D,
7-
10 IIP.
M. I, D,
23.
8 26 P.M.
I, D,
13.
5 36 A.
M. II, D.
25.
4 10 P. M.
III, D,
13.
5 55 A.
M. II, R,
25.
6 40 P. M.
I, D,
IS-
12 5 A.
M. Ill, R.
27.
4 28 P. M.
II. D,
IS.
12 15 A.
M. I, R,
31*
3 30 A. M.
Phases of the Moon.
P. S
.. T.
Full
VC<Mtfl,
Apr. 6,
H. M.
I 20 P» M.
Last
Quarter,
Apr. 13,
6 28 A. M.
New
Moon,
Apr. 20,
2 21 P. M.
First
Quarter,
Apr. 28,
6
5 P. M.
The Sun.
R. A.
Declination.
Ris*s.
Transits.
Sets.
1898.
H. M.
'
H. M.
H.
M.
H. M.
Apr. I.
43
+ 4 40
5 48 A.M.
12
4 P.M.
6 20 P.M.
II.
I 20
+ 8 26
5 32
12
I
6 30
21.
I 57
+ 11 58
5 18
II
59 A.M.
6 40
May I.
2 35
+ 15 10
5 4
II
57
6 50
Mercury.
Apr. I.
I 39
+ 11 38
6 20 A.M.
I
P.M.
7 40 P.M.
IC.
2 31
+ 17 45
6 12
I
12
8 14
21.
2 48
+ 19
5 42
12
49
7 56
May I.
2 34
+ 15 41
5 2
Venus.
II
56 A.M.
6 50
Apr. I.
I 26
+ 84
6 19 A.M.
12
46 P.M.
7 13 P.M.
II.
2 12
+ 12 45
6 9
12
53
7 37
21.
3
+ 16 56
6 3
I
2
8 I
May I.
3 50
+ 20 24
6
I
12
8 24
Astronomical Society of the Pacific. 21
Mars.
R. A. Declination. Rises. Trwisils. Sets.
1898. H. M. ® ' H. M. H. M. H. M.
Apr. I. 22 43 — 9 24 4 36 A.M. 10 4A.M. 3 32P.M.
II. 23 12 — 6 26 4 16 9 54 3 32
21. 23 41 - 3 23 3 54 9 43 3 32
May I. o 9 — o 18 3 33 9 32 3 31
JUPITER^
Apr. I. 12 19 — o 21 5 40 P.M. II 38 P.M. 5 38A.M.
II. 12 15 4- o 8 4 54 10 54 4 54
21. 12 II + o 33 4 9 10 II 4 13
May 1. 12 7 + o 52 3 25 9 28 3 31
Sa turn.
Apr. I. 16 44 —20 24 II 19P.M. 4 6a.m. 8 53A.M.
II. 16 43 — 20 21 10 38 3 25 8 12
21. 16 41 — 20 17 9 56 2 44 7 32
May I. 16 39 — 20 12 9 15 23 6 51
Uranus,
Apr. I. 16 6 — 20 39 10 40P.M. 3 27A.M. 8 14A.M.
II. 16 4 — 20 37 10 o 2 47 7 34
21. 16 3 — 20 33 9 19 26 6 53
May I. 16 I — 20 29 8 38 i 25 6 12
Neptune,
Apr. I. 5 17 +21 45 9 19A. M. 4 37P.M. II 55P.M.
II. 5 18 + 21 47 8 40 3 58 II 16
21. 5 19 -}- 2C 48 82 3 20 10 38
May I. 5 20 + 21 50 7 24 2 42 10 o
Eclipses of Jupiter's Satellites, P. S. T.
(Off right hand limb, as seen in an inverting telescope.)
H. M. H. M.
I. R, Apr. I. 6 59 p. M. I. R, Apr. 14. 4 18 a. m.
II, R. I. 9 17 p. m. I, R, 15. 10 47 p. m.
Ill, R. 3. 8 25 p. M. II, R, 16. 2 30 A. M.
I, R, 7. 2 24 A. M. I, R, 175 15 P- M.
I. R, 8. 8 53 p. M. I, R, 23. 12 41 A. M.
II. R, 8. II 53 p. M. I. R, 24. 7 9 p. M.
Ill, R. II. 12 22 A.M. II, R, 26. 6 24 p. M.
22
Publications of the
(TWENTY-EIGHTH) AWARD OF THE DONOHOE
COMET-MEDAL.
The Comet-Medal of the Astronomical Society of the Pacific
has been awarded to C. D. Perrine, Assistant Astronomer in
the Lick Observatory, for his discovery of an unexpected comet
on October i6, 1897.
The Committee on the Comet- Medal,
Edward S. Holden.
j. m. schaeberle.
December 16, 1897.
AS1
PRONOMICAL
Made by Torval
Va
OBSERVATIONS IN 1897.
D Kohl, at Odder, Denmark.
RiABLE Stars.
Z Cyg-ui.^
January
i:
Z invisible.
September 11: id.
2:
id.
25: < e.
February
3:
id.
27: id.
4:
id.
October 20: id.
24:
= e.
25: id.
27:
id.
November 8: id.
April
19:
= a.
11: a little < d.
29:
f >a.
l<26.
-■■{^i:
May
23:
= b.
December 13: a little > a.
August
22:
invisible.
18: = a.
19: id.
The Stars A
and By near X^ Cygni.f
January
i:
A >B.
October 20: id.
2:
A = B.
25: id.
February
4:
id.
November 8: A = B.
April
29:
id.
11: A<B.
May
23:
id.
December 19: A < B.
Septembei
• 14:
27:
A > B.
A < B.
Thei
star A
is reddish.
*l^idg the sketch in the Publications A. S. P., No. 48, paKe69.
^l^ide the sketch in the Publications A. S. P., No. 34, page 37, and the observations
in No. 48, page 71.
Astronomical Society of the Pacific,
23
S Urs(B
majoris.
January
-\tt
September 1 1 : . ^ ^•
27: id.
14: id.
February
-{ti
18: a little > d.
25: id.
24: = d.
27: id.
27: id.
October 20: a little < e.
March
.i.f<e.
25: < e.
November 11: = f.
April
19: =g.
14: id.
29: invisible.
December 13: < g.
May
23: id.
18: id.
August
27: = d.
T Ursos majoris.
The star was invisible on all the dates on which S Ursa
majoris was watched, with the exception of the following dates: —
March
April
31
19
T<g.
f>f.
l<e.
May 23: a little > b.
August 27 : = g.
W Pegasi [a, a little > a, ].
•a,
X *w
%
*(lz
/o Zo So ^o yt?
The Region about IV Pegasi,
^O
August
22:W|<^-
r 23:
September 18:
October 20:
21:
26:
>c.
a little < b.
<b.
a little < c.
id.
id.
id.
November 14: < c.
December 13: i ^
18: id.
19: a little < g.
24
Publications of the
14 and 16 Coma Berenicis,
For many years I have perceived a slight variation in the
stars 14 and 16 Coma^ namely: —
1879,
1880,
1881.
1882,
1885,
1887,
1891,
1894,
March 20:
January 19:
March* 8:
December 9:
March 28:
April 18:
January 14:
February 2 1 :
November 19:
April 12:
March
March
April
March
April
16:
9:
5:
28-
8:
14 > 16.
id.
id.
14 = 16.
14 > 16.
14 = 16.
14 > 16.
id.
id.
id.
id.
id.
id.
14 < 16.
14 = 16.
1895, March 2:
November 27:
December 11:
1896, March 4:
11:
17:
31:
i:
4:
9.*
2:
24:
27:
31:
19:
May
14 >
14 <
14 =
14 <
14 =
id.
14 >
14
id.
id.
14
id.
id.
id.
14 <
December 19: 14 ^
1897, January
February
March
April
16.
16.
16.
16.
16.
16.
16.
= 16.
16.
12 and I J Coma Berenicis,
These two stars also seem to have a slight variation in brigfht-
ness.
1894.
March 28:
13 = 12.
May 9:
13 < 12-
April 8:
13 < 12.
1897, January 2:
13 = 12.
1895.
March 2 :
13= 12.
February 24:
13 < 12.
December 1 1 :
13 > 12.
27:
id.
1896,
March 17:
13 = 12.
March 3 1 :
id.
May i:
13 < 12.
April 19:
id.
4:
13 = 12.
December 19:
id.
Besides the above-mentioned observations, a great many other
sketches of fixed stars have been made with reference to sup-
posed variations.
Astronomical Society of the Pacific. 25
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26 Publications of the
The little observatory in the garden of the Real School at
Odder has been altered in the past year, so that the dome which
formerly could be opened in six directions can now be turned
around.
FIRST AWARD OF THE BRUCE MEDAL.
The award for 1898 of the Bruce Medal of the Astronomical
Society of the Pacific has been made to Professor Simon New-
comb.
SPECTROSCOPIC BINARY STARS.
By R. G. Aitken.
The announcement made in Harvard College Observatory
Circular, No. 21, that fi Lupi is a spectroscopic binary, calls new
attention to one of the most interesting classes of stars known.
Binary star systems — that is, systems comprising two suns in
orbital motion about a common center of gravity — have been
known since the time of Herschel; but their periods of revolu-
tion are reckoned in years and even in centuries. The most
rapid binary known at the beginning of the present decade
needed eleven and a half years to complete a single revolution.
Small wonder then, that the startling announcements made by
Pickering and Vogel that i Ursa majoris made a complete
revolution in about 105 (later reduced to 52) days, and that
^ Persei (Algol), fi Auriga, and a Virginis had periods of from
2.9 to 4 days, should be received with caution and even with
suspicion.
It is true, indeed, that Goodricke, who discovered the
variable character of the light of Algol in 1782^ suggested an
eclipse of the visible star by a dark body as a plausible explana-
tion of the periodic dimming of its light. But another explanation
that found favor was, that Algol was a bright star, upon .whose
photosphere spots analogous to our sun-spots were irregularly
distributed, the periodic time of light variation corresponding to
the time of axial rotation. At best, Goodricke*s hypothesis
was classed with other theories, convenient as explanations, but
not susceptible of proof. The modern spectroscope, however,
by demonstrating that the spectrum of the star was sensibly the
Astronomical Society of the Pacific. 27
same in quality in all its light phases, disposed of the spot theory;
and later, in the skillful hands of Vogel, proved that Good-
rick e's hypothesis was substantially correct.
Professor Vogel photographed the spectrum of Algol on
many nights, and on each plate photographed also the spectrum
of hydrogen. If the star were at rest relatively to the Earth » the
hydrogen lines in the star*s spectrum should correspond to those
in the artificial spectrum. If the star were receding from the
Earth, the lines in its spectrum (according to Doppler's
principle) should be shifted slightly, with respect to the lines in
the hydrogen spectrum, toward the red end, and if approaching
the Earth, toward the violet end of the spectrum. Now, Vogel
found that before the obscuration the lines were shifted toward
the red end by an amount corresponding to a velocity of reces-
sion of about twenty-seven miles a second. After obscuration,
the shifting of the lines towards the violet end indicated a some-
what greater velocity of approach. This is just what should
happen if a dark body were swinging the bright star around a
common center of gravity in an orbit nearly edgewise to the
Earth, the whole system meanwhile approaching the Sun.
Vogel's results were published in November, 1889. In
August of the same year. Professor E. C. Pickering announced
that certain lines in the photographic spectrum off Ursa majoris
(Mizar) were found to be double on some plates, single on others.
Examination of many plates showed a periodic recurrence of the
phenomenon at intervals of about fifty-two days. A little later
in the same year, he announced that Miss A. C. Maury had
discovered the same peculiarity in the spectrum of 1^ Auriga,
with the important difference that in the latter star the doubling
of the lines occurred at intervals slightly less than two days.
The explanation of this phenomenon is, that these stars consist of
two components revolving, as in the case of Algol, in an orbit
turned nearly edgewise to us, each component being bright.
When the stars are at right angles to the line of vision (at elonga-
tion, that is), one will be moving towards us, the other away from
us, and the lines in their spectra are, consequently, shifted in
opposite directions. As the stars are so close together that their
spectra overlie each other on the plate, the effect is to show the
lines in the resulting compound spectrum apparentiy double.
In April, 1890, Vogel published his investigations on the
spectrum of a Virginis, Discordances in the values of the
28 Publications of the
velocity of the star in the line of sight led to more extended
observations, with the result that it was found that the star is
moving in a nearly circular orbit, with a period of about four
days. As the lines in the spectrum show no evidence of doub-
ling, the companion must be relatively a dark star, as in the case
of AlgoL But as the bright star suffers no diminution in its
light, the orbit must be sufficiently inclined to the line of sight to
prevent eclipses.
These stars, then, are typical of the three varieties of binary
systems whose existence has been demonstrated by the spectro-
scope, viz. (i) a bright star with a relatively dark companion,
the plane of the orbit passing so nearly through the Sun that the
brighter star suffers periodic partial or total eclipse; (2) a bright
star with a relatively dark companion, the plane of the orbit
being so inclined to the line of vision that eclipses are impossi-
ble; (3) a system of two bright stars. It is probable that stars
of the 17 Aquila type— to which attention is called in a note else-
where in this number — should be included in the second class.
Perhaps, too, that puzzling variable, ^ Lyra, — a variable siii
generis, one writer calls it — should be included, as Pickering
(H. C. O. Circular 7) classes it with the A/go/ type variables.
Since this observer's discovery of the composite nature of its
spectrum, fi Lyra has been carefully studied by many observers,
and important papers on its photographic spectrum have been
published by Belopolsky, Vogel, Sidgreaves, Lockver,
and others. To indicate, even in the briefest manner, the com-
plex nature of the observed phenomena and the various hypoth-
eses that have been framed to account for them, would require a
separate article. As it is the purpose of the present paper merely
to give some account of our knowledge of the three varieties of
binaries above enumerated, it must suffice here to say of fi Lyrcg
that, while it is probably binary, no hypothesis has yet been
framed that explains completely all the observed changes in light
and spectrum.
When Vogel made public his researches pn j3 Persei, ten
A/go/'type variable stars were known. Since then, their number
has been increased to fifteen, possibly sixteen. They are here
given, together with their discoverers, dates of discovery, approx-
imate periods, range of magnitude, and duration of change.
The data are nearly all taken from Chandler's " Third Cata-
logue of Variable Stars.*'
Astronomical Society of the Pacific.
29
Name.
? Petsei (Algol) .
S Cancri ....
\ Tauri
% Librae
U Corona . . . .
UCet*hei . . . .
UOphtnchi . . .
YCygni
R Cants Majoris .
5 Aniline t . . .
Z Herculis . . .
R Ara
RS SagUlarii . .
S Velorutn . . .
Y BootisO)X . .
W Delphini . . .
Discoverer.
Period.
Goodricke,*
Hind.
Baxendall,
Schmidt,
Winnecke,
Ceraski,
Sawyer,
Chandler,
Sawyer,
Paul,
1782
1848
1848
1859
1869
1880
188 1
1886
1887
18S8
2d 20*^
9 II
22
7
MulIer&Kempf,i89i
Roberts,
Gould,
Woods,
Parkhurst,
Miss Wells,
1891
1874
1894
1894
1895
48m 55*
37 45
52 2
51 23
10
II
20
II
3
7
23
10
9
22
2.6
4 19
51
49
7
57
15
46
49-54
12.7
58.6
2435
21.2
Magnitude anii
Duration of Change.
2.3 to 3.5 in loh
8.2 to 9.8 in 2i>^
3.4 to 4.2 in 10
5.0 to 6.2 in 12
7.5 to 8.9 in 10 nearly
7.1 to 9.2 in 10
6.0 to 6.7 in 5
7.1 to 7.9 in about 8
5.9 to 6.7 in 5
6.7 to 7.3 in about 3>^
7. 1 to 8.0
6.9 to 8 o in 10.3
6.4 to 7.5
7.8 to 9 3 in 15.2
8.0 to 8.6
9.5 to < 12 in 3 lb
The eclipse hypothesis was naturally applied to these Algol-
type stars, but not with immediate and complete success. In the
case of Algol itself a difficulty was encountered, in that the period
was known to be about six seconds shorter than at the time ol
GooDRiCKE*s discovery, while in 1798, and again in 1830, it was
slightly longer. The irregularities in the periods of other stars,
as, for instance, 6* Cancri and X Tauri^ were even more marked ;
in fact, it is even now impossible to determine the law governing
the inequalities of the last-named star.
Dr. Chandler (A. J. VII) had investigated the irregularities
in Algol's period fully; and in 1892 he followed this investiga-
tion with the demonstration of a proposition that may be put
most briefly in his own words: —
^^ Algols together with the close companion — whose revolu-
tion in 2** 20*'. 8 produces by eclipse the observed fluctuations in
light, according to the well-known hypothesis of Goodricke,
confirmed by the elegant investigation of Vogel, — is subject to
still another orbital motion of a quite different kind. Both have
a common revolution about a third body, a large, distant, and
dark companion, or primary, in a period of about 130 years.
• Suspected by Montanari, 1669.
t Questioned by Pickering, H. C. O. Circ. 7.
t Parkhurst's idea that this star is of the Aigol'iy\tc has not yet been confirmed.
X Caritur is also suspected to belong to this class, but Roberts' announcement still
awaits confirmation.
30 Publications of the
The size of this orbit around the common center of gravity is
about equal to that of Uranus around the Sun. The plane of
the orbit is inclined about twenty degrees to our line of vision.
Algol transited the plane, passing through the center of gravity
perpendicular to this line of vision, in 1804 going outwards, and
in 1869 coming inwards. Calling the first point the ascending
node, the position-angle, reckoned in the ordinary way, is about
sixty- five degrees. The orbit is sensibly circular, or of very
moderate eccentricity. The longest diameter of the projected
ellipse, measured on the face of the sky, is about 2". 7.'*
It would take us too far to enter into the proofs of this propo-
sition. It must be sufficient to say that Dr. Chandler made
out a very strong case, and that subsequent observations and
investigations seem to substantiate his argument. Chandler
further pointed out the fact that analogous irregularities existed
in the periods of six, or, perhaps, seven others of the ten stars of
this type then known, while two were of too recent discovery to
make possible any assertion about the constancy of their periods.
** The principle of attributing like effects to like causes allows us
to assume, with high probability, that ... all the stars of
this class have similar motions, namely, one around a near com-
panion, the other a common motion of these two bodies around
a distant one.'*
In this connection it is of historical interest to note that Pro-
fessor Wm. Ferrel, in 1855, suggested,* as an explanation of
the retardation and subsequent acceleration of its period, that
Algol and its hypothetical close companion revolved about a
distant dark companion in a period of perhaps several centuries.
In speaking of Algol's close companion, we have called it
''relatively dark.'* Vogel showed that iT its light were one
eightieth part as intense as that of its primary, a secondary mini-
mum would be produced, caused by the brighter star occulting
its faint companion. In at least three of the Algol-type stars, viz.
/^S Sagittarii^ Y Cygni^ and Z Herculis^ this phenomenon has
been observed.
According to Roberts, the first-named star usually has a
magnitude of 6.60; at the chief minimum this becomes 7.59,
and at the secondary minimum 6.89. This he accounts for by
assuming that one star of the system is nearly twice as bright as
• Nashville Journal of Medicine and Surgery, April, 1855. Reprinted in Astronomy
and Astro-Physics, Vol. XII, p. 429.
Astronomical Society of the Pacific, 31
the other; that the orbit is eccentric, the line of apsides nearly
coinciding with the line of sight; and that the fainter star is
almost directly between us and its primary (thus causing the
chief minimum) when the stars are at their greatest distance
apart.
The secondary minimum in Y Cygni differs so little in point of
magnitude from the principal one that it is only recognized by
the fact that the minima, instead of following each other at
uniform intervals, occur at intervals of thirty- two hours and forty
hours alternately. Hence, for this star the terms even and odd
minima are used. Duner*s explanation of these facts is, that the
star consists of two equally large and bright components, revolv-
ing about their common center of gravity in an elliptic orbit in a
period of nearly three days, the perihelion passages occurring
between the even and the odd epochs. The eccentricity of the
orbit need only be o.i to explain fully all the observations.
Observation seems to show that the intervals between even and
odd minima are not constant; and this Duner would explain by
assuming a third invisible perturbing body, which causes a motion
of the line of apsides such as is found in the planets and satellites
of the solar system.
Z Herculis differs from Y Cygni in that the minima, which
occur at intervals of forty-seven and forty-nine hours, respec-
tively, are alternately faint and very bright.
To suit these intervals and magnitudes, Duner finds that we
must assume that Z Herculis consists of two stars of equal size,
one of which is twice as bright as the other. The semimajor axis
of the elliptic orbit of the stars is six times their diameter (assum-
ing that one star remains fixed in the focus Oi'' the ellipse). The
plane of the orbit passes through the Sun, the eccentricity is
about o. 25, and the line of apsides is inclined at an angle of four
degrees to the line of sight.
While there are still many difficult and interesting problems
to solve in connection with the A /go/- type stars, it is now certain
that the solutions will be sought — and probably found — in exten-
sions of the theory of orbital motion; and enough has been said
here to indicate the lines along which the investigations are pro-
ceeding.
One further characteristic may be mentioned that is common
to all these stars, namely, their small mean density. Several
investigators have found that the mean density of A/go/ is not
32 Publications of the
more than one fourth that of water, while other stars of the type
are even more tenuous. If these results are correct, the Algol-
type stars must be completely gaseous.
Turning now to the binary stars which have been revealed by
the doubling of the lines in their spectra, we find that, so far,
only five have become known to us.
Name. Discoverbr. Period.
1^ Ursa maj oris, Pickering, 1889 52 days.
j3 AurigcB, Miss Maury, 1889 3** 23** 36.7™
/x' Scorpii, Bailey, 1896 i 10 42.5
A, G, C. 10534, Pickering, 1896 3 2 46
fi Lupi, Mrs. Fleming, 1897 Undetermined.
As already stated, { Ursa majoris was the first star of this
type to reveal its binary character by the periodic doubling of its
lines. But it is, nevertheless, the one whose period we are least
certain of — with the exception of fi Lupi, just discovered. As
the lines are clearly double about every fifty-two days, the period
was at first announced as 104 or 105 days. Later evidence,
however, indicates that half this time is the true period, the orbit
of the second star about its primary being probably an ellipse of
considerable eccentricity, with the major axis nearly perpendicular
to the line of sight. In this case the lines would be seen double
once in each revolution — at the time of periastron passage, —
but would only become broader and blurred at the time of
apastron. This theory would seem to fit the observations fairly;
but there appear to be irregularities in the period, which may
perhaps indicate the presence of a third body. The maximum
relative velocity of the two components is found to be about 100
miles per second.
The second star in this list, fi Auriga^ is much more rapid
and decided in its changes. So rapid, in fact, are the changes in
the spectrum, that they are sometimes perceptible, according to
Pickering, In successive photographs, and in the course of an
evening are very marked. The distance between the lines when
at their greatest separation is so great that measures are easy
and accurate. There is a very slight difference in the intensity
of the lines, and the fainter line is alternately more and less
refrangible than the brighter one. As the measures of the
amount of separation in the two positions indicate nearly the
same velocity, — about 150 miles per second — it is probable that
Astronomical Society of the Pacific. 33
the orbit is nearly circular. As the period is four days, it follows,
assuming the plane of the orbit to be parallel to the line of sight,
that the distance between the stars is about 8,000,000 miles, and
the combined mass 2.3 times that of our Sun. If the orbit is
inclined to the line of sight, as is probable, these values must
be increased by an amount depending on the inclination.
Pritchard has found the value of the parallax of fi Auriga to
be o".o62; hence the greatest angular separation of the compo-
nents is less than o".oi. The most powerful existing telescope,
therefore, can never make the components visible to us.
/i' Scorpii and A, G, C, 10534 resemble fi Auriga, in that
their periods of revolution are short and the doubling of the lines
very marked. In fact, in these respects they surpass the latter
star, as the recent measures by Mrs. Fleming show that the
relative velocities of the components are about 286 and 379 miles
per second, respectively. In each of these stars one component
is noticeably fainter than the other. The relative intensity of the
lines in /x' Scorpii seems to change, indicating a possible light
variation in one of the components; but this needs further inves-
tigation.
If we except the short period variable stars, like 17 Aquila and
S Cephei, which are almost certainly binary systems, but which
require additional hypotheses to account for their variability, we
have two stars left which call for brief notice, viz. a Virginis
{Spied) and a' Geminorum, the principal component of the well-
known double star Castor, As has been said above, the former
was discovered by Vogel, in 1890, by the shifting of the hydro-
gen lines in its spectrum alternately toward the red and violet end,
with respect to the lines in an artificially produced spectrum of
hydrogen. It was thus found that, while the system is approach-
ing the Sun at the rate of nine miles per second, the two compo-
nents are in orbital motion, with a velocity of about fifty-seven
miles per second, completing one revolution in 4.0134 days. In
the same way Belopolsky found, in 1896, that the components
of of Geminorum complete a revolution about their common
center of gravity in 2.91 days.
That the number of known spectroscopic binary stars will be
largely- increased by future discoveries, is certain, and it is entirely
possible that the study of their phenomena, as shown in light
variations and changes in spectrum, may yet reveal to us systems
more complex than even our own solar system.
34 Publications of the
The mathematical formulae, by means of which the elements of
a binary star orbit may be computed from measures of the relative
velocities of the components in the line of sight, have been fully
developed by Rambaut,* WiLSiNG,t and LEHMANN-FiLHfes.J
but the discussion of their methods and results is beyond the
province of this article.
Lick Observatory, University of California,
January 26, 1898.
* Mon, Not. R. A, S., March, 1891.
fA. AT., 3198.
XA. A'., 3242.
Astronomical Society of the Pacific, 35
NOTICES FROM THE LICK OBSERVATORY.*
Prepared by Members op the Stafp.
Rediscovery of Winnecke's Periodic Comet = a 1897.
This comet was observed by the writer on the morning of
January 2d. At 2*^ 5°* 42* G. M. T. it was in R. A. \^ 19°* 2*. 51
and Decl. — 3° 58' 34". 3. It is, therefore, 2° o* east and 8'. 7
south of the place predicted for it by Hillebrand {AsL I^ach,^
No. 3447).
The comet is very small and faint, about 10" to 15" in
diameter, and slightly brighter at the center. It is much less
favorably situated at the present return than at the last, in 1892,
and hence will be faint during this entire apparition and probably
not within the range of small telescopes.
This comet was first discovered by Pons in 18 19, and a period
of five and a half years deduced by Encke. It was, however,
not seen again until 1858, when it was discovered as a new comet
by WiNNECKE. It has been observed at the subsequent returns
in 1869, 1875, 1886, and 1892. C. D. Perrine.
The Probable State of the Sky along the Path of
Total Eclipse of the Sun, May 28, 1900.!
* * Having regard to the cost of establishing temporary eclipse
stations, and the losses to science in case a clear view of the Sun
is not secured during totality, it is proper to determine, as far as
practicable, the probable state of the sky along the path, with the
view of selecting the best sites for the observations. To do this,
a study may be made of the cloud conditions prevailing annually
along the shadow track for a period of time, including the date
• Lick Astronomical Department of the University of California,
t Abstract from the Report by Professor Frank H. Bigbi.ow, in the Monthly Weather
Review for September, 1897.
3^ Publications of the
of the eclipse. Certain areas may show greater tendency to
cloudiness than others, and this fact will have some weight with
observers in choosing their stations.
** The eclipse track for May 28, 1900, passes over the Southern
States from New Orleans, La., northeastward to Norfolk, Va.,
and it will be surveyed by the U. S. Weather Bureau for the
benefit of the astronomical expeditions.
** ... Beginning with May 15, 1897, ^^^ continuing until
June 15, 1897, so as to include May 28th centrally, observations
were made at sixty-six stations, . . . covering quite uniformly
the portions of the States of Virginia, North Carolina, South
Carolina, Georgia, Alabama, Mississippi, and Louisiana, over
which the track is plotted. . . . The general state of the sky
at 8 A. M., 8:30 A.M., and 9 a. M., was noted. ... At the
same hours the state of the sky near the Sun was observed. The
observers were generally volunteers, who did this work at the
request of the Weather Bureau. . . .
** Judging from the table [of the results of the observations] it
would be much safer to locate in central Georgia or Alabama,
upon the southern end of the Appalachian Mountains, where the
track crosses the elevated areas, than nearer the coast line in either
direction, northeastward toward the Atiantic coast, or southwest-
ward toward the Gulf coast.
** ... It is intended to repeat the observations during the
years 1898 and 1899, after which we shall be as well informed as
possible regarding the selection of the eclipse stations for the year
1900.''
Eclipses of fupiTER's Satellite IV.
The present cycle ol eclipse phenomena for fupiter' s fourth
satellite is nearly closed, and, of course, the latest observations
are among the most favorable for correcting the ephemeris.
Immediately ^i\.^x fupiter has made his appearance on this coast,
at midnight. January 9th-ioth, Satellite IV will suffer eclipse,
and the reappearance nearly two hours later should be well
observed.
The last eclipse, when the satellite will be only half an hour in
the shadow, may possibly be seen from Mt. Hamilton, on the
morning of March ist, when, although the Sun is just above the
eastern horizon, fupiter is low down in the west. C. B. H.
San Francisco, December 5, 1897.
Astronomical Society of the Pacific. 37
The Star with the Largest Known Proper Motion,
The star, Cordoba Zone Catalogue, 5**, No. 243, has been
found by Professor J. C. Kapteyn and Mr. R. T. A. Innes to
have an annual proper motion of +o*.62i in Right Ascension
and — 5". 70 in Declination, or of 8". 7 in the arc of a great circle.
The announcement in the Astronomische Nachricktetiy 3464,
states that the discovery was made in comparing the Cape Photo-
graphic Durckmusierung star places with those of other star
catalogues.
The largest known proper motion of any star previous to this
discovery was that of the so-called ** runaway'* star, 1830
Groombridge, which has an apparent drift of 7".o annually.
January 6, 1898. R. G. A.
Astronomical Telegram (Translation).
Lick Observatory, Jan. 3, 1898.
To Harvard CoUege Observatory, j ^gent 10:50 A. M.)
Cambridge. Mass. )
Comet Winnecke was observed by Perrine, January
2.0873, R. A. 15^ 19™ 2*.5, Decl. - 3° 58' 34". Faint.
Observational Astronomy: a Practical Book for
Amateurs. By Arthur Mee, F. R. A. S.
The library of the Society has become the possessor, through
the courtesy of the author, of the second and thoroughly revised
edition of what Knowledge calls **an excellent, honest little
book.'* A cursory examination indicates that the author is
justified in believing ** that this second edition may be described
as the most detailed work at the price that has ever been offered
to the fast-growing circle of amateur astronomers.'* It is up to
date, contains a vast amount of information well arranged,
ample references to special treatises and articles in the scientific
journals and reports of observatories, and is illustrated with
portraits, maps, drawings, and photographs. ** Every care has
been taken to insure accuracy, and the fanciful results of the
recently established school of marvel-mongers are either dismissed
altogether, or viewed in these pages with a skeptical eye. ' '
A brief but appreciative memoir of the Rev. Prebendary
Webb, author of the well-known * ' Celestial Objects for Common
Telescopes," is appended.
38 Publications of the
Some Interesting Double Stars.
I have recently secured three measures of the star /3 395 ^ the
latest addition to the rank of rapid binary stars. The mean of
these measures is, —
1897.92 273°.; o".27.
In 1891 Burnham's measures gave an angle of 118° and a
distance of o".75. According to See, the period of this star is
about sixteen years.
Measures of O 5 j/j, ^ Andromeda^ on three nights give a
mean result of, —
1887.98 56° 4 o".23.
This is in good agreement with measures made by Professor
Hussey about the same time. So far as I know, these are the
only measures that have been made since Burnham*s rather
uncertain measure on one night in 1892, just after the star had
passed periastron. The angular motion since 1851, the date of
discovery, exceeds 250°.
The star k ig68y though not a binary, is interesting because
of the relative proper motion of the two close components. The
distance, which in 183 1 exceeded 20", is now about 2". 5. A recent
discussion by Professor S. Glasenapp shows that the relative
annual motion of B to A is ©".2753 in the direction 235° 11.
The minimum distance, 2". 28, between the stars will be reached
in 1904.
The following measures have been made of the companion
to Procyon: —
1897-838 321°. 7 4"- 84
.876 324 .8 4 .67
.915 324 '8 4 '59
1897.88 323^.8 4". 70
These measures, like those by Professor Schaeberle, indi-
cate direct orbital motion.
Two measures of the companion to Sirius have been secured
in addition to those published in No. 59 of these Publications.
They are: —
1897.838 i75°.8 4". 14
.915 172 .8
Clouds prevented distance measure on the second night. All
the above measures were made with the 36-inch telescope.
January 21, 1898. R. G. AlTKEN.
Astronomical Society of the Pacific. 39
Errata in Star Catalogues.
In the course of some work involving an extensive use of
southern star catalogues, a few errata and unusual discrepancies
have been noted. In general they are of minor importance, but
the insertion of the corrections in the catalogues may save some
annoyance.
Cordoba Durchmusterung : —
— 23° 13035 for G C. read Z C.
— 24° 15285 differs —2'. 2 in 8 from Z C. I9'.695.
—24° 16622 print G C.
—24° 16626 for G C. read Z C.
— 24^ 16877 delete Z C.
—24° 16874 print Z C.
— 24° 16959 print G C.
— 24° 16960 delete G C.
— 25° 13024 delete G C.
— 25° 13025 print G C.
—25° 15714 for G C. read Z C.
—26° 10862 for G C. read Z C.
— 27° 12682 for G C. read Z C.
—28° 6607 delete G C
— 28"^ 17047 for G C. read Z C.
—28° 17523 Decl. for 32'.© read 22'.©.
^31° 3136 Declination differs 1^.5 from G C. 7589.
—31° 3^ Right Ascension minute 41 is omitted. It should
be printed with No. 1538.
—32° 16677 for G C read Z C.
""34° 5905» 5906. The magnitudes in C D M. are respect-
ively, 9.6 and 7.9. G C 12906 gives CDM. 5905
a magnitude of 7)4. Are the CDM. magnitudes
interchanged ?
-34"
page
139, for —36° read -
-34°.
-36°
6426
for 3.5 mag. read 8.5
-38°
9130
for G C. read Z C.
-39°
141M
\ Decl. for 29'. I read
24'. I
-40°
8818 for G C. read Z C.
-40°
9495
delete U A.
-40°
9496 print U A.
40 Publications of the
Cordoba Zones: —
17^ 2644 Right Ascension is I'.i greater than G C. 24105.
Cordoba General Catalogue: —
2107, column Prec. An., for 2*.934 read 2'.634.
Argelander's Southern Zones ( Weiss): —
1607 Declination i' too far south? See G C. 3239.
8708 Declination i' too far south? See G C. 14501.
18236 Right Ascension differs + i' from G C. 32393.
ScHONFELD'S Souihem Durchmusierung : —
— 20° 5055 is marked A, but is not in Weiss's Arge-
lander,
Yarnall (Frisby) 327. An. Prec. for 10". 85 read
19". 85.
Yarnall (Frisby) 8888 is called Arg. (Oe) 20215.
Weiss gives 50' less Right Ascension.
R. G. AlTKEN.
January 15, 1898.
Award of the Lalande Gold Medal to Assistant
Astronomer C. D. Perrine, of the Lick Observatory.
The members of the Astronomical Society of the Pacific will
be pleased to learn that at the meeting of the French Academy
of Science, held in Paris, December 30, 1897, the Lalande
Gold Medal was awarded to C. D. Perrine for distinguished
services in astronomy.
Since his connection with the Lick Observatory, Mr. Perrine
has discovered five new comets and rediscovered two periodic
comets. In addition to these discoveries, he has not only pub-
lished long series of observations on these bodies, but has also
computed and published various orbits and ephemerides of the
new comets from his own observations.
It is quite remarkable that every one of the last five comets
observed was successively discovered by this same observer,
three being new, and two rediscoveries of the periodic comets
ol d' Arrest and Winnecke.
The award of the Lalande Gold Medal to Assistant
Astronomer C. D. Perrine, is but a just recognition, by one of
the world's leading scientific bodies, of a most worthy investigator.
J. M. S.
Lick Observatory, January 21, 1898.
Astronomical Society of the Pacific. 41
Belopolsky*s Researches on y^AQUiiM.
The variable character of 17 Aquilce was discovered by Pigott
in 1784, and from the observations since that time the period of
its variation in brightness, ranging from 3.5 to 4.7 magnitude,
has been determined with great accuracy. According to Chan-
dler's Third Catalogue of Variable Stars, the period is 7. 176381
days, or somewhat more than seven days four hours.
In September, 1895, M. Belopolsky reported to the Academy
of Sciences of St. Petersburg that his spectrographic observations
of this star indicated a variable velocity in the line of sight.
During the past year he has again studied the star by means of
photographs of its spectrum, taken with improved spectroscopic
apparatus in connection with the 30-inch refractor at Pulkowa.
His former results have been confirmed. He finds the velocity
in the line of sight periodically variable, ranging from -\-\,(>\ to
— 18.63 miles per second. Assuming the variations of velocity
to be due to orbital motion and with a period of revolution equal
to the period of the star as a variable, he has determined elliptic
elements, so as to satisfy the observed velocities in the line of sight.
It is found that the times of minimum brightness and the times at
which the velocity in the line of sight is the same as that of the
motion of the system, do not coincide, and for this reason some
explanation other than that of eclipses must be sought to explain
the variations of brightness.
M. Belopolsky has arrived at a like result in the case of
I Cephei, a variable star, whose range in variation of brightness
and whose light curve are very much the same as those of
HI Aquilce, W. J. HussEY.
Meteors Visible in Full Daylight.
The number of shooting stars or meteors that fall to the Earth
in the course of twenty-four hours reaches high into thousands,
but the great majority of them are small, and do not attract any
particular attention. At very rare intervals, however, it happens
that they are of sufficient size and brilliancy to be seen in the day-
time. The following are among the instances to be found in
astronomical records: —
On the afternoon of September 13, 1795, a meteoric stone,
weighing fifty-six pounds, fell within thirty feet of a workman in
Yorkshire, England. This stone fell with a loud explosion, and
penetrated a foot of soil and half a foot of chalk rock.
42 Publications of the
About nine o'clock in the morning of September lo, 1813,
another was seen to fall in southern Ireland. Its appearance
was accompanied with the formation of a cloud of smoke in a
clear sky. Soon after eleven distinct reports were heard, resem-
bling the discharge of heavy artillery, followed by an uproar like
that of the continued discharge of musketry. Bodies moving in
a horizontal direction towards the west with great velocity came
out of the cloud of smoke. One of these was seen to fall to the
Earth, burying itself deep in the ground. It was immediately dug
up, and found to be still hot and to have a sulphurous smell. It
weighed seventeen pounds. Other fragments fell at the same
time, and were picked up in the neighborhood.
In 1879 a meteor was seen to fall in the daytime in Southern
Virginia with sounds likened to that of an earthquake.
On the afternoon of January 19, 1898, I observed a bright
meteor from the Lick Observatory. It was merely a flash, from
five to ten degrees in length. It appeared white against the clear
sky and was visible for only a very short time, not more than a
few tenths of a second. It was moving very rapidly towards the
north in a path slightly inclined towards the Earth, and increas-
ing in brightness along its course until its sudden disappearance.
From the observatory it was seen almost directly in the west, but
its distance must remain unknown, unless at least one other
observation has been secured elsewhere. It was, however,
probably far out over the Pacific Ocean.
The time of observation was i*' 8" 40* P. S. T. The azimuth
of the point of disappearance, as seen from the Lick Observatory
and subsequently determined with surveyor's transit, was south
ninety-three degrees west, and its altitude was estimated to be
about eight degrees. E. F. Coddington.
January 21, 1898.
Report on the Teaching of Astronomy in the
United States.
The next report of the U. S. Commissioner of Education will
contain a chapter by Dr. Edward S. Holden on the teaching
of astronomy in the primary and secondary schools, and in the
colleges and universities of the United States.
Dr. Holden was elected a member of the American Philo-
sophical Society of Philadelphia at its meeting in December,
1897. R- G. A.
Astronomical Society of the Pacific. 43
Success of the Crocker Lick Observatory Eclipse
Expedition.
A cablegram received at Mt. Hamilton from Professor Camp-
bell, who is in charge of the Crocker Lick Observatory
Expedition at Jeur, India, states that most satisfactory photo-
graphs of the corona were obtained with three different telescopes
— one set with a telescope forty feet long, and two other sets with
five- foot and three-foot telescopes. He also reports that the
great equatorial extension of the corona, which formed such a
conspicuous feature of the eclipse of January, 1889, has again
been photographed.
He also satisfactorily photographed the changes in the solar
spectrum at the Sun's edge with the aid of one of the spectro-
scopes, and probably obtained successful photographs of the
reversing layer with the aid of a second spectroscope.
Professor Campbell originally intended to locate his station
in the neighborhood of Karad ; but, owing to the ravages of the
plague in that section of the country, he was compelled to change
his plans, so far as the selection of the station was concerned.
The instrumental equipment of the Lick Observatory Eclipse
Expedition was, without doubt, as complete as that of any other
party sent out on this occasion, and we believe that the results
secured by Professor Campbell will, when fully discussed, add
very materially to our knowledge of the Sun's constitution, the
nature of the forces there at work, and the character of the Sun*s
corona. J. M. Schaeberle.
Lick Observatory, University of California,
January 24, 1898.
Death of Dr.' Winnecke.
We regret to record the death of Dr. A. F. T, Winnecke,
at Bonn, on the 3d of December, 1897. Born at Hanover on the
5th of February, 1835, Winnecke received his training in astron-
omy at Gottingen, Berlin, and Bonn, coming under the personal
influence of Gauss, Encke, and Arge lander. Already well
known by his work, both in practical and theoretical astronomy,
he accepted, in 1858, an appointment in the Russian observatory
at Pulkowa. His work here in the next six years placed him in
the front rank of astronomers, but his incessant activity over-
taxed his strength, and in 1865 he was obliged to return to Bonn
44 Publications of the
in search of health. The few years following were mainly
devoted to regaining his strength, but that his scientific work
was not entirely abandoned is sufficiently made evident by the
discovery of four new comets during this time. In 1872 he had
so far recovered as to be able to accept the appointment of
Professor of Astronomy at the newly founded University of
Strassburg. Nine years of fruitful work as Director, observer,
and instructor followed; but in 1881 failing health compelled him
once more to lay aside his work and seek rest. The hope that
he might soon resume his duties was never realized.
In discovery, observation, and theoretical astronomy, WiN-
necke's work constitutes a most valuable contribution to the
science he loved.
Success of the Pierson Chabot Observatory Eclipse
Expedition.
On the afternoon of January 24th, the following telegram was
received from the Hon. Wm. M. Pierson, of San Francisco: —
** BuRCKH ALTER Cables unqualified success, and weather con-
ditions perfect. ' '
As is well known, this expedition, in charge of Charles
BuRCKH ALTER, of the Chabot Observatory, was sent out at the
expense of another member of the Astronomical Society of the
Pacific — the Hon. Wm. M. Pierson, of San Francisco, who has
taken such lively interest in the affairs of the Society, and aided
previous eclipse expeditions in various ways.
According to the above telegram, Burckhalter has obtained
satisfactory photographs of the corona with his device (described
in No. 42 of our Publications) for securing detail of both the
inner and outer corona on the ^ame negative. J. M. S.
Lick Observatory, January 25, 1898.
Astronomical Society of the Pacific. 45
The Great Nebula in Andromeda.
(See the frontispiece.)
The frontispiece of the present volume is reproduced from a
negative which I obtained with the Crocker photographic tele-
scope of the Lick Observatory on December 21, 1897, with an
exposure of five hours.
The Great Nebula in Andromeda is the only one that was
known before the invention of the telescope. Al-Sufi, in the
tenth century, was familiar with the dim, hazy region near the
most northern of the three stars composing the girdle of Andro-
meda, The telescope was first turned to this wonderful object
by Simon Marius, December 15, 16 12. He described it as like
a candle shining through horn. It received but little attention
until the time of Boulliaud, whose attention was directed to it
by the passage of the comet of 1664 across that part of the sky.
Halley described it as being triangular in shape, with the apex
of the triangle on the south preceding end, which corresponds to
the right of the accompanying reproduction. Messier described
it more accurately as two luminous pyramids having a common
base, the distance from apex to apex being about two thirds of a
degree, and the common base being about a quarter of a degree.
The next important advance in our knowledge of this nebula
was made by Professor G. P. Bond, September 14, 1847. While
examining it with the 1 5-inch refractor of the Harvard College
Observatory, he saw on the north preceding side two dark rifts,
nearly parallel to each other. These were observed with many
smaller instruments after their discovery by Bond, but they were
always drawn as straight lines.
It remained for photography to determine the true form of
these rifts. On October i, 1888, Mr. Isaac Roberts, with his
20-inch reflector, obtained a photograph of this nebula which was
a revelation to the astronomical world. It showed for the first
time the elliptical form of the nebula, with the rifts extending
almost continuously around it, as shown in the accompanying
reproduction. E. F. Coddington.
4^ Publications of the
Minutes of the Meeting of the Board of Directors,
HELD in the Rooms of the Society, January 29,
1898, AT 7:30 p. M.
Vice-President Seares presided. A quorum was present. The
minutes of the last meeting were approved. The following members
were duly elected:—
List of Members Elected January 29, 1898.
Prof. H. D. Curtis j Umversity^of the Pacific. CoUege
Dr. F. P. VON Keller Ardmore, Ind. Terr.
The John Crerar Library Chicago, III.
Mr. Henry Payot 204 Pine St., S. F. Gal.
Mr. Clarence McKenzie Lewis was elected to Life Membership.
It was, on motion.
Resolved^ That the name of the Harvard College Observatory,
Cambridge, Mass. , be added to the list of corresponding institutions.
Adjourned.
Minutes of the Meeting of the Astronomical Society
OF THE Pacific, held in the Rooms of the
Technical Society, January 29, 1898.
The meeting was called to order by Mr. Seares. The minutes of
the last meeting were approved.
The Secretary read the names of new members duly elected at the
Directors* meeting.
A committee to nominate a list of eleven Directors and Committee
on Publication, to be voted for at the annual meeting, to be held on
March 26th, was appointed as follows: Messrs. E. S. Clark, C. A.
MuRDOCK, G. V. Hicks, L. H. Pierson, J. R. Ruckstell.
A committee to audit the accounts of the Treasurer and to report at
the annual meeting was appointed as follows: Messrs. Jos. F. Gass-
mann, a. H. Babcock, and F. H. McConnell.
The following papers were presented: —
1. The Total Solar Eclipse of 1898, by E. W. Maunder.
2. A Series of Star Maps, by C. D. Perrine.
3. Planetary Phenomena for March and April, 1898, by Malcolm
McNeill, of Lake Forest.
4. Spectroscopic Binary Stars, by R. G. Aitken.
5. Observations of Variable Stars in 1897, by Torvald K5hl, of
Odder, Denmark.
Adjourned.
Astronomical Society of the Pacific, 47
OFFICERS OF THE SOCIETY.
Mr. William Alvord (Bank of California, S. F.) Prtsidtnt
Mr. £. J. MOLBRA (606 Clay Street, S. F.)
Mr. Frbosrick H. Sbakbs (Berkeley, Cal.) > Vice-Prgsidtntt
Mr. C M. St. John (U. S. Custom House, S. F.) '
Mr. C. D. Pbrrinb (Lick Observatory) Secretary
Mr. F. R. ZiBL (301 California Street, S. F.) . . Secretary and Treasurer
Board af Directors- hl^sn. Alvord, Molera. Morsb, Miss O'Halloran, Messrs.
Pbrrinb, Pibrson, Sbarbk. St. John, Tucicbk, von Gbldern, Zibl.
Finance Cammittee—Mtisn, Wu. M. Pibrson, E. J. Molbra, and C. M. St. John.
Camsmitteeon PubiicatioH — Messrs. Aitkbn, Babcock, Sbarbs.
Library Comtmittee-'MtMn. Hussby and Sbarbs and Miss O'Halloran.
Committee on the Comet' Medal— yitaaxs, Schabbbrlb and Campbbll.
OFFICERS OF THE CHICAGO SECTION.
Sxecutrtfe Committee — Mr. Ruthvbn W. Pikb.
OFFICERS OF THE MEXICAN SECTION.
Rjcecutive Committee — Mr. Francisco Rodrigubz Rbv.
NOTICE.
The attention of new members is called to Article VIII of the By* Laws, which provides that
the annaal subscription, paid on election, covers the calendar year onlv. Subsequent annual
paymcnu are due on January ist of each succeeding calendar year. This rule is necessary in
order to make our book-keeping as simple as possible. Dues sent by mail should be directed to
Astronomical Society of the Pacific S19 Market Street, San Francisco.
It is intended that each member of the Society shall receive a copy of each one of the Pub-
lications for the year in which he was elected to membership and for all subsequent years. If
there have been (unfortunately) any omissions in this matter, it is requested that the Secretaries
he at once notified, in order that the missing numbers may be supplied. Members are requested
to preserve the copies of the Publications of the Society as sent to them. Once each year a title*
page and contents of the preceding numbers will also be sent to the members, who can then bind
the numbers together into a volume. Complete volumes for past years will also be supplied, to
members only, so far as the stock in hand is sufficient, on the i>ayment of two dollars per volume
to either of the Secretaries. Any non>resident member within the United States can obtain
books from the Society's library by sending his library card with ten cents in stamps to the
Secretary A. S. P., 819 Market Street, San Francisco, who will return the book and the card.
The Committee on Publication desires to say that the order in which papers are printed in
the Publications is decided simply by convenience. In a general way, those papers are printed
first which are earliest accepted for publication. It is not possible to send proof sheets of papers
to be printed to authors whose residence is not within the United States. The responsibility for
the views expressed in the papers printed rests with the writers, and is not assumed by the
Society itself.
The titles of papers for reading shotild be communicated to either of the Secretaries as early
as poesible, as well as any changes in addresses. The Secretary in San Francisco will send to
any member of the Society suitable stationery, stamped with the seal of the Society, at cost price,
as folknrs: a block of letter paper, 40 cents; of note paper, as cents; a package of envelopes, 35
cents. These prices include postai^e, and should be remitted by money-order or in U. S. postage
stamps. The sendings are at the risk of the member.
Those members who propose to attend the meetings at Mount Hamilton during the summer
should communicate with *'The Secretary Astronomical Society of the Pacific " at the rooms of
the Societ^r, 810 Market Street, San Francisco, in order that arrangements may be made for
transportation, lodging, etc
PUBLICATIONS ISSUED BI-MONTHLY.
(February^ April t June ^ August, October, December,)
L2^
''^^^^
liS^^k'^'ox
'•Oi/A,X^/^0
^MO.
ZlP^S
A LUNAR LANDSCAPE.
(Photographed at the Lick Observatory. Dec. 31. 1897, y\i 58'" 30s to ;»» 58m 50s, P. S. T.)
PUBLICATIONS
OF THE
Astronomical Society of the Pacific.
Vol. X. San Francisco, California, April 2, 1898. No. 61
ADDRESS OF THE RETIRING PRESIDENT OF THE
SOCIETY, IN AWARDING THE BRUCE MEDAL
TO PROFESSOR SIMON NEWCOMB.
By William Alvord.
At each preceding annual meeting of this Society, it has been
the custom for the retiring President to deliver an address, either
upon some specialty in the domain of astronomy, or upon some
particular features or needs of our organization. The present
meeting will of necessity mark a departure from that custom, for
it is the first at which the President of this Society is allowed the
privilege of making a public award of the Bruce Medal. Follow-
ing the plan of the older societies similarly endowed, I shall
occupy your time this evening with a brief sketch of the life and
works of the distinguished American astronomer who, with the
sanction (and it might almost be said, at the command) of his
fellow scientists of this and many other countries, becomes the
recipient of the Bruce Medal of the Astronomical Society of the
Pacific ** for distinguished services to astronomy.'*
To those of you who have followed in our Publications the history
of this recendy founded medal and the regulations adopted for its
award, it will be perfectly clear that the recipient must have
endeared himself, in a scientific sense, to the astronomers of the
world. Not only will this ako be true of each subsequent
bestowal of the medal, but such a condition must especially mark
this first presentation, since, according to the desires of Miss
Bruce, the medal is to be ** international in character, and may
be awarded to citizens of any country and to persons of either
sex." It must strike us, then, with peculiar force, that of all the
50 Publications of the
names of living astronomers that have been so brilliantly con-
nected with the wonderful advances in astronomical research
during the past half century, with all the manifold branches of
observational work, mathematical investigation, spectroscopic and
photographic study in which to seek out a worthy exponent for
this distinction, one name stood forward so prominendy in the
communications from heads of six leading observatories of the
world, that the Directors of this Society could but set the seal of
their approval upon the verdict of his peers, and award the first
Bruce Medal to Professor Simon Newcomb.
The labors of astronomical research are beyond computation
in the standards by which, for example, mercantile pursuits are
judged. The preliminary study and preparation and the hard-
ships of an apprenticeship in his chosen field would make of
a man possessing the requisite mental ability of the great
astronomer a most successful business man or practitioner, whose
closing days would, in a vast majority of instances, be spent in
the luxury of an acquired competence. There are no such
pecuniary rewards for scientific devotion. There are, it is true,
many noble endowments of scientific research, by means of which
the early privations of a few successful students are in a measure
lessened and their necessary equipment secured. The scholar-
ships of a great university are an instance of this; would that
there were more of them,— such as those established by another
distinguished philanthropic woman, by means of which a certain
number of advanced students are afforded a course of investiga-
tion at the Lick Observatory of our own University. But the
idea of an award such as that which it is my glad privilege to
make on behalf of the Astronomical Society this evening, is not
intended in any sense to be a reward. It is, like the gold medal
of the Royal Astronomical Society of England, and the Lalande
and Arago medals of the French Academy, simply the expression
of sincere appreciation for a grand work well accomplished —
another jewel in the crown of immortality, which alone rewards
the unselfish devotion of a worker in the cause of science.
It was such a design which prompted Miss Catherine
Wolfe Bruce, of New York (whose previous benefactions to
astronomy are many and judicious), to establish the gold medal
of the Astronomical Society of the Pacific. I cannot do better
than to here quote one or two sentences from the original
announcement made by Dr. Edward S. Holden, who had
Astronomical Society of the Pacific. 51
previously been made the recipient of many aids to the Lick
Observatory equipment and publications from the same bene-
factress, and by whom principally were drawn up the excellent
regulations for the bestowal of this medal: —
*• Not only will the Bruce Medal tend to the advancement of
astronomy, and enable the Astronomical Society of the Pacific to
adequately recognize scientific work of the highest class (and
these are Miss Bruce*s only desires), but it will forever con-
nect the name of the founder with the progressive advances
of astronomy. Those who are knowing to her very many
and wise subventions of astronomical research (a few of which
are spoken of in these PublicaHons) will welcome this, her latest
gift, for personal as well as for scientific reasons. The Society is
to be congratulated that Miss Bruce has selected it as the Trustee
to carry out her generous desires. If the trust is executed, as it
will be, with intelligence, fidelity, and circumspection, the time
will soon come when the Bruce Medal will be one of the most
highly-prized recognitions of original and useful service to Astro-
nomical Science.*'
To members of scientific societies situated in the Eastern
States, or even in Europe, the personality of our Medalist is well
known. All the world knows of his scientific achievements. I
have therefore thought that it would be gratifying to members of
the Society if I gave, in this place, some brief account of the life
of Professor Newcomb, especially because his life exhibits, in a
marked way, the qualities which distinguish the great man of
science, who is born, not made, and who will conquer his place
no matter what the obstacles may be.
Professor Newcomb was born in Wallace, Nova Scotia, on
March 12, 1835. His family came to New England about 1660,
but removed to Nova Scotia in 1761, shortly before the breaking
out of the Revolutionary War. None of his ancestors received a
college training, but, after the fashion of the times, they were
taught in the country schools. His grandfather was a stone-
cutter by trade, and'part owner of a quarry in Nova Scotia. He
must have been a man of parts, for among the books in his
library was a copy of Euclid's Geometry, not a common posses-
sion in the simple community in which he lived. His son, the
father of Newcomb, became a school-teacher. There was but
small opportunity for a boy in the little village in Nova Scotia
where Newcomb' s family lived. Most of the inhabitants were
52 Publications of the
very poor. The men and boys sawed lumber and cut wood for
a livelihood. The women and girls sheared the sheep and wove
the wool into homespun cloth. The garments for both men and
women were made at home. Life was hard and books were few.
In his father's school young Nevvcomb began his studies at
the age of five. At six he was already fond of arithmetic, and
soon gained a local reputation for his facility in working out
arithmetical problems. At the age of twelve the boy began the
study of algebra, and about the same time he commenced to teach
others. The Euclid which belonged to his grandfather was taken
down from the bookshelves when the lad was about thirteen
years old, and there he obtained his first ideas of geometrical
demonstration. As he has himself said: "The book delighted
me. It opened up a new world of thought, and I remember
that I explained its theorems to my brother, drawing the
diagrams with a pencil on the ends of the logs of a pile of wood.*'
From Nova Scotia young Newcomb went, as a country school -
teacher to the eastern shore of Maryland, where he taught reading,
writing, and arithmetic for a year or more.
Among Professor Newcomb' s papers is to be found the fol-
lowing certificate, which was valued then, but which reads quaintly
now among the formal diplomas from the learned societies and
the universities of the whole world: —
*' This is to certify that Mr. Simon Newcomb was well quali-
fied to instruct children in the various branches of an English
education, and possesses a good moral character. He exhibited
a very considerable knowledge of the higher branches of mathe-
matics. W. J. SUDLER,
John W. E. Sudler,
Trustees for Primary School No. 4 of Q. A. Co. , for
the year ending 1855.
(Dated) Sudlersville, November 23, 1855."
At this time he sent to Professor Joseph Henry, the Director
of the Smithsonian Institution, an algebraical problem that was
new, asking him if it were suitable for publication. The problem was
submitted by Professor Henry to a mathematician, who reported
that, while the demonstration was original, it was not precisely
suited for publication. Henry, with his unfailing kindness,
replied to Newcomb' s letter and became interested in the young
man, who came to Washington at his request. I have heard
that he walked from his home to the city. By Henry's inter-
Astronomical Society of the Pacific, 53
vention, Newcomb was appointed, in 1857, to be a computer
on the American Ephemeris (Nautical Almanac), which was
then installed at Cambridge, Massachusetts. The establish-
ment was under the direction of Lieutenant (afterwards Admiral)
Charles Henry Davis, of the Navy, and Davis* relative,
Benjamin Peirce, the Professor of Mathematics and Astron-
omy in Harvard University, was the consulting astronomer of
the Ephemeris. In this new atmosphere Newcomb was soon
at home. The little brick building on the main street of Cam-
bridge, which was the headquarters of the Ephemeris, contained
a number of men of first-rate ability, and many of the officers of
the institution had already made their mark. Peirce was a
pupil and protege of Nathaniel Bowditch, and had read for
him the proof-sheets of Bowditch*s translation of the Mhanique
Celeste of Laplace as it passed through the press. Newcomb's
immediate colleagues were, then or soon afterwards, Runkle,
Ferrel, Chauncev Wright, Winlock, and others. Ken-
dall, Sears C. Walker, and Dr. Gould were coadjutors also.
The Harvard College Observatory was in active operation under
William Bond and his son. The intellectual tone of Cambridge,
then a mere village, was extremely high. Newcomb found in
his new surroundings precisely the atmosphere that was needed
for his development. During his stay in Cambridge he attended
the Lawrence Scientific School of Harvard University, from
which he was graduated in 1858.
Some of his colleagues were men of high and varied culture,
and all of them were accomplished in scientific matters. Books
there were in plenty. The Observatory was actively engaged in
original work. In native talent few, if any, of his companions
approached Newcomb, but he had something to learn from each
one of them. Perhaps his friendship with Chauncey Wright
was as close as any. Wright was not only a mathematician; he
was also a philosopher, and his friendship was highly prized.
Gould had had the great advantage of a thorough training in
Europe by the best astronomers of the period.
Newcomb* s reputation steadily grew, and in 1861 he was
appointed to be Professor of Mathematics in the United States
Navy, and one of the Astronomers at the Government Observa-
tory in Washington. Previous to this (in 1857), he had been
appointed on the staflf of the American Ephemeris.
In 1 86 1 he received his commission in the Navy, and in the
54 Publications of the
year 1877 he was appointed to be Superintendent of the Ameri-
can Ephemeris, a position which he held until his retirement in
1896. His official position and his talents brought him the
Presidency of the U. S. Transit of Venus Commission, and placed
him at the head of various boards and scientific expeditions to
observe the Transit of Venus at the Cape of Good Hope in 1882.
Professor Newcomb married a granddaughter of Ferdinand
R. Hassler, who was the first Chief of the United States Coast
Survey. Mrs. Newcomb has been a veritable helpmate during
all the years of his activity, sharing in his trials and in his
triumphs, and sparing him all the minor ills of life so far as lay
in her power. Of his three surviving children, all girls, one at
least has shown decided talent, and has taken a high degree as a
physician from a foreign university.
A few words may be said of the individuality of our Medalist
as I have learned it fi'om a personal acquaintance, which extends
back to 1873, when I was one of the Trustees of the Lick Trust
and Newcomb its chief adviser; and derived also fi'om the con-
versation of astronomers who have known him intimately, and
who honor and revere his character and attainments. It is proper
to here mention that a great deal of the preceding information
has been kindly gathered for me by Dr. E. S. Holden, whose
acquaintance with our Medalist has been lifelong and intimate.
The basis of Professor Newcomb* s character is intellectual
and moral honesty pushed to its highest degree. He loves truth
and detests shams. He has, as it were, a veritable passion for
justice— whether in personal relations or in civic matters. The
circumstances of his career have made him ruggedly independent
in thought and in speech. The essential quality of his mind is
that of a philosopher, rather than that of a mathematician or an
astronomer merely. His achievements in the pure sciences have
been very extended and extraordinary, but his work in political
economy, though not so extensive, has fully proved that if he
had devoted himself exclusively to this science, he would have
attained the very highest rank. Even as it is, he ranks among
the great names. In his treatment of all quesdons, it is the
philosophical habit of his mind which is the most remarkable and
the most valuable.
His most original investigation — a new method of investiga-
tion in the lunar theory — is marked by philosophic insight as
well as by mathematical power and astronomical sagacity.
Astronomical Society of the Pacific. 55
With all these qualities, there is a notable practicality in his
methods of work which has stood him in good stead and
enabled him to complete vast labors, which another man scarcely
less gifted might not have been able to bring to a termination.
The tendency of the practical astronomer, who is this and nothing
more, is to refine on his observations until they have been
brought to the last possible degree of attainable precision and
even carried beyond it. In all of Newcomb's work in practical
astronomy, he has kept clearly in mind the object for which his
observations were made; and when his observations were suffi-
ciently accurate, and when there was an adequate number ol
them, he has terminated the work and calculated the desired
result with the least possible delay. In this way he has saved
himself and the world much time. His results have been quickly
forthcoming. The merit is great The danger of such a pro-
cedure is, that results may be too quickly reached and accepted
on authority.
In theoretical researches the same practical tendency is mani-
fest, and corresponding results have been attained. It is due to
this faculty that the enormous task of revising the elements of the
orbits of the major planets and of tabubting them in convenient
forms has been carried through to completion in a comparatively
short time. This gigantic task would have been above even his
powers, had it not been for this practicality to which I have
referred.
In pure mathematics his work has chiefly been directed to
investigations that were suggested by the needs of astronomy as
experienced in his previous work. His mathematical thinking
has usually been along lines suggested by astronomical necessities.
On a few occasions he has made successful excursions into the
geometry of Hyper-Space. These ** fairy tales of geometry ** are
very attractive to his mind, so that he chose for the subject of his
Presidential Address to the American Mathematical Society
(1897), **The Philosophy of Geometry of Four- Dimensions.'*
His many mathematical text-books are characterized by a prac-
tical tendency which gives them great value, and at the same time
the philosophical bent of his mind has forced him to regard the
subjects treated from a high and generalized point of view.
The list of Professor Newcomb's honors is a very long one.
He is a member of nearly every Academy of Science in Europe,
and has received honorary degrees from many universities in this
5^ Publications of the
country and abroad In 1872 he was elected one of the fifty
Foreign Associates of the Royal Astronomical Society of Lon-
don, and in 1874 he received the gold medal of that Society.
In 1877 he was elected a foreign member of the Royal Society
of London, and the Copley Medal was awarded to him in 1890.
In 1877 he was President of the American Association for the
Advancement of Science, and in the same year his portrait was
ordered to be painted for the gallery of portraits of great
astronomers in the Imperial Observatory of Russia.
In 1878 he received the Huyghens Medal from Holland, an
award which is made only once in each twenty years, and then
only for the most important work of the period.
He has been corresponding member of the Academy of
Sciences of Paris since 1874, and one of its eight Foreign Asso-
ciates since 1895, ^^^ ^^ officer of the Legion of Honor of France
since 1896.
In 1897 the Imperial Academy of Sciences elected him to
membership, and in the same year he received the Schubert Gold
Medal of the Academy — a rare honor.
In acknowledgment of his services to the Imperial Observatory
of Russia in the making of its great telescope, the Czar presented
him with a magnificent onyx vase, and the Japanese Gov-
ernment has also presented him with a pair of bronze vases. He
was Vice-President of the National Academy of Sciences during
the years 1883 to 1889, and President of the American Mathe-
matical Society in 1897. ^^ ^^ ^^ adviser of the Lick
Trustees from the beginning, and it was upon his plans that the
object-glass of the great telescope was contracted lor.
For ten years he was head of the Department of Mathematics
and Astronomy in the Johns Hopkins University, and editor of
the American Mathematical Journal, This long list of honors
is more than sufficient to exhibit the estimation in which Professor
Newcomb*s magnificent labors are held. His highest praise may
be succinctly expressed by saying, what is the undoubted fact,
that he has done more than any other American since Franklin
to make American Science respected and honored throughout the
entire world.
To these high honors, which have been fully deserved, the
Astronomical Society of the Pacific adds its first award of its
Bruce Gold Medal ** for distinguished services to astronomy.'*
During the Franco- Prussian War Newcomb was at the
Astronomical Society of the Pacific. 57
Observatory of Paris engaged in examining its records for data
necessary in his researches on the motions of the principal
planets. He entered the city just as the siege terminated, and
prosecuted his work in the midst of the horrors of the Commune,
passing the barricades daily in going to and from his study at
the observatory.
Professor Newcomb is not only an astronomer and mathema-
tician. He has made a name in political economy as well. In
1865 his book, "A Critical Examination of Our Financial Policy,"
was well received. His **A B C of Finance'* (1877) had a
very large sale and was extremely useful coming at that time.
His work, ** Political Economy " (1886) is a text-book in many
colleges. A favorite saying of Newcomb' s has been, * 'Astronomy
is my profession, and political economy my recreation."
I will not attempt to here enumerate the separate works of
Professor Newcomb. His writings upon astronomical subjects
not only fill coundess pages of the leading journals, both of
this country and of Europe, but occupy whole volumes upon the
shelves of every standard library. All who have read his
•• Popular Astronomy " have been impressed with the charm of
the narration no less than with the simple and direct explanation
of the most difficult points. The concluding chapters on the
** Stellar Universe," the *• Plurality of Worlds," and the ''Nebular
Hypothesis ' ' are the reflections of a true philosopher.
Outside of his mathematical works and treatises on planetary
and lunar theories, many of which have been published by the
American Government as appendices to " Washington Astro-
nomical and Meteorological Observations " (yearly), and as " Pro-
fessional Papers of the Nautical Almanac " (periodically), Professor
Newcomb has, in addresses delivered before learned bodies, and
in contributions to the different magazines, made frequent incur-
sions upon the literature of widely different subjects. In addition
to the works upon political economy already mentioned, there
may be specified his essays upon: "Abstract Science in
America" {North American Review, January, 1876); "The
Course of Nature" {Popular Science Monthly, October, 1878);
"Formative Influence" {Forum, April, 1891); **Why We
Need a National University" {North American Review, Febru-
ary, 1895); "Science During the Victorian Era" {The Inde-
pendent, June 17, 1897); besides the addresses at the dedications
of many important observatories, the latest and perhaps most
5^ Publications of the
prominent of which was the oration upon the * * Aspects of Ameri-
can Astronomy,* ' delivered at the opening of the Yerkes Observ-
atory in October last.
He has developed the theories, and prepared tables of the
moon and all the planets, besides investigating all the principal
* * Constants * * of astronomy, and his results are accepted as
standard places of the fundamental stars, upon the accuracy of
which the reliability of the deduced planetary and lunar move-
ments must necessarily depend. And he has even found time for
an extended investigation of the theory of the asteroids.
In the opinion of Professor Holden, who for many years
prepared the Smithsonian Reviews of ** Astronomical Progress,**
and is a recognized authority upon Astronomical Bibliography,
the best thing that Newcomb has done is his **New Method in
the Lunar Theory**; and the biggest thing his ••Series of
Planetary Tables.**
Although Professor Newcomb has retired from the manage-
ment of the ••American Ephemeris,'* it is certain that his con-
tributions to astronomy are by no means ended, and that as long
as he is spared to mankind his pen will be industrious for the
ennoblement of Science, and the demonstration of Truth. A full
and complete list of his writings may well be left to more com-
petent hands at that day (which we all hope may be &r remote)
when his grand work shall have been finished, and when full
justice may be done to the vast output of that mighty intellect
When future Boards of Directors of this Society shall award
subsequent Bruce Medak, the recipients [thereof may well look
back upon this date and think that the first one was tendered to,
and accepted by, the foremost American astronomer. The first
name has been entered upon a glorious roll of honor that will
reflect credit alike upon this Society, the wise and beneficent lady
who founded the medal, and upon the achievements of those who
explore the boundless depths of the Universe.
Mr. Secretary, in the absence of our Medalist, whose presence
here, had it been possible, would have been an additional source
of satisfaction to this Society, I beg to hand you the award for
transmission to Professor Newcomb.
WILLIAM ALVORD.
San Francisco, April 2, 1898.
Astronomical Society of the Pacific. 59
PLANETARY PHENOMENA FOR MAY AND JUNE,
1898.
By Professor Malcolm McNeill.
May.
Mercury passes inferior conjunction and becomes a morning
star on the morning of May ist. It moves rapidly away from the
Sun, but toward a more southern position, so that, although its
greatest elongation of twenty- four degrees, which it reaches on
May 28th, is above the average, its southern position makes it
difficult to see. It may possibly be seen for a few days at the close
of the month near the eastern horizon in the morning twilight.
Venus is an evening star, gradually increasing its distance
from the Sun, setting about two hours later at the close of the
month. It moves nearly forty degrees eastward during the
month, through the constellation Taurus into Gemini (See Map
III), passing /i Geminorum }ust before the close of the month.
Mars is a morning star, rising somewhat earlier than during
April. It b growing a litde brighter, but has not increased very
much as yet. It moves twenty-one degrees east and nine degrees
north during the month, in the constellation Pisces, There are
no bright stars in the constellation, but it is on Map I, between
Pegasus and Cetus.
Jupiter is in good position for observation all through the
evening until after midnight, and may be found on Map III, a
little east of -q Virginis, It moves about one degree westward
until May 27th, and then moves eastward.
Saturn is getting into better position for evening observation,
rising a little before sunset at the close of the month. It may be
found on Map IV, about six degrees north and a little east of
a Scarpa. It moves about two degrees westward during the
month. It is in opposition with the Sun on the morning of May
30th. The ratio of apparent axes of the rings is about 23/100.
Uranus is near Saturn, and may be found on the same Map
IV, about eight degrees west of that planet It moves a little
more than one degree westward, and early in the month passes
fi Scarpa, less than one degree to the south of the star.
Neptune is an evening star, in the constellation Taurus, Map
III. Ve7ius passes two degrees to the north of it on May 19th.
6o Publications of the
June.
The Sun reaches its greatest northern declination, and summer
begins on June 21st, 2 a.m., Pacific time.
Mercury is a morning star until June 30th, when it passes
superior conjunction. During the first ten days of the month it
rises about an hour before sunrise, and may possibly be seen
under favorable atmospheric conditions, but it is not in very good
position for observation.
Venus increases its distance from the Sun about seven degrees
during the month, but as its motion in declination is southward,
its setting time remains about two hours after sunset throughout
the month. It moves thirty-eight degrees east and six degrees
south, through the constellations Gemini and Cancer, into the
western part of Leo^ passing about five degrees south of fi Gemi-
norum a little before the middle of the month (Map III).
Mars rises about an hour earlier than during the correspond-
ing part of April. It moves twenty-one degrees east and seven
degrees north, through the constellations Pisces and Aries, and
may be found on Map I. It passes several degrees south of the
stars in Aries, which are marked on the map.
Jupiter is still in good position for evening obser\'ation, as it
does not set before midnight until nearly the close of the month.
It may be found on Maps II or III, in the constellation Virgo, not
far from ri Virginis, and at the end of the month it is only about
one degree west and north of the star. It has moved a little
eastward and southward during the month.
Saturn passed opposition with the Sun at the end of May, and
ii above the horizon nearly the entire night. It moves about two
degrees westward, in the constellation Scorpio (see Map IV), and
is about seven degrees north of a Scorpii,
Uranus is near Saturn, about eight degrees west, on the same
Map IV. It moves about one degree westward, and at the close
of the month it is about two degrees westward and 0°. 5 south of
the star /3 Scorpii,
Neptune is close to the Sun throughout the month, and is in
conjunction with it on June 12th.
Ocailtation. The Moon approaches very close to the first-
magnitude star a Scorpii on the evening of June 3d, and there
may be an occultation of the star for places in the northern part
of the United States.
Astronomical Society of the Pacific. 6i
Explanation of the Tables.
The phases of the Moon are given in Pacific Standard time.
In the tables for Sun and planets, the second and third columns
g^ve the Right Ascension and Declination for Greenwich noon.
The fifth column gives the local mean time for transit over the
Greenwich meridian. To find the local mean time of transit for
any other meridian, the time given in the table must be corrected
by adding or subtracting the change per day, multiplied by
the fraction whose numerator is the longitude from Greenwich
in hours, and whose denominator is 24. This correction is
seldom much more than i". To find the standard time for the
phenomenon, correct the local mean time by adding the differ-
ence between standard and local time if the place is west of the
standard meridian, and subtracting \i ^2&X., The same rules apply
to the fourth and sixth columns, which give the local mean times
of rising and setting for the meridian of Greenwich. They are
roughly computed for Lat. 40^, with the noon Declination and
time of meridian transit, and are intended as only a rough guide.
They may be in error by a minute or two for the given latitude,
and for latitudes differing much from 40® they may be several
minutes out.
Phases of the Moon, P. S. T.
H. M.
Full
Moon,
May 5,
10 34 P. M.
Last
Quarter,
May 1 2,
1 36 P. M.
New
Moon,
May 20,
4 58 A. M.
First
Quarter,
May 28,
9 14 A. M.
The Sun.
R. A.
Declination.
Rises.
Transits.
Sets.
1898.
H. M.
/
H. M.
H. M.
H. M.
May I.
2 35
+ 15 ID
5 4 A.M.
11 57 A.M.
6 50 P.M.
II.
3 13
+ 17 58
4 53
II 56
6 59
21.
3 53
+ 20 15
4 44
II 56
7 8
31-
4 33
+ 21 58
4 38
II 57
7 16
Mercury.
May I.
2 34
+ 15 41
5 1 A.M.
. II 56 A.M.
6 51 P.M.
II.
2 18
+ II 31
4 20
II
5 40
21.
2 25
+ 10 42
3 52
10 29
5 6
31-
2 57
+ 13 20
3 35
10 21
5 7
«
Venus.
May I.
3 50
+ 20 24
5 59 A.M.
I 12 P.M.
8 25 P.M.
II.
4 42
+ 22 57
6 2
I 25
8 48
21.
5 35
+ 24 25
6 8
I 38
9 8
31.
6 28
+ 24 44
6 21
I 52
9 23
62 Publications of the
Mars,
R. A.
DeclinaUoo. Rise*.
Transits.
Sets.
1898.
N. M.
« ' H. M.
H.
M.
H. M.
May I.
9
— 18 3 33 A.M
9
32 A.M,
3 31 r.vL.
II.
38
+ 2 45 3 12
9
21
3 30
21.
I 6
-^ 5 44 2 50
9
9
3 28
31-
I 34
+ 8 36 2 29
Jupiter.
8
58
3 27
May I.
12 7
+ 52 3 25 P.M.
9
28 P.M.
3 31 AM.
II.
12 5
+15 2 43
8
46
2 49
21.
12 4
+ I II 22
8
6
2 10
31.
12 4
-i- I 10 I 22
Saturn,
7
26
I 30
May I.
16 39
— 20 12 9 15 P.M.
2
3 A.M.
6 51A.M.
II.
16 36
— 20 6 8 32
I
21
6 10
21.
16 33
— 20 7 50
12
39
5 28
31-
16 30
- 19 54 7 3
Uranus,
II
52 P.M.
4 41
May I.
16 I
— 20 29 8 38 P.M.
I
25 A.M.
6 I2A.M.
II.
15 59
- 20 24 7 57
12
44
5 31
21.
15 58
— 20 20 7 15
12
3
4 51
31-
15 56
— 20 14 6 30
Neptune,
II
18 P.M.
4 6
May I.
5 20
+ 21 50 7 24 A.M.
2
42 P.M.
10 P.M.
II.
5 21
+ 21 51 6 46
2
4
9 22
21.
5 23
+ 21 53 6 8
I
26
8 44
31.
5 24
+ 21 55 5 30
12
48
8 6
Eclipses of Jupiter's Satellites, P. S.
T.
(Off right-hand limb, as seen in an inverting telescope.)
H. M.
H. M.
I, R.
May I.
9 4 p. M. I, R,
May 17.
7 21 P. M.
H. R,
3.
9 I p. M. II, R,
18.
2 14 A. M.
I.R,
8.
10 58 p. M. Ill, D,
23.
9 43 p. M.
I. R,
10.
5 27 p. M. Ill, R,
24.
12 9 A. M.
11, R,
10.
II 37 p. M. I, R,
24-
9 16 P. M.
I.R.
16.
12 52 A. M. II, R,
28.
6 9 P. M.
III. D,
16.
5 44 p. M. Ill, D,
31.
I 42 A. M.
III, R,
16.
8 12 p. M. I, R,
31.
II 10 P. M.
Phases of the Moon,
P. S
T.
Full
Moon, June 4,
H. M.
6 II A. M.
Last
Quarter, June 10,
10
4 P. M.
New
Moon, June 18,
8 19 p. M.
First
Quarter, June 26,
8 54 P. M.
Astronomical Society of the Pacific.
63
The Sun.
R. A.
Declination.
Rises.
Transits.
Sets.
I89S.
N. M.
'
H. M.
H. M.
H.
M.
June
I.
4 38
+
22 6
4 39 AM-
II 58 A.M.
7
17 P.M.
II.
5 19
+ 23 7
4 35
II 59
7
23
21.
6
+
23 27
4 37
12 2 P.M.
7
27
July
I.
642
+ 23 6
4 40
12 4
7
28
Mercury,
June
I.
3 I
+
13 44
3 34 A.M.
10 21 A.M.
5
8 p.m.
II.
3 57
+
18 26
3 32
10 37
5 42
21.
5 15
+
22 56
3 53
II 16
6
39
July
I.
6 49
+ 24 24
4 40
12 10 P.M.
7
40
Venus.
June
I.
6 33
+ 24 42
6 22 A.M.
I 53 P.M.
9
24 P.M.
II.
7 26
+ 23 42
6 41
2 7
9
33
21.
8 17
+
21 35
7 I
2 18
9
35
July
I.
9 6
+
18 30
7 23
Mars.
2 28
9
33
June
I.
I 37
+
8 53
2 26 A.M.
8 57 A.M.
3
28 P.M.
II.
2 5
+
II 34
2 5
8 45
3
25
21.
2 33
+
14 2
I 46
8 34
3
22
July
I.
3 2
+
16 16
J
I 26
'U PITER.
8 23
3
20
June
I.
12 4
+
I 9
I 18 P.M.
7 22 P.M.
I
26A.M
II.
12 5
+
I
12 41
6 44
12
47
21.
12 7
+
44
12 5
6 7
12
9
July
I.
12 10
+
21
ri 30 A.M.
5 31
II
32
Sa turn.
June
I.
16 30
—
19 54
6 59 P.M.
II 48 P.M.
4 37 A. M,
II.
16 27
—
19 48
6 15
II 5
3
55
21.
16 24
—
19 42
5 33
10 23
3
13
July
I.
16 21
—
19 38
4 50
9 41
2
32
Uranus,
June
I.
15 56
—
20 14
6 26 P.M.
II 14P.M.
4
2 A.M.
II.
15 55
—
20 9
5 44
10 33
3
22
21.
15 53
—
20 5
5 3
9 52
2
41
July
I.
15 52
—
20 I
4 23
9 12
2
I
Neptune.
June
I.
5 25
+
21 55
5 25 A.M.
. 12 44 P.M.
8
3P.M
II.
5 26
+
21 56
4 47
12 6
7
25
21.
5 28
+
21 58
4 10
II 29 A.M.
6
48
July
I.
5 29
+
21 59
3 32
10 51
6
10
64 Publications of the
Eclipses of Jupiter' s Satellites, P. S. T.
(Off rixht hand limb, a* seen
in an inverting telescope.)
I, R.
June 2.
R. H.
6 39 p. M.
II. D.
JuiM
•18.
R. M.
II 33 P. M.
II, R,
I. R.
I. R.
II, D.
4-
8.
9-
II.
8 45 p. M.
I 5 A. M.
7 34 P. M.
8 56 p. M.
I. R.
I, R.
HI, D,
III, R,
23-
25-
28.
28.
II 23 p. M.
5 52 P- M.
5 41 P- M.
8 I p. M.
II, R,
II.
II 22 p. M.
II, R,
29.
5 51 P- M.
I. R.
i6.
9 29 P. M.
LIST OF EARTHQUAKES IN CALIFORNIA FOR
THE YEAR 1897.
Compiled by C. D. Perrine.
The following list is a continuation of similar reports printed
in these Publications: Vol. II, p. 74; Vol, III, p. 247; Vol. V,
p. 127; Vol. VI, p. 41; Vol. VII, p. 99; Vol. VIII, p. 222, and
Vol. IX, p. 37. A more complete account will be published by
the Unites States Geological Survey as a bulletin. The dates
are civil dates. The times are Pacific Standard (120th meridian).
Roman numerals enclosed in parentheses indicate the intensity
on the Rossi- Fore L scale.
Some doubtful cases have been included, and are indicated
either by a note or by an interrogation point enclosed in paren-
theses.
In 1 897 there were twenty-five shocks of earthquake recorded
in California as against sixteen for the year 1896.
The shock of June 20th was accurately timed at Mt. Hamilton
and Oakland, and as we know approximately the center from
which the disturbance radiated, we can obtain the velocity over
this part of its path. At Mt. Hamilton the beginning was noted
at 12*" 12" 56' P.M., P. S. T., by several observers, and Mr. Bab-
cock obtained 12** 13"" 9" as the time of the same phase in
Oakland, an interval of thirteen seconds. Assuming the epicen-
trum to have been between San Juan and Salinas, we find Ml
Hamilton to be forty miles from this point, while Oakland is
eighty miles. As both points lie nearly in the same direction
from the origin of the disturbance, differing only twenty degrees,
we may assume that the disturbance moved with the same velocity
April
24.
May
II.
January
2.
June
28.
October
II.
April
19.
April
21.
July
26.
Astronomical Society of the Pacific. 65
towards both stations^ from which we find the velocity between
Ml Hamilton and Oakland to be 3j^^ miles per second.
This is an unusually high velocity, and in this connection it
will be interesting to note the intervals in the cases of other
shocks, which have been timed with sufficient accuracy.
1889. July 31. L. O.-East Oakland, + ii'
L. O.-San Francisco, + 7"
1890. April 24. San Francisco-San Jos6 (U. P.), — 40'
San Francisco-East Oakland, ±l o*
1891. January 2. L. O.-San Francisco, — 22"
L. O.-San Jos6, — 12"
L. O.-San Francisco, — lo'
San Francisco-Oakland, — 17"
1892. April 19. L. O. -Carson, Nev., — 70' d=
San Francisco-Reno, Nev., — 107*
1896. July 26. L. O.-San Francisco, -f 15'
The April, 1892, shocks had their origin in the great central
valley of California, and we may safely take a point near Vaca-
ville as the epicentrum of both disturbances. Assuming that the
velocity was the same at eqiM distances from this pointy we find,
for the shock of April 19th, an average velocity of 0.8 miles per
second for a distance of fifty-six miles from Carson, Nevada,
measured towards the center of disturbance. The interval of
time of seventy seconds is somewhat uncertain, perhaps ten
seconds or fifteen seconds. For the shock of April 21st, we find
an average velocity of 0.8 miles for ninety miles from Reno.
The epicentra for the other cases are entirely too uncertain to
base any velocities upon.
List of Earthquake Shocks, 1897.
January i. Berkeley, 1:10 p.m.
January 11. Oaxaca (Mexico), 4:25 p.m.
January 16. Mt. Hamilton, 3' 58" 38' a.m. (I).
January 17. San Francisco, i' 9" p.m.; Alameda, i' 11" p.m.;
Oakland, i** 11- ii' p.m. (A. H. B.), i^ 10- 55" ± 2' (G.
R. L.); MiUs College, i^ ii"p.m.
January 26. Newport, Alsa Bay (Oregon), 2*" 45" p.m.
February 2. Tomales.
February 5. Orizaba Volcano (Mexico).
February 13. Colima, Tepic (Mexico).
66 Publications of the
February i8. Mt Hamilton, 8* 3" 52' ± 5' p.m. (I) C. D. P.;
S** 4" 30' ± P.M. (II) E. S. H.
The above are two separate shocks. C. D. P.
February — . Cacaluta (Mexico).
February — . Great Salt Lake (Utah). (?)
March 6. Acapulco, Vera Cruz, Oaxaca, Orizaba, Cordoba
(Mexico), 7** 30" P.M.
March 13. Mt Baker (Wash.) (?)
March 15. Ukiah, ii** p.m.
March 15. Highland Springs, Pieta, Lakeport, 10** 51" p.m.
Reported by Mr. Wm. B. Collier.
April 10. Mexico, south of Oaxaca.
May 14. Moro Bay. (?)
May 14. Reno (Nevada), 6 P.M.
May 15. San Diego, 4 A.M.; Carson (Nevada), 11:04 ^*'^'
May 22. San Diego, 6:58 a.m.
June 20. A heavy shock of earthquake was felt generally
throughout the central portion of California shortly after
noon. The center of the disturbance seemed to be in the
Salinas Valley. Considerable damage was done to buildings
in towns in this and neighboring valleys. Mt Hamilton,
j2»» i2» 56' (beginning). Duration, 20*-30* (V); College
Park; Mills College, reported by Professor Keep; Oakland,
i2*» 13" 9' to 13" 34" P.M., reported by Mr. A. H. Babcock;
Cantua Creek (Fresno Co.), reported by Mr. S. C. Lillis;
San Jos6; Gilroy; Hollister; Salinas; Los Gatos; Santa
Cruz; Templeton; Monterey; Pacific Grove; Stockton;
Modesto; Newman; Merced; Visalia; Milton; Santa Rosa;
Haywards; Decoto; Sacramento; Watsonville; Hanford;
San Francisco, 6:37 a.m., 12:15 p.m., 12:48 p.m.; Gonzales;
Fresno; Redwood City; San Rafael.
June 20. Tehuantepec (Mexico).
June 21. Gilroy, 5:15 a.m.; Salinas.
June 24. Santa Barbara, 6:10 a.m.
June 26. Tehuantepec (^Mexico).
June (26 ?). Douglas Island (Alaska). Volcano.
June (27?). *'Saw Miir' Peak, Butte Co. (?)
July 19. Santa Barbara, 11:45 P-M.
July 26. Mt. Hamilton, ^ 40"* 50' p.m. (Ill) E. S. H. ; San Fran-
Cisco, 5^40^35' P.M., reported by Professor George David-
son; Berkeley; Oakland.
Astronomical Society of the Pacific. 67
September 27. Olympia (Wash.), 1:30 a.m.
October 2. College Park, S** 41" 57*.3 a.m., reported by Pro-
fessor H. D. Curtis; San Francisco.
October 5. Stockton, 7:44 p.m.
October 17. Mt Hamilton, 3** 30" 26"-3i" p.m. (Ill); San Jos^.
November 21. Randsburg, 11:30 A.M.; 12:30 P.M.
December 6. Forest Grove (Oregon), 8:30 p.m.
December 10. Mt. Hamilton (in night).
December 15. Waterville, Lakeside (Wash.).
December 16, 17, 20. Lakeside (Wash.), 6 a.m.
December 23. Mills College, 5:15 A. m. Reported by Professor
Keep.
December 26. Centerville, 7:06 a.m.
LATITUDE WORK WITH THE FAUTH TRANSIT
INSTRUMENT OF THE LICK OBSERVATORY.
By Hbber D. Curtis.
At the suggestion of Dr. Holden, I last summer entered
upon a triad of the four-inch Fauth transit of the Lick Observ-
atory to detenniiie its value as a zenith telescope for finding the
latitude.
The latitude level found in place upon the transit ^-as rejected
because of irregular curvature. After tests on all the level-tubes
in the possession of the observatory, the tube •*Repsold, No.
1491 '* was selected as being the most regular. Nearly six hun-
dred readings were made on the Repsold level-trier belonging
to the observatory, to determine the value of the division of this
level, at temperatures ranging from 45^ to 83° F. It was found
to be a tube of very regular curvature.
In reversing the transit with the aid of the carriage, it is
necessary to place the telescope in a horizontal position, thus
bringing the level-tube to a position greatly inclined to the hori-
zon, invariably shortening or lengthening the bubble, and making
it necessary to bring back the bubble tp a more moderate length.
It therefore became necessary to determine whether any factor of
change in the value of a level division could be found to depend
upon change in bubble length. Accordingly the length of the
68 Publications of the
bubble was varied in the different series of trials from 14*47 mm.
to 45.90 mm. The resulting equations of condition gave, as a
value of this factor, o".ooo4 (L — 28.3 mm.) — practically zero.
The temperature &ctor was much more interesting. Above
52° the value of one division may be represented by the formula, —
d = i".358 + (6o°-r^) o".oo2.
Below 52° (no opportunity was found below 45°) the change is
much more rapid, all values being best satisfied by the formula, —
d=i".374 + (52^-T°)o".o2i.
The probable errors of all the mean values of the different series
used in the formation of these equations are small, in only one
case exceeding o".oo5. The tube was twice removed from its
enclosing tube, and tried without it, to determine whether any
strain in the mounting caused the curious increase below 52°.
Some internal strain in the glass seems the best explanation.
No evidence was found, from a considerable number of transits
of stars, to warrant altering the assumed value of one revolution
of the micrometer screw : 2'. 931 = 43". 96. Tests were, however,
made on the micrometer screw for periodic error. The microm-
eter box was placed on the measuring engine, and set at quarter-
revolutions, from — 20 to + 20 revolutions. At each setting
four bisections were made with the microscope of the measuring
engine, and the averages of these sets of readings were so grouped
as to bring all readings of the same quarter-revolution of the
micrometer head together. The screw of the micrometer, as
well as the screw of the measuring engine, worked against the
springs. The following values were found (in terms of one
revolution of the measuring engine micrometer screw) : —
0.00 to 0.25 i'.2i89
0.25 to 0.50 I .2195
0.50 to 0.75 I .2231
0.75 to 1. 00 I. 2238
Mean, 1.2213 ±l o.ooio
This periodic irregularity is entirely insensible; the maximum
variation between readings in the first and fourth quadrants, due
to this cause, would be but o".02i, and, in the long run, the
resulting errors would tend to balance each» other. There was
no evidence of variation in the screw at different portions of its
length.
X
>
C
<
>
at.
<
>
O
Astronomical Society of the Pacific. • 69
The latitude observations themselves show that the instrument
as it stands is not well adapted for use as a zenith telescope.
As it b now arranged, much time is lost in reversal, and the
greatest care must be taken, else the latitude level, which is a
later addition, will strike the clamp. The fact that the level-tube
must be greatly inclined to the horizon in reversing, is most
objectionable, as errors are almost certain to be introduced.
With some arrangement by which the reversal could be easily
and rapidly accomplished without altering the inclination of the
telescope, this instrument would doubtless give good results in
latitude work.
In all. after rejecting numerous obviously erroneous observa-
tions, 116 were used.
The resulting value of the latitude of the transit instrument
was found to be 37° 20' 24".4, with the large probable error of
dbo".3i.
University of the Pacific,
College Park, Cal., February, 1898.
THE ROYAL OBSERVATORY, EDINBURGH,
SCOTLAND.*
By R. G. Aitken.
About the middle of 1888 the Earl of Crawford and Balcarres
offered to the Government, for use in a national Scottish observ-
atory, the splendid and valuable equipment of his own observatory
at Dun Echt.
The Government accepted the gift; but the space available in
the Royal Observatory on the Calton Hill being entirely inade-
quate for the housing of the instruments, a new building became
necessary; and eventually the present site of three and one half
acres on the eastern slope of Blackford Hill was chosen. The
plans of the new observatory were prepared by Mr. W. W.
Robertson, of Her Majesty's Board of Works, and the build-
*This description is based upon an article by Mr. Thomas Hbath, B. A., Assistant
Astronomer. Royal Observatory, Edinburgh, read before a meeting of the Royal Scottish
Society of Arts, November 33, 1896; a letter from Mr. Heath to Professor Holden ; and
an article in the Scotsman, April 4, 1892. Many of the sentences are directly quoted from
one ct another of these papers.
70 Publications of the
ings erected by Messrs. W. and J. Kirkwood, of Edinburgh, at
a cost, including fittings, of about ;^34,ooo.
The buildings consist of an observatory proper and transit
house, placed along the north front of the site, and two detached
residences for the Astronomer Royal and his assistants. The
observatory proper consists of a T-shaped building, with a front-
age toward the north of i8o feet. The flat-roofed central build-
ings are flanked by octagonal towers of unequal size, crowned
with cylindrical domes of copper — the larger, 75 feet high and
40 feet in diameter, placed at the east end; and the smaller, 44
feet high and 27 feet in diameter, placed at the west end. These
towers contain the two large equatorial telescopes — the 15-inch
refractor from the Dun Echt Observatory being placed in the
eastern or larger tower, which from its height allows the tele-
scope to sweep the entire horizon; and the 24-inch reflector
from the Calton Hill Observatory in the western tower, where it
will command the horizon, except for the part cut off" by the
larger tower. The piers are built of brick, and are hollow,
affording room in the larger one for a vault, in which the two
standard sidereal clocks are placed, to be protected from any but
the most gradual changes of temperature. In addition to this
precaution, one of the clocks, known as the Brisbane clock, has
also been enclosed in an air-tight case, in order to avoid errors
arising from changes of atmospheric pressure. The inner air is
partly exhausted until the barometer within the case reads twenty-
five inches, at which reading the barometer is to be kept By the
aid of a stuffing box containing quicksilver, the clock is wound
without opening the case.
The 15-inch equatorial is completely equipped with the most
modern apparatus for every kind of astronomical work — a series
of eyepieces of different powers, a micrometer of the most perfect
construction, a Zollner astrophotometer, and several spectro-
scopes, one of which is among the most powerful in existence.
It was with the last-named instrument, designed by himself, that
Professor Copeland was enabled to make the very notable dis-
covery of the presence of helium in the great nebula of Orion,
Up to the date of this discovery, all that was known of helium
was that it caused a certain line to appear in the spectrum of
the Sun.
The central range of buildings between the towers is devoted
to laboratory rooms for astrophysical work. The flat roof of
THE 15-INCH EQUATORIAL REFRACTOR.
Royal Observatory, Edinburgh.
J THE NEW YOHK
PUBLIC LIBRARY
ASTOR, LF\'^X
TILDEN f-Oir,- .
Astronomical Society of the Pacific. 71
this portion of the building facilitates communication between
the domes, and affords room for numerous meteorological instru-
ments. On the main floor, beginning at the west end, are, (i)
the spectroscopic room, to the south of which, outside the build-
ing, is placed a heliostat, by which the Sun's rays are reflected
into the apartment through a lo-inch aperture; (2) the experi-
menting room, shown in one of our illustrations, which has three
isolated pillars, supporting the mean time clocks, the dividing
engine, the photographic measuring engine, and other instru-
ments for delicate measuring operations; (3) the electric room,
containing the large stock of electrical apparatus from the
Dun Echt Observatory, the meteorological registering apparatus,
etc, and (4) a mechanic's workshop and the chronograph room.
The basement is occupied by stores, workshops, and printing
room.
Southward from the central building extends a wing, 80 feet
long, 28 feet wide, and having three floors. The basement floor is
occupied by the heating plant and rooms for the electric dynamos
and accumulators. The principal floor contains the Crawford
Library, one of the finest astronomical libraries in the world. Its
shelves are specially rich in cometary literature. They contain,
also, sets of the scientific publications of most of the astronomi-
cal societies and observatories in the world, the majority of the
sets being complete from their beginning. Besides the library,
this floor contains the Director's rooms and computing rooms.
The top floor is one long apartment, used in connection with the
14-inch FoucAULT siderostat, the hut containing which may be
noticed on the central roof in both of the accompanying exterior
views.
Eighty feet west from the main building and in line with the
northwest front is placed the transit house, which is connected
with the main building by a covered way. Here is placed the
meridian circle from the Dun Echt Observatory, with telescope
of 8.6 inches aperture, and the necessary collimators. This
instrument is not exceeded in size and power by any in the
world.
In addition to these instruments the observatory is supplied
with a magnificent collection of minor instruments, so that it is
completely equipped for the most thorough and advanced astro-
nomical work, and ranks easily as an observatory of the first
class.
72 Publications of the
A NEW VARIABLE STAR.
By Torvald Kohl.
The star No. 121 in Birmingham's Catalogue, = No. 144
in Chandler's Catalogue of red stars, — position for 1875.0:
5^ 38- I2'.47 (+ 3'. 57). + 20° 38' 24''.9 (+ i''.9)— has shown
a remarkable change in brightness. It has formerly been esti-
mated as a star of the 7.5th magnitude (B. D. has 7.7, Berlin
A. G. Catalogue has 7.2). Dreyer observed it at Dublin from
1875 to 1879, and I at Odder from 1887 to 1893, without seeing
any change of light in this orange-red star until on January 22,
1898, when I was surprbed at the faintness of the star, which is
now of about the 9th magnitude, and thus it has also been seen
on the dates January 27 and 31 and February i, 1898.
Odder, Denmark, February 6, 1898.
MAGNIFYING RATIOS OF EWING SEISMOGRAPHS
' OF THREE COMPONENTS. AND OF THE
DUPLEX-PENDULUM SEISMOGRAPHS.
By C. D. Perrine.
In the following deductions the jJen and plate are assumed to
move with respect to the steady-point, and the motions of each
are considered separately. In the reduction of the recorded
displacements given by the pens upon the smoked glass plate, to
the actual displacement of the Earth particle, there are several
circumstances to be taken into account. In the case of the two
horizontal components there are four considerations, viz: —
A, — The ratio of the pens, /. e. the distance from the point of
the pen to the steady- point, divided by the distance from the
steady- point to the point of support.
B, — The angle which the meridian of the pens makes with the
true meridian of the place. If they coincide, there is no factor to
be introduced on that account.
C — The angle which a radius of the circular plate drawn
through the point of the pen makes with a line drawn through
THE 24-INCH NEWTONIAN REFLECTING TELESCOPE.
Royal Observatory, Edinburgh.
THE NEW YORK
PUBLIC LIBRARY
A^tUh, LENOX AND
Astronomical Society of the Pacific. 73
the point of the pen and the steady-point. If this angle is ninety
degrees, there is no factor to be introduced on this account.
D. — The effect on the record caused by the motion of the
record-plate itself, due to the earthquake.
Let a = the record of the N. and S. pen as it appears upon
the plate.
b = the record of the E. and W. pen as it appears upon
the plate.
d = distance from steady-point to point of support of pen-
dulum.
e = distance from steady-point to point of pen.
X = angle which the meridian of the pendulums makes
with the true meridian of the place.
>^and>^' = angle between the direction of the pen-arm and a
radius of the plate drawn through its point for the N.
and S. and E. and W. pens, respectively.
z = angle which the radius of the plate drawn through the
point of the pen makes with the true meridian of the place,
a = actual displacement of the Earth N. and S.
fi = actual displacement of the Earth E. and W.
A, — The ratio of the pens is the ratio of the distances from
the steady-point to the point of the pen, and from the steady-
point to the point of support — in the instruments we are especially
considering, the line joining the steel points which bear in the
agate cups. Theoretically, the steady -point, or rather line, is the
vertical line through the cylindrical weight about which the force
of gravity is symmetrical. Practically, there is a little uncertainty
as to the exact location of the steady-point — which, however,
will be very near the axis of the cylindrical weight.
This ratio is given by the formula: —
e
B.^The horizontal pendulums should be so adjusted that
their meridian coincides with the true meridian of the place, t. e,
that the plane (^) passing through the points of support and the
steady-point of the pendulum, in the case of the E. and W. pen-
dulum, should coincide with the meridian; in the N. and S.
pendulum, thb plane should lie E. and W.
If, however, there is no such coincidence, and the meridian of
74 Publications of the
the instruments makes an appreciable angle (x) with the true
meridian, then the displacements of the pendulums in the true
co-ordinates by the earthquake will vary with this angle. If the
direction of the Earth* s motion which it is designed to register
is not normal to the plane (^), then the recorded motion will be
less than it should be in the ratio of cos x w,
C — If the horizontal pens are so situated that when at rest
the radii of the plate passing through their points are tangent to
the arcs described by them, then no factor is to be introduced on
this account. Otherwise the displacement measured on such a
radius will be too small in the proportion cos_y : i.
D, — The plate upon which the record is made is, of course,
carried about by the Earth in its movements, which must be
taken into account in deducing the actual motion of the Elarth
from the records of the pens.
In horizontal pendulums where the angle (^) between the
lines drawn from the steady-point to the point of the pen, and
from the steady-point to the point of support, is greater than
ninety degrees, it can be shown that the motion of the plcUe due to
the earthquake will be additive to the perCs motion^ thus increas-
ing the record of the pen, the plate being carried under the
pen in an .opposite direction to that in which the pen is moving.
On the other hand, if the angle (^) is less than ninety degrees, the
effect will be the opposite, /. e, to decrease the pen's record.
Thb assumes that the pendulums are not far out of adjustment
with respect to their meridians. In the Lick Observatory instru-
ments the angle (^) is greater than ninety degrees, hence the
effect is to increase the record. This b true for both co-ordinates-
The component motion of the plate N. and S. as projected on
a radius depends upon the angle •{£) which that particular radius
makes with the meridian, and varies as the cosine of that angle.
The component motion of the //a/^ E. and W. as projected on
the radius passing through the point of the E. and W. pen will
vary as the sine of the angle {z).
From the foregoing we deduce the following formulae for the
reduction of the observed records to the true displacements of the
Earth:—
a e cos ;r sin r , ^
- = -^ ± cos Z, (I.)
b e cos ;r sin y' . , .
^ = 2 ^ sm z, (2.)
THE TRANSIT CIRCLE, ROYAL OBSERVATORY, EDINBURGH.
THKKr.,'/ -,
r^: »
PUBLIC!;:,-
AS", (;■!, L:
T .L'N r ..
Astronomical Society of the Pacific. 75
Professor Schaeberle suggests that we may ako consider the
plate and supports of the pens as one rigid system,, and the steady-
point to move with respect to this system.
Let /= distance from point of pen to point of support of
pendulum, and, as before, d^= distance from steady-point to point
of support of pendulum.
Then, on the above assumption, it can be shown that,
- = 1 = 5- (3.)
a /3 a
so long as the instrumental meridian coincides with the true
meridian of the station, and the radius of the plate passing
through the points of the pens is normal to the lines passing
through the points of the pens and their points of support. If|
however, the instrument is not in adjustment in these two par-
ticulars, due allowance must be made for such variations.
THE VERTICAL COMPONENT.
In the mechanism for recording the Earth's vertical motion,
the pen proper is jointed to a vertical arm, which in turn is
fastened rigidly to the counterpoised pendulum. The lifting by
the Earth causes the joint between the pen-arm and the vertical
arm to be displaced in the arc of a circle, whose center is the
steady-point of the pendulum. This displacement is resolved into
a horizontal component (^), which leads to the magnified record
on the plate, and a vertical component (/).
Let h = distance from steady-point to point where pen-arm is
hinged to vertical arm.
i = distance from point of support to hinge of pen-arm.
j = distance from steady-point to point of support of pen-
dulum.
m = angular displacement of the hinge of pen-arm from the
steady-point as a center.
n = angle included between the lines drawn from pen-arm
hinge to steady-point, and from pen-arm hinge to point
of support of pendulum.
s = horizontal component of the displacement of pen-arm
hinge.
/ = vertical component of the displacement of pen-arm
hinge,
y = vertical displacement of the Elarth.
7^ Publications of the
c = the record of the vertical pen as it appears upon the
plate.
m and n are found from
sin m = ^, (4.)
J
tan « = 4, (5O
and we find j and / from
h sin Tfi fy/ , \ />- \
s = _ — cos Cj4 m + «), (6.)
cos }i m
/= — — sm (>^ w 4- »), (7-)
' cos Yi m
For ordinary dbplacements of the Earth {m being always
small) we may write (6.) and (7.) in the following forms: —
s =^ h sm m cos «, (8.)
i =z h sin m sin «, (9.)
It will be seen that the pen-arm hinge is lifted a little higher
by the Earth's motion than the plate itself. Thb causes the
pen's record on the plate to be shortened slightly.
In a seismograph of the usual form the dimensions are such
that so long as the pen- arm makes but a small angle with the
plane of the plate, this factor will be small.
To compute the amount of thb shortening, we have the
following quantities in a right triangle.
a^ = distance from point of pen to hinge of pen-arm =
hypothenuse.
y = perpeodicular let fall from hinge of pen-arm to
plate.
c^ = dbtance from pen's point to foot of perpendicular =
base of triangle.
A\ B\ C = angles opposite given sides respectively, A^ being
the right angle.
We find B' from
sin B' = --' (10.)
a
and we have (approximately)
^c' = -SESL^, (X,.)
cos B'
the:,!-;// YORK
PUBLIC LIBRARY
.y(
A6TCR, Lr
Astronomical Society . of the Pacific. 77
in which A ^ is the decrease in the record due to the increase
(A y) in the distance from pen-arm hinge to plate as a result of
the lifting of the instrument by the shock.
For the Lick Observatory instrument we have: —
«' = 5^75.
*'=i^75.
Using this data, I have computed the shortening of the record
due to this cause, and find it to be only o'".oi4 for a vertical
motion of the Earth of o*".5o. Hence it will be seen that for
shocks likely to be observed with these instruments, this effect
may be ignored without sensible error.
If in equation (8.) we substitute for h cos n its equivalent /,
and for sin m its equivalent \ we find (approximately),
s /
T T'
It can be shown that the same result follows from considering
the motion to be about the support of the pendulum as the axis.
Finally we have for the magnifying ratio of the vertical pen,
- = - + A r', (12.)
y y
in which A c^ may be neglected, as shown, or with sufficient
accuracy,
-^ = 4, (13.)
y J
For the Lick Observatory instruments we have the following
data: —
^= 3.75 inches, *
^ = 13.0 inches,
y = 76^
z = 38^.5,
k = 10.3 inches,
t=g,o inches,
J = 5.0 inches,
from which we derive the following ratios: —
— = 4.11, (N. andS.)
a
A= 3.97, (E.andW.)
— = 1.8. (Vertical.)
7^ Publications of the
The date given above and the constants deduced from them
are suitable for the reduction of observations from April, 1893, to
date.
MAGNIFYING RATIO OF THE DUPLEX SEISMOGRAPH.
In the ordinary form of this instrument there are two circum-
stances to be considered as affecting the magnification of the
Eartk's motion, viz: —
I St. The nciagnifying ratio of the vertical arm which is given by
a"
in which
a" = distance from lower end of vertical arm to level
of glass plate;
^" = distance from lower end of vertical arm to gimbal
joint of bracket
2d. The motion of the plate itself during the shock. It catt
be shown that the motion of the plate itself tends to decrease the
record by the amount of the Earth's motion. Hence we have
the following formula for the magnification: —
^"
(14.)
In the Lick Observatory instrument of this class we have,
a"= 13'". 10,
f = 2 .35.
and consequently the magnifying ratio = 4.6.
Owing to uncertainties, such as the fnction of the pen upon the
plate, the friction of the pendulums at the point of support, the
probable motion of the steady- point itself after a few seconds, and
other minor causes, it is not necessary to take into account al 1
the lesser factors affecting the magnification of the record. All
that is here attempted is to include those which have a practical
effect. I have not been able to find the formulae for these
reductions in any publication on the subject here.
Mt. Hamilton, Cal., March 14, 1898.
Astronomical Society of the Pacific, 79
VERY BRIGHT METEOR, MARCH 4, 1898. 1
Observed by H. D. Curtis.
A very bright meteor was observed at College Park, March 4,
1898, 9* 50" 30' P. S. T., moving from a = 13* 40", 8 = + 25°
to a = 15* 40", 8 = + 40° Its path lay through the constella-
tion Bootes^ between the stars j3 and 8. At a point just a little
west of the line joining these two stars, there was a small but
abrupt angle in its path, inclining towards the south. Several
small meteors passed in almost exactly the same track during the
next hour.
ELEMENTS AND EPHEMERIS OF COMET b, 1898
(PERRINE).
By R. T. Crawford and H. K. Palmer.
The following results were obtained from Mount Hamilton
observations of March 20th and 2 2d and an observation taken
at Berkeley on March 23d: —
T= March 19.0580, G. M. T.
i= 72° 51' 42")
0= 263 15 31 V Mean Equinox 1898.0.
ft) = 49 28 52 )
^= I.I02I.
(O.— C.) AX cos ^ = -4".7 A^ = + 4". 7.
Constants to the equator: —
X = [9-54097] sin ( 27° 37' 25" + V) sec' y^ v.
y = [0.04218] sin (295 8 42 •\- v) sec' J^ v,
2r= [0,01954] sin ( 24 52 17 + v) sec* ^ v,
Ephemeris (Gr. Mean Midnight): —
1898. App. a. App. «. Brightness.
March 29.5 21*55" 9' +26° 29' 29" 0.99
April 2.5 22 12 4 30 26 49 0.96
6.5 22 29 56 34 12 41 0.91
10.5 22 48 45 37 43 53 0.86
The brightness is expressed in terms of the brightness at the.
time of discovery.
University of California,
Students* Observatory, March, 1898.
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Astronomical Society of the Pacific. 8i
NOTICES FROM THE LICK OBSERVATORY.*
Prepared by Members op the Staff.
A Lunar Landscape, Photographed at the Lick
Observatory.
The original negative from which the Moon-plate (given in
the present number of our Publications) was made, was taken on
December 31, 1897, with an enlarging lens, (magnifying the
principal focal image eight diameters), attached to the 36-inch
refractor.
The exposure time was from 7** 58"* 30" to 7'' 58°* 50", P. S. T.
The error in the clock-rate and the motion in declination were
counteracted by giving to the plate a single uniform motion by
means of a screw turned by hand, the required velocity and
direction of motion having first been determined by actual obser-
vation of the enlarged focal image.
The scale of the published plate (Moon's diameter = 40 inches)
is the same as that of the original negative.
We have satisfactorily enlarged portions ot some of our nega-
tives to a scale of sixty feet to the Moon's diameter.
J. M. S. and C. D. P.
The Lick Observatory Eclipse Expedition.
[Extracts from a letter by Professor W. W. Campbell.]
•'The story of the eclipse is too long to tell in a letter. I
had to locate in level country^ in a famine district^ water scarce^
dust plentiful, the plague on both sides of us. There were no
habitable buildings nearer than fifteen miles, so camping was a
matter of necessity. The difficulties were great, but I kept my
* Lick Astronomical Department of the University of California.
82 Publications of the
courage up, and was all ready for the eclipse on January i6th.
The assistants — fine ones — arrived firom January 17th to 20th,
and were drilled to the work. There had not been a cloud in
the sky for six weeks, and eclipse day was simply beautiful. The
* seeing* was fair that day, though it had been poor — Sun
boiling — on all previous days.
**The eclipse began within half a second of my predicted
chronometer time, and closed in the same manner. No wind
existed, though I was prepared for wind. The corona had great
extent, but was faint as a whole. The prominences were numer-
ous, but vastly smaller than in 1893. The sky was very^ very
bright Animals paid very little attention to the eclipse. Three
miles away, on the horizon formed by a low ridge, I saw the
small trees with perfect distinctness during totality.
** The 40-foot telescope gave —
1 instantaneous Seed 27 plates.
2 one-second ** ** **
2 two-second ** ** **
2 four-second ** ** **
2 eight-second ** ** **
I sixteen-second ** ** ** (defective plate).
I instantaneous Carbutt B plate (very little on plate).
I one-second ** ** (very little on plate, and
was caught by the Sun).
** There were eight beautiful negatives with the Dallmeyer
and with the Floyd. The spectrum of the Sun's edge was
fainter than I expected, but the plates are pretty successful and
valuable.
** But I '11 save the rest of the story till I get home. I had a
great struggle with the dust and the heat in developing the
plates. I had to have the dark-room in a tent, temperature 94*^
Fahr. in the daytime. Had to wait till i a.m. to begin develop-
ing. And the dust was awful, too. The water was absolutely
muddy — had to be boiled and filtered. I never saw such dry
climate. Some days the dry bulb was +32° C, and the wet
bulb +18° C, or even +17° C. My hands were cracked wide
open, and I could scarcely finish the development of the origi-
nal plates, to say nothing of making copies.''
These extracts from Professor Campbell's letter to Professor
ScHAEBERLE are printed here, as they will be of general interest
to the members of the Society. R. G. A.
Astronomical Society of the Pacific. 83
The Companions to Aldebaran.
I have recently made the following set of measures of the two
companions to Aldebaran: —
A and B = /3 550.
1898.10 109°. 7 31". 30 36-inch telescope 3 nights
A and C = S 2 (App. II).
1 898. 10 34°. 3 11 7". 90 1 2-inch telescope 4 nights
Cand D = j3 1031.
1898.10 275° 2 i".62 36-inch telescope 2 nights
These measures give additional confirmation to the conclusions
stated by Mr. Burnham in 189 i :t first, that the minute star ** B *'
has the same proper motion as the principal star ; the mean of
five sets of measures of A and B, made by different observers
between 1877 and 1891, is io9°8 3i".o8; second, that the
Herschel cooipanion, C, has a proper motion of its own,
differing from that of the principal star; third, that D, the com-
panion to C, shares its proper motion, the relative change being
due to some other cause. C and D, then, probably form a physi-
cal system, having no connection, other than optical, with A and
B, and the apparent distance between the two systems will con-
tinually increase. R. G. Aitken.
February 26, 1898.
A Remarkable Object.
JiWolsingham Observatory Circular^ No. 46.]
**A remarkable object, hitherto unrecorded, was discovered on
January i6th, and seen on three other nights. It is elliptical,
one degree long, major axis 336°, and rather resembles some
obscuring medium than a nebula, and is, I believe, unique.
•* Place: R. A. 4' 26"" o', Decl. -f 50° 44' (1855).
T. E. EsPiN.''
1898, February 16.
Request for Observations.
Mademoiselle VerA Stachevitet, Observatoire d' Ecole
Superieure des Femmes, He de Basil 10 Ligne d. 33, St. Peters-
burg, wishes to compute the definitive orbit of Comet 1896 I, and
would like any unpublished observations sent to her. C. D. P.
t Monthly Notices R. A. S., March, 1891.
84 Publications of the
A Daylight Meteor.
** Director of Lick Observatory.
**Dear Sir : I saw by the papers that a meteor had lately been
observed by one of your men, and thought it might be of interest
to you to say that last October, about an hour before sunset, I
observed a very large and brilliant meteor fall between this city
and a mountain to the north, not more than fifteen miles away.
It left behind a spiral-shaped cloud of smoke, which was visible
for about twenty minutes. Yours truly, Chas. Pixley."
Missoula, Mont., January 24, 1898.
Missing Books.
The following books and periodicals are missing from the
library of the Society, and no record of their whereabouts
appears upon the charging book. Any information concerning
them will be gratefully received by the Library Committee.
BOOKS.
No. 3. Proctor (R. A.): Other Worlds than Ours. i2mo.
9. Webb (T. W.): Celestial Objects for Common Tele-
scopes. 1 2mo.
10. Webb (T. W.): Celestial Objects for Common Tele-
scopes. i2mo.
17. Oliver (J. A. W., and others): Astronomy for
Amateurs. i2mo.
18. Oliver (J. A. W., and others): Astronomy for
Amateurs. i2mo.
46. Young (C. A.): The Sun. i2mo.
47. Young (C. A.): The Sun. i2mo.
49. Proctor (R. A.): Orbs Around Us. i2mo.
51. KiRKWOOD (D.): Meteoric Astronomy. i2mo.
57. Newcomb (S.): Popular Astronomy. i2mo.
252. Mueller (H.): Die Kepler^ schen Gesetze, 8vo.
253. Prestel (M. a. F.): Astronomisches Diagramm.
Svo.
260. Thornton (J.) Physiography. i2mo.
277. Brewster (D.): More Worlds than One. i2mo.
281. : Martyrs of Science. i2mo.
282. : Life of Sir Isaac Newton. i2mo.
301. Lynn (W. T.): Celestial Motions. i6mo.
302. Johnson (S. J.): Eclipses, Past and Future. i6mo.
Astronomical Society of the Pacific. 85
318. ScHELLEN (H.): Spectrum Analysis. 8vo.
322. Ledger (E.): The Sun, Its Planets, etc. i2mo.
330. Lewis (S. C): Historical Survey of the Astronomy
of the Ancients. 8vo.
489. Proctor (R. A.): Myths and Marvels of Astronomy.
i2mo.
PERIODICALS.
Tlie Observatory: No. 252 (April, 1897).
Monthly Notices Royal Astronomical Society: Vol. LVI, Nos.
2, 4> 5.
T7i€ Astrophysicat Journal: Vol. V, Nos. 2, 4, 6; Vol. 6, No. i.
The Library Committee.
Election of Professor James E. Keeler as Director
OF THE Lick Observatory.
At the regular meeting of the Board of Regents of the
University of California, held in San Francisco on Tuesday,
March 8, 1898, Professor James E. Keeler, Director of the
Allegheny Observatory, was chosen to fill the vacancy created
by the resignation of Professor E. S. Holden as Director of the
Lick Observatory.
At this date it is not known when Professor Keeler will
assume the duties of his new office. R. G. Aitken.
March 16, 1898.
Library Notice.
Attention is called to the report of the Library Committee
printed in this number in the minutes of the meeting of the
Board of Directors. The Committee is making every effort to
increase the value and usefulness of the library, both by adding
to the number of volumes and by making these more easily
accessible. It is especially desirable to increase the number of
books and periodicals of large popular interest Contributions
of this class from any source will be thankfully received.
Publication Committee.
Discovery of Comet b, 1898 (Perrine).
This comet was discovered in the morning of March 20th.
At o* 53" 56' G. M. T. its position was R. A. 21' i8» 36V89,
and Decl. +16^43' 23^.3. It was then very near the western
86 Publications of the
limits of the constellation Pegasus, a little south and west of the
iitar iota. Its daily motion is north i^ and east about the same
amount.
The head is composed of a nucleus, some lo" in diameter,
surrounded symmetrically by a nebulosity 2' in diameter. The
nucleus does not present a stellar appearance, but looks granular.
Extending away from the comet, in position -angle 281°, is a
moderately broad tail, which can be traced to a distance of i^.
It seems to broaden near the end, and there are indications of a
fainter nebulosity surrounding the main tail.
The head of the comet is about as bright as a seventh magni-
tude star, and can be seen with a very small telescope.
Mt. Hamilton. Cal., March 21, 1898. C. D. P.
Elements of Comet ^, 1898 (Perrine).
From Mr. Perrine' s observation of March 19th, at the time
of discovery, and my observations of March 21st and 22d, I
have computed the following elements of this comet : —
7"= March 19.1079, G. M. T.
0_,jf;;5;3 f Eclipdcand
•_ 2 =^^ '>=^ * Mean Equinox of 1898.0.
31' 16")
19 53 \
53 25 )
log q = 0.04252.
(O.-C.) AX' cos P^ = +5" ^/3' = +3"
W. J. Hussey.
Astronomical Telegrams (Translation),
Lick Observatory, March 20, 1898.
To Harvard College Observatory, 1
Students' Observatory. / ^ent 12'^ 35" P- m.
A bright comet was discovered by C. D. Perrine (on March
20th, at 4:30 A.M.). Its position, March 20th, o*" 53" 56' G. M. T.,
was, R. A. 21*^ i8'"36'.89; Decl. +16° 43' 23".3. Its daily
motions are +56' in R. A. and +61' in Decl. The physical
appearance of the comet is, nebulosity 2' diameter, seventh
magnitude, strong central condensation, tail i** long.
Lick Observatory, March 22, 1898.
To Harvard College Observatory: ) ^gent 10:15 a.m.)
To Students Observatory, Berkeley: )
Comet b, 1898, (Perrine) was observed by W. J. Hussey,
March 22.0532, G. M. T.; R. A. 21' 25"59".8, Decl. +18° 49' 17".
Astronomical Society of the Pacific. 87
Lick Observatory, March 23, 1898.
To Harvard CoUegeObsen^tory: ) (Sent 9:55 A. M.)
To Students Observatory, Berkeley: )
Comet b, 1898, (Perrine) was observed by C. D. Perrine,
March 22.9855, G. M. T.; R. A. 21*' 29- 28'.9, Decl. + 19° 4/ 24".
Lick Observatory, March 23, 1898.
To Harvard College Observatory: (Sent 9:30 p.m.)
The following elements and ephemeris of Comet b, 1898,
(Perrine) were computed by W. J. Hussey and C. D.
Perrine: —
T= 1898, March 18.67, G. M. T.
<u= 49° 2'
O = 264 7
i= 72 48
^= 1.1013.
[The ephemeris is omitted here.]
Erratum.
Volume X, page 35, line 3, for 1897 read 1898.
X
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Astronomical Society of the Pacific. 89
Minutes of the Special Meeiting of the Board of
Directors of the Astronomical Society of* the
Pacific, held in the Rooms of the Society, on
Saturday, November 27, 1897, at 2 p.m.
Mr. PiBRsoN presided. A quorum was present.
The purpose of the meeting being the First Award of the Bruce
Gold Medal; the letters received from the Directors of the six nomina-
ting Observatories were submitted by the Secretary. After a careful
consideration of the recommendations contained in these letters, the
selection of the Medalist was made by ballot, and the following certifi-
cate of bestowal was signed by all Directors present: —
San Francisco, November 27, 1897.
First Award of the Brucb Medal.
We. the undersigned Directors of the Astronomical Society of the
Pacific, hereby certify, that, in accordance with the Statutes for the
bestowal of the Bruce Medal, a special meeting of the Board of Direc-
tors was held this day, at 2 o'clock p.m., for the purpose of awarding
the medal for the year 1898; and that, the provisions of the Statutes
relating to its bestowal having been complied with, the medal was
awarded to —
SIMON NEWCOMB
for Distinguished Services to Astronomy, by the consenting votes ot
eight Directors.
Signed: Wm. M. Pibrson, Frederick H. Sbares,
Fremont Morsb, Rose O'Halloran, C. D. Perkins, F. R. Zibl,
E. S. Holdbn (by proxy), C. M. St. John (by proxy).
Adjourned.
On January i, 1898, the Secretary addressed a letter to Professor
Nbwcomb, notifying him of the action taken by the Directors. The
following letter of acceptance was received on January 17th: —
Washington, January ii, 1898.
Mr. F. R. Zibl, Secretary.
Dear Sir: I have the honor to acknowledge receipt of your com-
munication of the ist inst., apprising me that the Board of Directors of
the Astronomical Society of the Pacific had awarded me the first
Bruce Gold Medal, being that for the year 1898. It gratifies me
extremely to know that this should have been the result of so admirable
a method of selection as that prescribed in your statutes. I beg that you
will assure the Board of Directors of my very high appreciation of such
an honor from my own Country, and of the pleasure with which I
signify my acceptance.
Yours most respectfully,
Signed: Simon Nbwcomb.
90 Publications of the
Minutes of the Meeting of the Board of Directors,
• held in the Rooms of the Society,
March 26, 1898, at 7:30 p. m.
Miss 0*Halloran presided. A quorum was present. The minutes
of the last meeting were read and approved. The following members
were duly elected:—
List of Members Elected March 26, 1898.
Mr. W. W. ALLEN {^"ct^S^^ola' ^^""^
Mr. Manley F. Bendall | '^France."^^ '^'^''^'' Bordeaux
Mr. John Everding, Jr 48 Clay St., S. F., Gal.
Mr. J. H. Firehammer 1590 Pacific Ave., Alameda, CaL
Miss Adelaide M. Hobe 604 Capp St., S. F., Gal.
Mr. Harold K. Palmer Berkeley, Gal.
The Library Committee presented its report, as follows, and the
report was, on motion, adopted and filed:—
Report op the Committee on the Library, Submitted March a6, 1898.
To the Board of Directors of the Astronomical Society of the Pacific :
Gentlemen— We, the undersigned, Committee on the Society's Library, respectfully
report as follows:—
During the year the library has been reaccessioned, and the construction of a card
catalogue has been undertaken. The bound books have been classi6ed on the shaves
according to subject; the unbound books and pamphlets have been similarly classified
and arrans:ed in drawers specially provided for tne purpose. A large amount of hi nding
has been done, and considerable purchases of books have been made. Through binding
and purchase, together with gifts from corresponding institutions, 290 volumes have been
added to the shelves.
The library consists at present of about 910 bound volumes and several hundred
pamphlets. Exact numbers cannot be given until the work of cataloguing has been
finished.
The purchases have been made in pursuance of the recommendation contained in the
report of the Library Committee for the year 1890-91 [.Publications A. S. P., Vol. IlL
page 149), as follows: " Your committee . . . would recommend that hereafter the
revenue derived from the remainder of ihe Alexander Montgombry Fund should be
applied to the purchase of the more technical and recondite works on astronomy." While
acting in- accordance with this recommendation, the present Library Committee has,
nevertheless, felt that the library should also secure, as largely and as rapidly as possible,
the astronomical works of ^eater popular interest. Gifts of single books or of sets of
books of this class are especially desired.
During the past year special effort has been made to secure for the library valuable
books which are out of print, and which are rapidly becoming rare.
The following is an account of the expenclitures of the Alexander Montcoiierv
Library Fund for the year ending March 26, 1898:—
1897, Aug. 24. Pobular Astronomy | 1400
Hicks-Judd Co. for binding 105 volumes 94 ^
Kreutz— missing numbers Astron NachricKten . . x 90
94 volumes of Astronomiscfu Nachrichten 306 00
Cable re 94 vols. Astron. Nachrichten 7 24
Freight on 94 vols. Astron. Nachrichten 9 46
Sept X. 4 chests drawers for pamphlets 12 00
15. Freight on card catalogue from Chicago — 2 90
16. Card catalogue, etc. . 19 10
1S98, Jan. 7. Expressage on H. C O. Annals from Cambridge. . 5 10
Feb. 14. Hicks-Judd Co. for binding 38 volumes 32 80
Mar. 9. 3 volumes Astronomical foumai 7 50
Respectfully submitted, :^=
William J. Hussey,
Frederick H. Searbs,
Rose 0'Hall.oran,
Committee,
Astronomical Society of the Pacific. 91
Minutes of the (adjourned) Annual Meeting of the
astronobncal society of the pacific, held in the
Rooms of the Society, April 2, 1898, at 8 p. m.
The meeting was caUed to order by Mr. Pierson. A quorum was
present The minutes of the last meeting were approved.
The Secretary read the names of new members duly elected at the
Directors' meeting of March 26, 1898.
The following papers were presented:—
I. Address of the retiriuR President, by Hon. William Alvord.
a. Reports of Committees: on Nominations; on the Comet-Medal; on the Library; on
Auditing; and Annual Report of the Treasurer.
3. The Edinburgh Observatory, by Professor R. G. Aitkbn.
4. Earthquakes in California in 1897, by Mr. C. D. Pbrrinb.
S* A New Variable Star, by Mr. Torvald KOhl, oi Odder, Denmark.
6. Latitude Work with the Fauth Transit of the Lick Observatory, by Professor H. D.
Curtis.
7. Planetary Phenomena for May and June, 1898, by Professor M. McNeill.
8. Magnifying Ratios of Ewing Seismographs of Three Components, and of the Duplex-
Pendulum Seismographs, by Mr. C. D. Pbrrinb.
The Committee on Nominations reported a Ust of names proposed
for election as Directors, as follows: Messrs. R. G. Aitkbn, C. B. Hill,
Jambs E. Kbblbr, £. J. Molbra, C. D. Pbrrinb, Wm. M. Pibrson,
F. H. Sbarbs, C. M. St. John, O. von Gbldbrn, F. R. Zibl, and Miss
R. O'Halloran.
For Committee on Publication: Messrs. R. G. Aitkbn, F. H.
Sbarbs, O. von Gbldbrn.
Messrs. Cushing and Mosbs were appointed as tellers. The polls
were open from 8:15 to 9 p. m., and the persons above named were duly
elected to serve for the ensuing year.
Report of the Committee on the Comet-Medal,
Submitted March 26, 1898.
The present report relates to the calendar year 1897. The comets
of 1897 are:—
Comet a (d' Arrest's periodic comet), rediscovered June 28, by
C. D. Pbrrinb, Assistant Astronomer in the Lick Observatory.
Comet b (unexpected comet), discovered October 16, by C. D.
Pbrrinb, Assistant Astronomer in the Lick Observatory.
The Comet-Medal of the Society has been awarded to Mr. Pbrrinb
for the discovery of Comet b. This is the fifth award (made for similar
previous discoveries) to the same observer.
Respectfully submitted.
E. S. Holdbn,
J. M. Schaeberlb,
W. W. Campbbll.
92 Publications of the
The Treasurer submitted his Annual Report, as follows:—
Annual Statbmbnt op thb Receipts and Expenditures op the
Astronomical Society op the Pacipic for the
Fiscal Year ending March 26, 1898.
general fund.
Receipti,
Cash Balance, March 28, Z897 1 489 >9
Received from duea. I1471 67
** " sale of publications 6935
*• •• "stationery 150
*• " " " furniture, etc xa 00
** •' advertisements 63 25
** " Security Savings Bank (interest) 4 37
•' ** Life Membership Fund (interest) 73 49
I169563
Less transfer to Life Membership Fund 4So 00 I1245 63
117349a
Expenditurts.
For publications | 723 10
" general expenses 62404
I134614
Cash Balance March 26, 1898 38878
>I734 9»
LIFE membership FUND.
Cash Balance March 28, 1897 I1750 61
Received from General Fund 450 00
" '« interest 7349
I2274 10
Less interest transferred to (general Fund 73 49
Cash Balance March 26, 1898 $1200 61
donohoe comet-medal fund.
Cash Balance March 28, 1897 >.. I 676 04
Interest 26 21
I 70a as
Less transfer to Montgomery Library Fund (see Vol. IX, page 1x3) 70 89
Cash Balance March 26, X898. 163136
ALEXANDER MONTGOMERY LIBRARY FUND.
Cash Balance March 28, X897 |i93a 68
Interest 71 X2
Transfer from Comet-Medal Fund (see Vol. IX, page 1x3) 70 89
1207469
Less expended for books, binding, etc 5x260
Cash Balance March 26, X898 |i56« 06
BRUCE MEDAL FUND.
Sept. 20, 1897. Cash received from Miss C. W. Bruce |a750 00
Interest x8 30
Cash Balance March 26, 1898 $2768 3
I 388 78
I2200 6z
I 631 36
I1562 09
Astronomical Society of the Pacific. 93
FUNDS.
Balances od Deposit as follows:
Geoerml Fund:
with Donohoe-Kelly Banking Co I 33o 45
*• Security Savings Bank 58 33
Life Membership Fund:
with San Francisco Savings Union. . . Iiooo 61
*' German Savings and Loan Society 600 00
" Hibemia Savings and Loan Society 600 00
Dooohoe Cometh Medal Fund:
with San Francisco Savings Union I 205 34
•• German Savings and Loan Society ai3 36
** Hibemia Savings and Loan Society 21266
Alexander Montgomery Library Fund:
with San Francisco Savings Union '. IS28 55
" German Savings and Loan Society 421 36
" Hibemia Savings and Loan Society 612 18
Brace Medal Fund:
with San Francisco Savings Union I1510 06
* •• Security Savings Bank 628 99
*' German Savings and Loan Society 629 25
I2768 30
$7551 14
San FRANasco, March 26, 1898. F. R. ZIEL, Treasurer.
The committee appointed to audit the Treasurer's accounts reported
as follows, and the report was, on motion, accepted and adopted: —
TV the President and Members of the Astronomical Society of the. Pacific :
Gbntlbmbn— Tour committee appointed to audit the accounts of the Treasurer for
the fiscal year ending March 26, 1898, have made a careful examination, and find same to
be correct Yours respectfully,
Jos. GASSMANN,
F. H. MCCONNELL.
In the absence of Mr. Alvord, the address of the President was
read by Mr. Gushing.
The following resolution was, on motion, adopted:—
Resolved, That all the acts appearing in the minutes of the meetings of the Board
of Directors of this Society, as having been done by said Board during the past fiscal
year, are here now, by this Society, approved and confirmed.
Adjourned.
94 Publications of the
Minutes of the Meeting of the Board of Directors,
held in the rooms of the society,
April 2, 1898, at 9 p. m.
The new Board of Directors was called to order by Miss O'Hal-
LORAN. A quorum was present The minutes of the last meeting were
approved.
The business in hand being the election of officers and committees
for the ensuing year, the following officers and conmiittees, having
received a majority of the votes cast, were duly elected:—
President: Mr. R. G. Aitken.
First Vice-President: Mr. C. B. Hill.
Second Vice-President: Miss R. 0*Halloran.
Third Vice-President: Mr. F. H. Shares.
Secretaries: Messrs. C. D. Perrine and F. R. Zibl.
Treasurer: Mr. F. R. Ziel.
Committee on the Comet-Medal: Messrs. Schaeberlb {ex-ajficio)^
PlERSON, BuRCKHALTER.
Library Committee: Messrs. F. H. Seares, Geo. C. Edwards,
Miss R. O'Halloran.
Mr. Seares was appointed Librarian.
The Chairman was authorized to appoint the members of the
Finance Committee, and accordingly made the following selections:
Finance Committee: Messrs. Pierson, von Geldbrn, Hill.
The Committee on PublicaMon is composed of: —
Messrs. Aitken, Seares, and von Geldern.
Adjourned.
Astronomical Society of the Pacific, 95
OFFICERS OF THE SOCIETY.
Mr. R. G. AiTKKN Prtsidtnt
Mr. C. B. Hill First Vict-Prtsident
Miss R. D'Halloman Stcond Vict-Presidtnt
Mr. F. H. Sbarrs Third Vice-President
5JJ:R-g:lr'""| '"^'"■,.
Mr. F. R. ZiEL Tretuurer
B0ard o/ Direct^rs^VLtxsn, Aitkbn, Hill, Kkblkr, Molbra, Miss O'Halloran, Messrs.
Pkrrinb, Pibrson, Sbarbs, St. John, von Gbldbrn, Zibl.
Finance Committee — Messrs. PibrsON, von Gbldbrn, Hill.
Committee on Publication— yi^9ax%* Aitkbn, Skarbs, von Gbldbrn.
L^rmry Committee— lAesax%. Sbarbs, Gbo. C. Edwards, Miss O'Halloran.
Committee on the Cotnet- Medal— lAtssn, Schabbbrlb (ex-ojicio)* Pibrson, Burckhaltbr.
OFFICERS OF THE CHICAGO SECTION.
Executive Committee— lAr. Ruthvbn W. Pikb.
OFFICERS OF THE MEXICAN SECTION.
Executive Committee— Ut. Francisco Rooricubz Rbv.
NOTICE.
The attention of new members is called to Article VIII of the By-Laws, which provides that
the annual subscription, paid on election, covers the calendar year onlv. Subsequent annual
pajrmenu are due on January ist of each succeeding calendar year. I'his rule is necessary in
order to make our book-keeping as simple as possible. Dues sent by mail should be directed to
Astronomical Society of the Pacific 819 Market Street, San Francisco.
It is intended that each member of the Society shall receive a copy of each one of the Pit6-
lications for the year in which he was elected to membership and for all subsequent years. If
there have been (unfortunately) any omissions in this matter, it is requested that the Secretaries
he at once notified, in order that the missing numbers may be supplied. Members are requested
to preserve the copies of the Publications of the Society as sent to them. Once each year a title-
page and contents of the preceding numbers will also be sent to the members, who can then bind
the numbers together into a volume. Complete volumes for past years will also be supplied, to
ntembers only, so far as the stock in hand is sufficient, on the payment of two dollars per volume
to either of the Secretaries. Any non-resident member within the United States can obtain
books from the Society's library by sending his library card with ten cents in stamps to the
Secretary A. S. P., 819 Market Street, San Francisco, who will return the book and the card.
The Committee on Publication desires to say that the order in which papers are printed in
the Publications is decided simply by convenience. In a general way, those papers are printed
first which are earliest accepted for publication. It is not possible to send proof sheets of papers
to be printed to authors whose residence is not within the United States. The responsibility for
the views expressed in the papers printed rests with the writers, and is not assumed by the
Society itself.
The titles of papers for reading should be communicated to either of the Secretaries as early
as possible, as well as any changes in addresses. The Secretary in San Francisco will send to
any member of the Society suitable stationery, stamped with the seal of the Society, at cost price,
as follows: a block of letter paper, 40 cents; of note paper, 25 cents; a package of envelopes, 25
cents. These prices include postage, and should be remitted by money-order or in U. S. postage
stamps. The sendings are at the risk of the member.
Those members who propose to attend the meetings at Mount Hamilton during the summer
should communicate with "The Secretary Astronomical Society of the Pacific " at the rooms of
the Society, 810 Market Street, San Francisco, in order that arrangements may be made for
transportation, lodging, etc
PUBLICATIONS ISSUED BIMONTHLY.
( February t Aprils June^ August t October, December.)
THE SPECTROSCOPE ATTACHED TO THE is-INCH REFRACTOR OE THE
ROYAL OBSERVATORY. EDINBURGH.
THE KEY/ Y',RK
Fi:BLICL:3n.\RY
TiU; N
PUBLIC LIBRARY
A6TCR. LENOX AND
, TKt KEV/ YORKl
PUBLIC L:3'^/\RY I
THE NEW YORK
PUBLIC LIBRARY
A6TCR, LFNOX AND
TlLOEN FOUNDATIONS.
THE SOLAR CORONA OF JANUARY 22, 1898.
(Photographed with the Floyd telescope, by W. W. Campbell.)
FUBLICLIB^A-V
FUBLICAriONS I uloen foundations.
or T H B
Astronomical Society of the Pacific.
Vol. X. San Francisco, California, June i, 1898. No. 62.
ON THE CAUSES OF THE SUN'S EQUATORIAL
ACCELERATION AND THE SUN-SPOT PERIOD.
By E. J. VVlLCZYNSKI.
In the beginning of every science isolated facts present them-
selves, which apparently have no connection with each other.
As the science is gradually perfected, relations are found between
the different phenomena, the subject becomes more complex, and
covers a wider stretch than it did at first; but at the same time it
becomes easier to understand because it is found that all of the
phenomena, which have been observed, are but the consequences
of certain fundamental laws. In solar physics two laws of funda-
mental importance have been found, the law of the equatorial
acceleration and that of the periodicity of sun-spots. Their
great significance lies in this, that they give numerical relations
between measurable quantities, and that their consequences can,
therefore, be deduced by mathematical reasoning.
The researches which I have made upon this subject have
appeared in my inaugural dissertation on * * Hydrodynamische
Untersuchungen mit Anwendungen auf die Theorie der Sonnen-
rotation," Berlin, 1897, and in some papers in the Astrophysical
Journal: A brief account has also appeared in the Astronomical
Journal^ Vol. XVIII, No. 416. In this paper I will try to pre-
sent the principal points in popular language.
We assume the Sun to be a fluid body, the general term fluid
comprehending both gaseous and incompressible fluids as special
cases. Its present condition and the present motion of its parts
are, then, but the consequences of the condition of the nebula from
which it has been formed, and of the motion of the parts of this
9^ Publications of the
nebula. This is exactly the same as in the case of planetary orbits.
The form of the planet's orbit and its position in space was deter-
mined by the position and the motion of the planet at the time of its
formation. Such an orbit must be a conic section, if we neglect
the perturbations, and it may possibly be a circle. And just in
the same way as a circular orbit is an exception in the case of
planetary orbits, only one occurring among an infinite number,
so also is it infinitely improbable that a gaseous body starting to
rotate should rotate in the same way as a solid mass. It may do
so, but in general it will not
But obviously we must take into account the influence of the
internal fluid friction, which, of course, tends to make the body-
rotate as if it were solid. But the mathematical theory shows
this influence to be very small, so small that it will not change
the daily arc described by a point upon the Sun by 2' in 27,500,000
years.
This result is obtained in the course of investigating the follow-
ing problem. All particles of a viscous fluid describe circles in
parallel planes around an axis perpendicular to these planes.
The conditions for the motion and figure of such a body are
investigated. The angular velocity of rotation is supposed to be
diflerent in different parts of the fluid. It is found that an
important theorem holds, which we proceed to explain.
The density of the body, as well as the temperature may vary
from point to point. All points in which the density has the
same value constitute, in general, a surface which is called a
surface of constant density. Similarly we can speak of surfaces
of constant temperature. The theorem which we have in view is
this:—
In a rotating viscous fluids the angular velocity of rotation is
the same fur all points whose distance from the axis of rotation is
the same, if the surfaces of constant density and of constant tempera-
ture coincide. If we conceive the axis of rotation to be surrounded
by a family of co-axial cylinders, the surface of each cylinder
rotates as if it were rigid.
This theorem is shown to be very probably true for the case
of the Sun, and the surfaces of constant density are calculated
approximately. By applying the theorem to the comparison ot
the different laws of rotation which have been empirically found
for the sun-spots, for the faculae and for the so-called reversing-
layer, the difference in level of these different solar strata can be
Astronomical Society of the Pacific. 99
ascertained. The discussion of these numbers lea^ds to the result
that the solar atmosphere, i. e. the region above the ** photo-
sphere" is much more extensive than has usually been believed.
The contradictions, which seem to rise herefrom at first sight,
can ^be easily cleared up if the power of refraction, which this
atmosphere must have, is taken into account. One other impor-
tant conclusion is that the sun-spots must be higher up in the
solar atmosphere than the photosphere, a view which, while
opposed to the classical idea of Wilson, is nevertheless constantly
gaining more adherents.
If the motion of the solar particles is not stricdy uniform and
circular, and it is easy to see that in general it will not be so, the
deviations from the uniform circular motion cause corresponding
changes in the temperature, pressure and density, as the equa-
tions show. Now it is quite easy to show that these deviations,
supposed to be small in comparison with the principal motion,
are of an oscillatory character, tending at the same time towards
zero. That is, they will be periodic functions of the time but
become constantly smaller, in the same way as a pendulum
swinging in air oscillates backward and forward, but finally comes
to a stop. But in our case this dampening effect is only very
slight, and may not be noticed for thousands of years. To the
periodic variations of the motion will then correspond periodic
changes in temperature, etc., and it is extremely plausible that
hereto will correspond periodic variations of the Sun's activity.
This line of thought gives a very reasonable explanation of the
sun-spot period, which is also supported by some numerical
work which is meant to show that the causes invoked are suffi-
cient to explain the observed phenomena.
If we remember that the theory sketched out here is based on
no arbitrary assumptions, that it reaches its conclusions by rigid
mathematical reasoning, and that it succeeds in uniting the
observations of solar physicists, which have been the source of so
many wild hypotheses, into one consistent whole, it certainly
seems to be a step in the right direction. And it seems to me
that we are justified in saying that the rotation-law is the instru-
ment with which to fathom the solar mysteries. It is the funda-
mental law to which all others, even that of the sun-spot period,
are but supplementary.
Nautical Almanac Office,
Washington, D. C, May 6, 1898.
loo Publications of the
THE NEW ATLAS OF VARIABLE STARS.*
By the Rev. Father J. G. Hagen, S. J.
Dear Sir:—\n compliance with your kind invitation to send to
you a description of the forthcoming Atlas of Variable Stars, I offer
the following remarks on the plan of the work, on the observations,
and on the construction of the charts: —
L The Atlas is planned to contain all variable stars from the
north pole to — 25° Declination. For the present are excluded the
the new stars, called Nova, and the recently discovered stars,
whose variability and character are not yet sufficiendy established.
The Atlas is divided into five Series, the first three of which
comprise those Variables that fall below the loth magnitude at their
minimum phase, while the fourth series contains those that can be
followed with a three-inch telescope throughout their entire
variation, and the fifth gives all the naked-eye Variables. The first
three Series cover respectively the zones from —25° to the equator,
from the equator to -{-25° and from +25° to the pole. Arrange-
ments have been made with the publisher by which each of the
five series can be procured separately, so that observers will be
enabled to select for themselves that Series which best suits their
equipment and their location with regard to the equator. Begin-
ners especially will find this division of the whole Atlas advan-
tageous, as they will have the whole program of their work marked
out, without the danger of omitting interesting variables or of
wasting time upon unsuitable objects.
The following description is confined to the first three Series,
as the fourth and fifth will require special explanations.
II. The observatiojis for the first three Series were the most
laborious, and differ in many respects from those required for the
fourth and fifth Series, on account of the many faint stars that
had to be determined with regard to position and magnitude.
The field chosen for these three Series is one degree square,
in whose center is the variable. In this square all the BD stars
• This letter by Father Hagen is in answer to one sent to him requesting informatioii
concemins: his new Atlas of Variable Stars. The value of the work is evident, and its
appearance should give new impetus to the study of variables. It is perhaps not out of
place to add that the systematic observation of variable stars is one of the most profitable
lines of work into which the amateur can enter. It is a field in which any member of the
Astronomical Society of the Pacific can do work, the results of which will be of real benefit
to the Science of Astronomy. Editor.
Astronomical Society of the Pcuific. loi
were plotted, and then identified in the sky by means of a
five-inch equatorial. Not only were the errors noted, but all the
stars of a chart were connected with each other by sequences of
brightness, according to Argelander's method, beginning with
the brightest star. This operation was repeated after an interval
of many months, generally a year.
After the first three Series were finished in this way, the
charts were taken to the 12-inch equatorial for the insertion of
the fainter stars. For these fainter stars a smaller square was
marked around the variable, viz. half a degree square, covering
only one-fourth of the area of the whole chart. The positions of
all the stars within this smaller square, visible in our 12-inch
refractor, and of all the BD stars of the whole chart, were then
determined by means of a semi-circular glass scale, measuring
30', and divided into ten parts. Thus 3' could be read directly,
and o'.3 by estimation. The lines were cut in the glass by
means of a dividing engine and then painted black by hand rather
coarsely, to make them visible in the light of the stars without
field illumination. Hence the glass scale was similar to the one
used for the BD, but the method of observation was different.
The declinations were determined separately from the Right
Ascensions while the telescope was following the stars by means
of the driving clock. For the R. A. the telescope remained
clamped, but the clock was stopped, and the approach of the stars
to the vertical diameter of the glass scale was recorded on the
chronograph. This record was made three times, not so much
to reach greater accuracy as to make sure that the combinations of
the Decl. and R. A. were placed beyond doubt. Since the glass
scale covers only one-half of a chart, the northern and southern
parts of the charts had to be observed separately. In the cata-
logue the Decl. and R. A. are given differentially from the Variable
as zero point. The inclination of the glass reticle to the hour
circle was determined from several stars whose position was
known either from catalogues or from kind communications of
astronomers now engaged in making the southern zones of the
A. G. , or finally from observations with our own Ertel transit
instrument. All these observations and computations for correct-
ing the inclination of the reticle were carried out by Rev. Father
J. T. Hedrick, S. J.
The chronograph sheet was read off and the new stars plotted
on the chart, in different ink, on the morning after the observa-
I02 Publications of the
tion, in order to compare the chart with the sky, and to estimate
the brightness of the stars on the first succeeding clear night.
All the stars, including the BD stars, were then connected by
sequences of brightness, from the brightest to the faintest, and
these estimates were repeated about a month later. Hence, all
the fainter stars were estimated in brightness twice, besides
occasional revisions, and the BD stars four times. Each chart
was therefore compared with the sky at least ^v^ times.
For the construction of charts it was necessary to transform the
sequences of steps into a series of magnitude. For this purpose
the steps observed in the 5 -inch telescope had to be reduced to
those observed in the 12-inch refractor, by a multiplying factor,
which changed from one chart to another, and then they were
combined into a mean value. The value of one step, expressed
in magnitude, had to be found so as to make the computed mag-
nitudes agree as nearly as possible with any of the adopted scales
(in this case the BD), at least between the limits 7" and lo".
How the step value was computed, and from what starting point it
was applied, is of little importance. The test of the method will
be the agreement between the two series of magnitudes. This
same step value was then applied to the sequences of the fainter
stars, without regard to the different limits of magnitude which
would thus be reached on different charts. The lowest limit is
about I3".5, which is in good accord with the limit expected from
a comparison of our charts with those of Charcornac, Peters,
and Palisa. That this lowest limit was not reached on all charts is
partly owing to the well-known fact that estimates of steps do not
run uniformly from the brighter to the fainter stars, and hence
require a variable step value for their reduction to a uniform
photometric scale, and partly also owing to the fact that tele-
scopes have no fixed limit of visibility for all parts of the sky
and all times of the year. Hence, the magnitudes assigned to
the fainter stars of our charts are not to be considered as an
extension of the BD scale below the loth magnitude, but only
as serving the immediate purpose of engraving the charts. New
magnitudes can be deduced from the steps as soon as a photometric
scale is established for stars below the loth magnitude. All the
computations of the magnitudes were made by Mr. M. EscH,
S. J., assistant of this observatory. It may be well to state that
the observations at the telescope of positions and brightness were
all made by myself.
Astronomical Society of the Pacific. 103
III. The charts of the first three Series measure, as has been
said before, one degree in each direction, but the field that con-
tains the faint stars below the loth magnitude measures only one-
half degree in each co-ordinate. The variable star is placed in
the middle of the chart, and designated by a circle and a dot in
the center, which correspond respectively to its maximum and
minimum brightness. The identification of the variable was con-
sidered the most important point of the Atlas, and no chart is
sent to the engraver before the variation of the star in the center
has been established by actual observations. There is good
ground for the hope that all errors of this kind have been avoided.
The projection of the net is not optical, but artificial, the meridian
lines being all parallel and the Horizontal lines at equal distances
from each other. The color of the net is red, and no letters are
printed on the charts. Thus, in red light, which is found very
agreeable to the eye when frequent changes from light to darkness
are to be made, nothing appears on the chart except the black
disks of the stars. This gives them the nearest resemblance to
the sky, and facilitates recognizing the configuration.
The inscription of each chart is supposed to furnish everything
necessary for the night work, while the catalogue gives other
data useful for the computations.
The AtloLs is published in Berlin, by Mr. Felix L. Dames
(Voss Strasse, 32). It will be agreeable to your readers to learn
that Miss Catherine Wolfe Bruce, so well known for her
many contributions to astronomical science, has placed in the
hands of Professor Edward C. Pickering a security of nearly
two thousand dollars, which, while not covering the expense of
engraving and printing of the whole Atlas, has encouraged the
publisher to run the risk of this publication.
J. G. Hagen, S. J.
Georgetown College Observatory, March 19, 1898.
OBSERVATIONS OF o Ceti {Mird). 1897-98.
By Rose O'Halloran.
The variable star o Ceti attained a greater magnitude last
November than during any of the recent years since the maxi-
ma commenced to occur in months when the constellation was
not obscured by sunlight. Observations were taken of its rela-
I04 Publications of the
tive brightness on eighty-six nights between September 29, 1897,
and February 28, 1898; but to avoid repetition, only nights of
marked change are mentioned.
September 29. Equal to adjacent star of eighth magnitude.
October 17. Equal to 66 Cetu
October 23. Nearly e(Jual to i Piscium,
October 26. Brighter than ^ Piscium,
November 3. Brighter than h Ceii,
November 10. Moonlight. For the first time since the maxima
have occurred out of sunlight the variable is as bright as y
CeH.
November 21. One- fourth of a magnitude brighter than y when
near meridian on a dark sky.
December i. One- fourth brighter than y. Moonlight. Clouds,
December 12. Equal to y.
December 14. Not fully as bright as y in a clear dark sky.
December 16. About one-fourth dimmer than y.
December 21. Midway between y and 8.
December 31. Equal to 8.
January 3. Not fully as bright as 8.
January 7. Even in moonlight not as bright as 8, which being a
white star, pales in moonlight.
January 9. Same as f Piscium.
January 13. About one-third magnitude fainter than i Piscium.
January 19. Brighter than 66 and 70 CeH^ and equal to 75 CeH,
January 24. Less than 75 in luster.
January 28. Equal to 70 Ceti,
February 4. In a hazy atmosphere seems brighter than 70.
February 12. The same as 71 Ceti,
February 19. Not as bright as 71.
February 28. Half a magnitude fainter than 71 CeH, Mira
was less than 7 magnitude on this date, when observations
were discontinued.
San Francisco, May, 1898.
HONOR CONFERRED ON PROFESSOR SCHAEBERLE.
On commencement day, May 18, 1898, the University of
California conferred the honorary degree of LL. D. upon Pro-
fessor J. M. SCHAEBERLE.
..i-x---''^'<
Astronomical Society of the Pacific. I los^^^y;, i-* ijcv?
THE RED STARS V HYDROS AND 277 OF BIRMING-
HAM'S CATALOGUE.
Bv Rose O'Halloran.
Two crimson stars, now visible in the evening sky, are espe-
cially worthy of the notice of telescopic observers. Unlike hun-
dreds of stars classed as red, which, in a steady atmosphere, have
merely a pinkish-yellow hue, these orbs preserve their claim to
redness under all conditions of visibility. The brighter of the
two, V Hydra, in R. A. 10** 46" 17' Decl. + 20° 40', may be
found (even with an opera-glass) west of a and )8 Crateris, with
which it forms a triangle. Since the beginning of April, it has
maintained a deep crimson color, though described as pale crim-
son, copper-red, and intensely red, by reliable observers in the
past At present it is of the seventh magnitude, and it is known to
vary from the sixth to the ninth, though the period seems to be
uncertain or irregular, being about 575 days, according to Gould,
but 653 days if the recent data of the Companion to the Observatory
be correct. The last maximum having been predicted for Octo-
ber 25, 1896, in this ephemeris, the next may occur in the
middle of August, when V Hydra sets in sunlight, but its alti-
tude will be sufficiently high for observation for some weeks yet.
Spectroscopists describe the spectrum of this star as being
strongly lined in the red and green, and class it as of the fourth
type.
Another orb, unusually free from yellow light, is numbered
277, in Birmingham's catalogue of red stars. Being in R. A.
12** 19"* 37* Decl. + 1° 22' it may be found about 2° northeast of
17 Virginis. Fitly classed as crimson, it is recognized as a vari-
able, with a range of from six and a half to eight and a half
magnitude, though its period seems to be unknown. In numer-
ous observations during the spring months of the last five years,
I have failed to detect any variation greater than from about
seven and a half to eight magnitude. It is considered that its
spectrum is probably of the fourth type, and as it terminates in
the green, this interesting orb may be surrounded by dense
vapors that obstruct all radiation of violet light.
San Francisco, May 20, 1898.
K>6 Publications of the
A NEW ASTRONOMY FOR BEGINNERS. BY DAVID
P. TODD, M.A., PH.D., PROFESSOR OF ASTRO-
NOMY AND DIRECTOR OF THE OBSERVATORY,
AMHERST COLLEGE. AMERICAN BOOK CO.,
NEW YORK. I2MO. 480 pp. $1.30.
As indicated in the title, this book is intended for those
having no previous acquaintance with astronomy. It is written
in an easy, descriptive style, and without presupposing mathe-
matical knowledge beyond the most elementary notions of
geometry. By far the greater part of the work is devoted to a
description of the fundamental principles of the science; next in
order comes the exposition of well ascertained facts, while mat-
ters that are as yet mere theories rightly receive but little atten-
tion. The portions of the book devoted to the methods and
results of astrophysical research are very limited, amounting to
less than five per cent of the whole, or much less than would be
expected in view of the prominence which has attached to this
department of the subject.
The book contains nearly 350 illustrations, most of them very
good. They may be roughly grouped as follows: Six colored
plates, some sixty astronomical drawings and celestial photo-
graphs, some twenty illustrations of instruments and observa-
tories, and many diagrams. These diagrams constitute a charac-
teristic feature of the book. In most cases, words, phrases or
sentences are printed along the lines forming them, so as to make
their meaning clear without further explanation, though such
explanation is also given in the text. Another characteristic
feature is the detailed directions for the construction and use of
simple apparatus to- enable the student to derive from his own
observations, in a rough way, to be sure, but correct in principle,
approximate values of some of the more easily obtainable astro-
nomical constants.
While the book, as a whole, is a good one, and contains a large
amount of well-selected and accurate information concerning
astronomical matters, there are, as may be expected in first edi-
tions, some blemishes that appear in the course of a critical
examination. One of these is an occasional incompleteness of
description, marring somewhat the effectiveness of the exposi-
tion. This, in general, is not serious, and in part seems to result
from the plan of the work, in that elementary explanations are
Astronomical Society of the Pacific, 107
often first given, to be followed later by more complete ones.
Such, however, is not always the case. For example, the
account of Talcott's method for finding the latitude (p. 85) care-
fully omits the fundamental principle of the method. We also
notice the occasional inclusion of matter wholly irrelevant to the
subject of the paragraph in which it is given. This, of course,
is of little consequence, and merely indicates imperfection in the
order of arrangement. Some of the statements made in relation
to the surfaces of the planets, particularly some of those giving
interpretations in explanation of the phenomena observed on
Mars, are not likely to pass unchallenged. The last sentence on
page 121, viz., * 'About the 20th March, at mean noon, when the
fictitious sun is crossing the equator, etc.,*' reads strangely, in
view of the fact that this ** fictitious sun*' (p. iii) travels in the
equator. Chapter II, which is probably the weakest in the book,
contains some loose description, some poor diagrams and some
erroneous defiriltions. The diagrams on pp. 35 and 37 bid defi-
ance to the laws of projective geometry, and it is difficult to
imagine how they can be otherwise than confusing to the student
On page 37, the ecliptic is defined in such a way as to be a fixed
circle in reference to the horizon, and on the next page the
equinoxes in such a way as to be fixed points in the meridian.
The logical consequence of these definitions would be that the
solstices are fixed points in the horizon, coincident with the east
and west points. The definitions referred to are as follows :
** Imagine the equator system pivoted at the two opposite points
where equator and meridian cross. Then carry the north pole
towards the west 23)^°. The equator will then have assumed
a position inclined by an angle of 23^^° to its former position.
It will, in short, have become the ecliptic. . . . Upper of
the two pivotal points upon which the equator turned about
meridian is called the Vernal Equinox^ or First of Aries ; its
opposite point, 180° away, the Autumnal Equinox V These
definitions, as they stand, are wholly inadmissible. They lack
completeness and accuracy of statement, and do much to accen-
tuate the looseness of ^pression prevalent in the chapter contain-
ing them. W. J. HussEY.
May 30, 1898.
io8 Publications of the
PLANETARY PHENOMENA FOR JULY AND AUGUST.
1898.
Bv Professor Malcolm McNeill.
July.
Eclipses, There will be two eclipses during the month, but
neither of them will be visible in the United States. The first, on
July 3d, is a partial eclipse of the Moon, not quite total. It will
be visible over nearly all of the eastern hemisphere. The second
is an annular eclipse of the Sun on July i8th. The path of the
annulus is entirely in the South Pacific ocean. It will be seen
as a partial eclipse in the southern part of South America.
The Earth is in aphelion on the morning of July 2d.
Mercury is an evening star, having passed superior conjunc-
tion on the morning of June 30th, and during the latter half of
the month it sets a little more than an hour after sunset; so it
may be seen under good conditions of weather. It makes a very
close approach to the first magnitude star a Leonis (^Regulus) on
the morning of July 27 th during daylight in the United States,
but the planet and star will not be far apart on the evenings of July
26th and 27th.
Venus is an evening star setting about two hours after the
Sun. It moves 33° east and 13° south during the month through
the constellation Leo^ passing i]4^ north of Regulus on July 13th.
Its apparent distance east of the Sun increases 3°, but on account
of its great southern motion the interval between sunset and the
setting of the planet diminishes about a quarter of an hour.
Mars rises earlier than before, only a little after midnight
toward the close of the month. It moves 21° east and 5° north
in the constellation Taurus, and on July 31st is about 5° north of
the first magnitude red star Aldebaran, a Tauri, It distance from
the Earth on July 15th is about 160,000,000 miles, and it will be
nearly twice as bright as it was during January.
Jupiter is still conspicuous in the southwestern sky in the even-
ing. It moves 3*^ east and south in the western part of the con-
stellation Virgo,
Saturn is in good position to be seen until after midnight. It
moves about 1° westward, and is about 7° north and a little west
of the first magnitude red star Antares, a Scorpii. The outer
Astronomical Society of the Pacific. 109
minor axis of the rings is just about the same as the diameter of
the planet.
Uranus is in the same neighborhood as Saturn, about half an
hour ahead. It moves about 1° westward in the constellation
Scorpio. It may be found by its proximity to the third magni-
tude star )8 Scorpiu On July ist it is about 2° west of the star.
Neptune is a morning star in the eastern part of Taurus,
August.
Mercury is an evening star and comes to greatest east elonga-
tion on August 9th. It remains far enough from the Sun to be
be seen under good conditions of weather through the first half
of the month, but during the latter half it rapidly approaches the
Sun, and it will reach inferior conjunction on September 5th.
Venus is still an evening star. The interval between its set-
ting and sunset diminishes about 10" during the month, although
it does not reach its greatest eastern distance from the Sun until
nearly the close of September. It moves 30*^ east and 15° south
during the month from the constellation Leo into Virgo, and on
August 30th passes about 1° north of the first magnitude star
Spica, a Virginis.
Mars rises before midnight at the end of August. It moves
about 21° eastward during the month in the constellation Taurus,
Its distance from the Earth diminishes 20,000,000 miles during
the month and at the end is less than 140,000,000. Its brightness
will perceptibly increase.
Jupiter is rapidly approaching conjunction with the Sun, and
at the end of the month can be seen for only a short time after
sunset. It moves about 5° east and 2° south in the western part
of Virgo,
Satur7i is still in fair position for observation, not setting until
late in the evening. It is in quadrature with the Sun on August
29th. It is nearly stationary in the constellation Scorpi but after
August 9th moves a fraction of a degree eastward.
Uranus is also nearly stationary in the same constellation,
about 2° west of the third magnitude star /3 Scorpii,
Neptune rises before midnight at the end of the month.
no Publications of the
Phases of the Moon, P, S. T.
Full
Moon,
July 3,
H. M.
I 12 P. M.
Last
Quarter,
July 10,
8 43 A. M.
New
Moon,
July 18,
II 47 A. M.
First
Quarter,
July 26,
5 40 A. M.
Full
Moon,
Aug. I,
8 29 P. M.
Last
Quarter,
Aug. 8,
10 13 P. M.
New
Moon,
Aug. 17,
2 34 A. M.
First
Quarter,
Aug. 24,
12 32 P. M.
Full
Moon,
Aug. 31,
4 51 A. M.
The Sun.
R. A.
Declination.
Rises.
Transits.
Sets.
1898.
H. M.
'
H. M.
H. M.
H.
H.
July I.
6 42
+ 23
6
4 41 A. w
[. 12 4 P.M.
7
27 P.M.
II.
7 23
+ 22
5
4 46
12 5
7
24
21.
8 3
+ 20
26
4 53 .
12 6
7
19
Aug. I.
8 47
+ 17
58
5 3
12 6
7
9
II.
9 25
+ 15
12
5 13
12 5
6
57
21.
10 2
+ 12
2
5 22
12 3
6
44
31.
10 39
+ 8
33
5 31
12 OM.
6
29
Mercury.
July I.
6 49
+ 24
24
4 40 A. M.
12 10 P.M.
7 40 P.M.
II.
8 17
+ 21
35
5 43
I
8
17
21.
9 29
+ 16
8
36
I 32
8
28
Au^. I.
10 28
+ 9
16
7 16
I 48
8
20
II.
II 5
+ 3
35
7 33
I 45
7 57
21.
II 22
—
3
7 22
I 22
7
22
31.
II 9
+
41
6 28
Venus.
12 30
6
32
July I.
9 6
+ 18
30
7 23 A.M.
2 28 P.M.
9 33 PM-
II.
9 53
+ »4
38
7 45
2 35
9
25
21.
10 37
+ 10
10
8 5
2 40
9
15
Aug. I.
II 23
+ 4 49
8 27
2 43
8
59
II.
12 4
—
16
8 45
2 44
8
43
21.
12 44
' 5
21
9 3
2 45
8
27
31.
13 24
— 10
16
9 20
Mars.
2 45
8
10
July I.
3 2
+ 16
16
I 26 A.M.
8 23 A.M.
3
20 P.M.
II.
3 30
+ 18
14
I 9
8 13
3
17
21.
3 59
+ 19
54
12 51
8 2
3
13
Aug. I.
4 30
+ 21
22
12 34
7 50
3
6
II.
4 58
+ 22
22
12 18
7 39
3
21.
5 26
-^ 23
3
12 4
7 27
2
50
31.
5 54
+ 23
26
II 50 P.M.
7 15
2
40
Astronomical Society of the Pacific. 1 1 1
Jupiter.
July
Aug.
r.
I.
31.
12
12
12
10
24
44
+ 21 II 30 A.M.
- I 20 9 47
.- 3 31 8 17
Sa turn.
5 31 P.M.
3 43
2 5
II
9
7
32 P.M.
39
53
July
Aug.
I.
I.
31.
16
16
16
21
16
18
- 19 38 4 50 P.M.
- 19 33 2 44
- 19 43 12 47
Uranus,
9 41 P.M.
7 35
5 38
2
12
10
32 A.M.
26
29 P.M.
July
Aug.
I.
I.
31-
15
15
15
52
49
50
— 20 4 23 P.M.
— 19 55 2 19
— 19 58 12 22
Neptune
9 12 P.M.
7 8
5 II
2
II
10
I A.M.
57 PM.
July
Aug.
I.
I.
31.
5
5
5
29
34
37
+ 21 59 3 32A.M.
+ 22 I I 35
4-22 2 II 39 P.M.
10 51 A.M.
8 54
6 58
6
4
2
10 P.M.
13
17
Eclipses of Jupiter s Satellites, P. S. T.
(Off right-hand limb, as seen in an inverting telescope.)
I. R.
July
2.
H. M.
7 47 P- M-
11. R.
Aug.
7-
H. M.
8 6 P. M
III. D.
5.
9 40 p. M.
lll.D.
10.
6 38 p. M
11. R.
6.
8 27 p. M.
III. R.
10.
7 51 P. M
I. R.
9.
9 42 p. M.
I.R.
17-
8 14 p. M
I. R.
18.
6 6 p. M.
I, R.
26.
4 37 p. M
I. R,
25-
8 I p. M.
11. R.
31.
5 31 P- M.
(TWENTY- NINTH) AWARD OF THE DONOHOE
COMETMEDAL.
The Comet-Medal of the Astronomical Society of the Pacific
has been awarded to C. D. Perrine, Assistant Astronomer in
the Lick Observatory, for his discovery of an unexpected comet
on March 20, 1898.
The Committee on the Comet-Medal,
J. M. Schaeberle,
Wm. M. Pierson,
Chas. Burckhalter.
May 20, 1898.
NOTICES FROM THE LICK OBSERVATORY.*
Prepared by Members of the Staff.
Photograph of the Total Eclipse of the Sun,
January 22, 1898.
[See Frontispiece.]
The original negative from which the eclipse plat^, shown in
our frontispiece, was made, was taken by Professor Campbell
with the Floyd telescope, exposure time five seconds.
Those who are familiar with the difficulty of making even
satisfactory contact positives from eclipse negatives, need not be
told that a large part of the detail shown by the original is
necessarily lost in the reproduction. A notion of the general
form of the corona only can be gained from the print; the
details must be studied on the original negatives.
Changes in the Staff of the Lick Observatory.
Professor James E. Keeler arrived at Mt. Hamilton and
assumed his duties as Director of the Lick Observatory on
June 1st. Professor Campbell returned to the Observatory from
his expedition to India on the same day.
A note concerning Professor Schaeberle's resignation will
be found on another page.
Electric Illumination of the Micrometers at the
Lick Observatory.
For nearly two years and a half, electric illumination has been
used for the micrometers of both the .12- and 36-inch telescopes,
and it has proved so satisfactory that oil illumination is no longer
in use except on rare occasions and then only in case of emergency.
The current is supplied by a storage battery, five cells of which
are ordinarily used on a lamp at a time, giving about ten volts,
one-half ampere and one-half candle power. The battery is
• Lick Astronomical Department of the University of California.
114 Publications of the
charged from time to time, as may be necessar}', by means of a
dynamo.
In each case the electric lamp is fitted to the end of a small
wooden cylinder of the same size as the oil lamp previously used.
This cylinder takes the place of the oil lamp in the apparatus
attached to the micrometer, no. change in this being made. Wires
run from the lamp through the cylinder to a switch within easy
reach of the observer at the eye-end of the telescope. The wires
from the battery are brought up to the pier, where a cable is
attached of sufficient length to reach any part of the dome. A
plug at the end of the cable completes the circuit at the switch.
This arrangement is very satisfactory, and it has decided
advantages over oil illumination. It is perfecdy under control,
any degree of illumination of the wires being easily obtained. It
may be instantly extinguished by turning the switch or by with-
drawing the plug, and as readily turned on. It is not affected
by wind and there is no dripping oil. It may be completely
covered up, preventing the escape of extraneous light, which is
especially desirable in observing exceedingly faint objects. And
it takes but a moment to change to the oil lamp in the case of
emergency. W. J. Hussey.
The Lowell Observatory Catalogue of Double Stars.
A most important contribution to double-star astronomy is
Dr. T. J. J. See's catalogue of ** Discoveries and Measures of
Double. and Multiple Stars in the Southern Heavens,'* recently
published in the Astronomical Journal, The catalogue contains
the positions for 1900.0, and measures of the position-angle and
distance of 500 new stars between the limits 20° and 65** South
Declination, which were found by Dr. See and Mr. Cogshall
with the 24-inch telescope of the Lowell Observatory during the
sixteen months ending December 31. 1897. The components of
122 of the stars are separated by less than i", and in many of
the wider pairs one component is very faint. With respect to
the proportion of close and difficult stars contained, the list there-
fore takes a high rank. In the course of the work, 500 stars
previously known were measured also,* and. Dr. See states,
more than 100,000 stars were carefully examined.
It is to be regretted that the magnitude of the undertaking
* Measures to be published later in A. N.
Astronomical Society of the Pacific. 115
prevented the carrying out of the original plan of measuring each
star on three different nights. Nearly three-fifths of the number
were passed with two observations made on one night only and by
one observer only. One fears that the positions resulting from
such measures, though * * made in a manner as independent as
possible, ' ' will not be sufficiently reliable to make it certain that
differences between these and future measures are due to motion
in the stars. For, as noted above, many of the stars are difficult,
and the catalogue contains a number of instances of discordances
in the measure of a star by the same observer on different nights,
amounting in some cases to from i" to 3" in a mean distance of
8" or less» and occasionally to 10®, and even more, in position
angle. We must also acknowledge that we cannot understand
why some discordant measures are rejected (e. g. A, 42, \ 112),
while others, equally discordant (e. g. A, 76, \ 170) are given
full weight.
It is to be hoped that Dr. See may soon find time — even at
the cost of delaying the completion of his survey of the southern
heavens — to recur to the more promising of those stars in the
present catalogue which were measured on one night only, and,
by additional measures, place the present position of the compo-
nents beyond doubt; lor it is highly probable that a number of
these stars will show rapid motion. R. G. Aitken.
Changes in the American Ephemeris.
In the preface to the American Ephemeris for 1900, just
received, Professor Harkness states that certain changes of
importance have been introduced in the volume. ** First, the
constant of precession for the epoch 1900.0 has been changed
from 50". 2638 to 50". 2482; the constant of nutation for the
same epoch has been changed from 9". 2231 to 9". 21; the con-
stant of aberration has been changed from 20". 4451 to 20". 47;
and the constant of solar parallax from 8". 848 to 8".8o. Second,
Professor Newcomb*s tables of the Sun, Mercury and Ventis,
and Dr. Hill's final printed (as distinguished from his provi-
sional manuscript) tables of Saturn have been substituted for the
tables which were formerly used. Third, the 175 additional fixed
stars, whose apparent Right Ascensions only were heretofore
given, have been transferred to the regular list, which now con-
tains their complete apparent places throughout the year.'*
The volume, it seems, was prepared entirely under Professor
Newcomb*s supervision, before his retirement in 1897.
ii6 Publications of the
The changes in the astronomical constants above noted are
made in conformity with the decisions of the Paris Conference
on Fundamental Stars, held in May, 1896. They have also been
introduced in the English Nautical Almanac for 1901, recently
issued, and will be introduced in the Berliner Astronomisches
Jahrbuch and the Connaissance des Temp? for the same year.
Considerable opposition to these changes at this time has
developed among astronomers; and those who are interested may
find a vigorous discussion of the subject in recent numbers of the
Astronomical Jour ncd, R. G. A.
Solar Observations in 1897.
In the AstrophysicaJ Journal for March 1898, Professor P.
Tacchini gives a r6sum6 of the solar observations made at the
Royal Observatory of the Roman College during the second half
of 1897. From his tables it is seen that the spots have con-
tinued to decrease, particularly in area, while the prominences
have remained practically stationary in activity. The promi-
nences have continued to show themselves in nearly all zones —
with a maximum of frequency between the equator and — 20°.
Two secondary maxima, however, occurred in the zones di 40** to
it 60°. The spots were confined to regions within 20*^ of the
equator. One eruption was observed on November 23d. A very
bright jet suddenly formed on the west limb at latitude -j- 8^.2 and
rose to the height of 168'' (about 15,000 miles), disappearing in
twenty minutes. R. G. A.
New Elements of Comet b 1898.
I have derived the following elements, using my observations
of March 19th, 22d, and 26th.
T= 1898 March 16^79123
0)= 46° 57' II".6^ ^ ,. .
o 2 o f Ecliptic and
0= 262 18 53 .1 > w ^ y coo
( Mean Equinox of 1808.0.
t= 72 21 14 .4 ) ^ ^
log g = 0.040024.
Residuals for the middle place, observed — computed
A A' cos/3' +o".3
A/}' -0.3
C. D. Perrtne.
Mt. Hamilton, April 5, 1898.
Astronomical Society of the Pacific, n?
Elliptic Elements of Comet b, 1898, and a Certain
Similarity to the Comets of 1684, and 1785 I.
Using the following observations of this comet: —
1898. Mt. Hamilton M. T. App. a App. <
March 19, 16^ 47- 21* 21*' i8» 36-.89 + 16° 43' 23".3
April 8, 16 19 7 22 41 0.88 +36 20 50.5
April 28, 15 26 54 o 23 20.68 +49 41 32 .4
I obtained the following system of parabolic elements: —
T = 1S98 March 17.35984 Gr. m. t
co= 47° 36' 8".o^ _ ,. . ,
^ , ^ f Ecliptic and
0=262 32 26 .3 > .- _ r
^ ( Mean Equinox 1898.0
z = 72 26 50 .4 J ^ ^
log q = 0.040820
The residuals from these elements for the middle place being —
Observed — Computed, A A' cos )8' — 14". 7
A )8' + 22 .4
From the same observations I then obtained the following
system of elliptic elements: —
Epoch 1898, March, 20.0 Gr. m. t.
M= 0° o' 34". I
> 1898.0
0) = 47 14
48
.8
= 262 24
42
.9
1 = 72 32
55
.8
log^= 0.039179
- a= 1.656386
** e= 9.989386
** /A= 1.065428
/A= ii".62595
* 77° 23' 3". 5
Period, 305.208 years.
The residuals for the three places used are: —
O-C. « a
-i".2 4- I". I
— o .3 - I .2
+ .5 + I .1
The brightness of the comet remained almost unchanged for
several weeks. The comet has been losing its light more rapidly
the past ten days. It still retains its stellar nucleus; but this, too,
is fading slowly, and is not brighter now than 10 magnitude.
ii8 Publications of the
Since ascertaining that this comet is periodic I have been led
to notice more particularly a similarity which exists between its
orbit and those of 1684 and 1785 I. Below are the approximate
elements of the three comets for comparison: —
1684 330°. 3 268° 2 65^.4 0.958
1785 I 205 .7 264 .2 70 .2 1. 143
1898 b 47 .6 262 .5 72 .4 1094
The agreement of the positions and dimensions (O, ;, and ^)
of the three orbits is sufficiently close to warrant the belief that
the three comets belong at least to the same family. The differ-
ences in 0) are very large, too large to believe at first sight that the
orbits all belong to the same comet — unless the discrepancies
can be satisfactorily accounted for. It is to be noticed, however,
that the variations in w are in the same direction. The intervals
of 10 1 and 113 years do not agree well with the period found
for the present comet, on an assumption that all three are
appearances of the same object. The period of 305 years for
the present comet must be considered uncertain to a large degree,
however. All things considered, it looks more as if all three
comets were members of one family than that they were appear-
ances of the same body.
The comet of 1684 was discovered by Bianchini at Rome,
and was visible to the naked eye. It was visible only a short
time, the observations extending over the period July 1-17. only.
The comet of 1785 I was discovered by Messier at Paris.
While it does not appear to have been so bright as the one o
1684, it was observed for some five weeks. C. D. Perrine.
Mt. Hamilton, Cal.. May 9, 1898.
CoMETARY Discoveries.
The total number of comets observed sufficiently well during
the last thirty years (i 868-1 897) for their orbits to be calculated
amounts to one hundred and thirty-five, but of these thirty-seven
were returns of periodic comets which had been previously seen.
The average rate of apparition of new comets has, therefore,
been 3.27 annually, and of new and periodic comets, 4.5 annually.
In 1873, 1881, 1892, and 1896, seven comets were discovered;
in 1872 not one was observed; and in 1875 the only two comets
which appeared were known ones. The best months for the
discovery of these objects appear to be July and August.
January,
22
February,
21
March,
24
April,
27
May,
20
June,
22
Astronomical Society of the Pacific. 119
Of three hundred and twenty-eight comets discovered between
the years 1782 and 1897, inclusive, the following are the numbers
in the various months: —
July, 37
August, 43
September, 25
October, 26
November, 34
December, 27
These figures include every description of those objects. Dur-
ing^ the sixty years from 1782 to 1841 there were eighty-seven
comets, averaging 1.45 per year; but during the fifty-six years
from 1842 to 1 897 there were two hundred and forty-one comets,
averaging 4.30 per year. W. F. Denning.
Knowledge, April, 1898.
The Variable Star Z Centaur r and the Nebula
N. G. C. 5253.
In December, 1895, ^^^ Harvard College Observatory an-
nounced that from an examination of the Draper Memorial pho-
tographs taken at Arequipa, Peru, Mrs. Fleming had discov-
ered a **new star** in the constellation Centaurus, The variable
character of this star has since been fully established, and it has
received the definitive name Z Centaiiri,
No trace of the star has been found on the fifty-five photo-
graphs taken from May, 1889, ^o June, 1895, but it appears on
those of July, 1895, having a brightness of 7.2 magnitude, and
on that of December 19, 1895, as 11 magnitude.
In the latter part of December, Professor Campbell estimated
its magnitude at 11. 2. During the two months following it
decreased in brightness very slightly. On June 11, 1896, I found
that it had decreased to 14.4 magnitude. Fifteen days later it
was 15^, and on July 9, nearly 16. Since then I have looked
for it every month or two when within reach, and on all these
occasions have found it either invisible in the large telescope or
not brighter than the i6th magnitude. During this time, when
visible, the star has been difficult on account of the faint nebula
surrounding it. This nebula, when seen under the best condi-
tions, has every appearance of being a part of the nebula N. G. C.
I20 Publications of the
5253. Regarding it so, the latter nebula, as seen in the large
telescope, may be described as having somewhat the same form
as the Great Nebula in Andromeda as seen in a very small tele-
scope. There are, however, these important differences: N. G. C.
5253 has a relatively stronger central condensation, and its ends
are not equally bright, the south preceding end being many times
brighter than the north following end in which Z Cciitauri is
situated. W. J. Hussev.
**A Remarkable Object in Perseus.'*
In the Wolsingkam Observatory Circular, No. 46, Rev. T. E.
EsPiN announces the discovery of **A remarkable object, hitherto
unrecorded, on January 16, and seen on three other nights.'* He
describes it as elliptical, one degree long, major axis 336°, and
rather resembling some obscuring medium than a nebula.
At the first opportunity after the receipt of the notice of
this discovery at the Lick Observatory, I obtained photographs
of this region with the Crocker Telescope. The exposures were
two hours in length, and the nights first-class. My plates show
an elliptical area largely devoid of stars in the position given by
Mr. EsPiN for his object. This area corresponds exactly tp a
like one on the DM charts. My plates also show other areas
devoid of stars, but none so large or so symmetrical as that
referred to, and it is well known that many such areas abound in
the Milky Way. E. F. Coddington.
May 20, 1898.
A Correction.
It seems desirable to correct a statement contained in the
May issue of Popular Astronomy,
My resignation from the Lick Observatory takes effect at the
close of the present month, and not one year hence, as stated in
the above-mentioned publication.
The Regents of the University of Califomina urged me to
withdraw my resignation, and offered me a year's leave of absence
with full pay, but I could not accept their kind offer, as I feel
satisfied that my present course is the proper one for me to take.
In justice to Professor Keeler, I desire to say, that had the
Regents elected any other man as director my action would have
been exacdy the same. J. M. Schaeberle.
Lick Observatory,
University of California. May 11, 1898.
Astronomical Society of the Pacific. 121
Recent Changes in the Double Star 02 341.
I have recently examined 02 341 on three good nights with
the 36-inch telescope without obtaining any indication of its
being double. This result was wholly unexpected. All the
measures of the star from the first ones in 1846, to the last ones
in 1886, are in fairly good agreement in indicating that the com-
ponents are. relatively fixed. Previous observers have generally
estimated the magnitudes the same, 7.0 or 7.5, and the average
of the distances given by the measures from 1846 to 1886 is
between o".4 and o".5. At this distance, on a good night, the
star would be an easy object for the large telescope. The star
has closed up since 1886, and this shows that the motion since
that time has been rapid. It also proves that thcf star is a binary,
and it is not difficult to imagine such a disposition of the elements
of its orbit as will account for the apparent fixity of the com-
ponents during the period mentioned. For illustration, if we
arbitrarily assume the following: system of elements: —
T =
= 1898.33
O:
= 90°
ft) :
= 90°
i ••
= 90°
e ■■
= 0.75
a
= o".75
H-
= 1^.5
Period
, 240 years;
and compute the positions for the dates of observation and com-
pare them with the observed places, we shall obtain the residuals
given in connection with the observations below. The observa-
tions that I have found are as follows : —
Date.
Position
angle.
Distance.
No. of
nights.
Residuals.
O-C
Observer.
1846.09
93°.o
o".53
3
+ 3^
^0
+ 0"
09 Otto Struve
1852.27
95 .5
.52
3
+ 5
•5
+
.05 Otto Struve
1866.32
88 .5
.6est
. 3^1
— I
•5
-fo
.10 Dembowski
187I.61
90 .7
3.0
+
.7
Dembowski
1878.28
84 .0
.38
3
-6
.0
—
.09 SCHIAPARELLI
1883.64
91 .4
.40
3
+ I
.4
—
.02 Perrotin
1884.55
91 .2
.45
3
+ 1
.2
4-0
.04 Perrotin
1886.39
86 .3
.52
7
-3
•7
4-0
.21 Engelmann
1898.32
Single.
3
.0
00 Hussev
122 Publications of the
It may be noted that Dembowski, Schiaparelli and Engel-
MANN observed with small telescopes, of 7J4 and 8 inches aper-
ture, and that the star must have been very difficult for them.
Dembowski did not measure the distance, and estimated it on
one night only. Schiaparelli' s largest position-angle differs
17°. 8 from his smallest, and Engelmann's largest 3o°.7 from
his smallest. These discordances bear witness to the difficulty of
the star for these observers, and may account for the magnitude
of some of the residuals given above.
It is evident that no reliable system of elements for this star
can now be obtained. The necessary data for the determination
of the orbit does not exist It will be necessary to wait, at least,
until the star becomes measurable again. The elements above
are given merely to show that the long period of apparent fixity
of the components and their present closeness or singleness are
not incompatible, but that they find a ready explanation in the
binary character of the star. W. J. Hussey.
May 24, 1898.
New Elements of Comet b 1898, (Perrine).
From my observations of March 21st, April 8th, and April
22d, I have computed the following elements of this comet: —
T= 1898 March 17.37195 Gr. M. T.
0,= 47^3/ 6".2J E^ii i,3„dMean
'^ \ -^ [ Equinox of 1898.0.
i = 72 26 56 .1 j ^ ^
iogq= 0.040916
O— C: AA'cos/}'=— 4".2, ^P' = +i2".^
From the same observations I also computed three other sys-
tems of elements, using different values of the ratio of the cur-
tate distances. The four systems of elements are nearly the
same. The residuals given above cannot be materially improved;
their ratio may be changed, but the sum of their squares cannot
be sensibly diminished. A careful examination of the data does
not reveal any error to which the magnitude of the residuals may
be attributed. These circumstances, taken in connection with the
fact that the comet has a well-defined nucleus, making accurate
observations of it comparatively easy, lead to the conclusion that
the true elements of the orbit are not parabolic. W. J. HussEV.
April 28, 1898.
Astronomical Society of the Paxific. 123
A New Large Nebula in Ursa Major,
While examining some negatives which I obtained with the
Crocker telescope on April 17 and 20, 1898, I discovered a large
faint nebula not given in N. G. C, nor in the supplement to
N. G. C, nor have I been able to find it in any of the more
recent catalogues.
On the night of April 22d, Professor Hussey and I observed
it with the 1 2-inch telescope, and found the position of its brightest
condensation to be
a= 10^ 18"" 7'
8= +69° lo'.i
referred to the mean equinox of 1860.0.
The telescope shows it to be large, irregular, very faint, and
composed of a number of condensations.
On May 19th I obtained an additional photograph of this
region with an exposure of four hours. This shows the different
condensations to be connected by faint nebulous matter, and the
whole to extend over an area fully 4' in width and 1 2' in length.
E. F. CODDINGTON.
May 25, 1898.
The Rumford Medal.
* * At the annual meeting of the American Academy of Arts
and Sciences held in Boston on May i ith, the report of the Rum-
ford Committee, which was there presented, contained the follow-
ing important statement and recommendation: —
The committee has also considered at length the question of
an award of the Rumford medal. The claims of various investi-
gators and inventors have been considered with great care, and
more than one among them appeared to be deserving of such
recognition. After prolonged consideration, the Rumford Com-
mittee has voted at two separate sessions (in accordance with
long-established custom) to recommend to the Academy an award
of the medal to Professor James E. Keeler, now Director of
the Lick Observatory, for his application of the spectroscope to
astronomical problems, and especially for his investigations of
the proper motions of the nebulae, and the physical constitution
of the rings of the planet Saturn, by the use of that instrument.
The report of the committee was presented by the chairman,
Professor Cross, who explained at some length the particular
nature and merit of the investigations of Professor Keeler for
124 Publications of the
which the award of the Rumford premium was proposed, after
which the Academy voted unanimously to adopt the recommenda-
tion of the committee.
The last previous award of the medal was to Mr. T. A. Edison,
in 1895. Among others who have recently received it are Profes-
sors Pickering, Michelson, Langlev, and Rowland.*' —
Science, May 27, 1898.
Stellar Parallax.
From Herr Bruno Peter's results, published in A, N. 3483,
of a series of observations made with the Leipzig heliometer during
the years 1887-92, we have taken the following list of values for
parallax and proper motion: —
Star.
P.M.
Parallax.
17 Cassioi>eice
I". 20
+ o".i8
fi CcLSsiopeice
3 .74
+ .13
Lai, 15290
I .97
+ .02
LaL 181 15 prec.
-h .18
LaL 18 II 5 fol.
+ .18
LaL 181 15 mean
I .69
+ .18
^ Ursce majoris
I .11
+ .09
A, CE, 10603
I .45
+ .17
pComa
I .20
+ .11
31 AquilcB
.96
-ho .06
Bradley 3077
2 .08
Erratum.
+ .13
R. G. A.
In No. 61 of these Publications, p.
78, line I, word 2,
date read data.
for
Astronomical Society of the Pacific. 125
Minutes of the Meeting of the Board of Directors,
held at the lick observatory, june ii, 1898.
President Aitken presided. A quorum was present. The minutes
of the last meeting were approved. The following members were duly
elected:—
List of Members Elected June ii, 1898.
Mr. Fred. R. French { ^ M^.^' ^'^^ "^"' Brockton,
Mr. C. J. Goodrich Robinson, Brown Co., Kansas.
It was, upon motion
Resolved^ That the Publication Committee be empowered to furnish reprints of
articles free of cost to persons contributing by request.
The name of Professor James E. Kbeler, Director of the Lick
Observatory, was added to the Comet-Medal Committee, to date from
June I, 1898. Professor J. M. Schaeberle retiring.
The Committee on the Comet-Medal is now composed of Messrs.
James E. Keeler {ex-officio), Wm. M. Pierson, Chas. Burckh alter.
Adjourned.
Minutes of the Meeting of the Astronomical Society
OF THE Pacific, held at the Lick Observ-
atory, June ii, 1898.
President Aitken presided. The minutes of the last meeting were
approved. The Secretary read the names of the new members elected
at the Directors* meeting.
The following papers were presented: —
X. a Variable SUr Atlas, by Father J. G. Hagan.
2. On the Causes of the Sun's Equatorial Acceleration and the Sun Spot Period, by Mr.
E. J. WlLCZYNSKI.
3. Review on Professor Todd's "New Astronomy," by Professor W. J. Hossey.
4. Observations o( Mira Ceti, by Miss Ross O'Halloran.
5. The Red Stars, V Hydrae and 277 of Birming^ham's Catalogue, by Miss Rose O'Hal*
loran.
6. Planetary Phenomena for July and August, 1898, by Professor Malcolm McNeill.
7. Profenor J AMES E. Keuler exhibited photographs of the Spectra of Stars obtained at
the Allegheny Observatory.
Adjourned.
126 Publications of the Astronomical Society ^ &c,
OFFICERS OF THE SOCIETY.
Mr. R. G. AiTKEN Prtsiden.r
Mr. C. B. Hill First Vice-President
Miss R. O'Halloran Second Vice-President
Mr. F. H. Searrs . . * Third Vice-President
Mr. C. D. Pbrrinb \ o.-^/^„v,
Mr. F. R. ZiBL 1 • Secretaries
Mr. F. R. ZiEL . . Treasurer
Board of Directors ~^\^s>%x%. Aitkbn, Hill, Kbblbr, Molbra. Miss O'Halloran, Messrs.
Pbrrinb, Pibrson, Sbarbs, St. John, von Gbloern, Ziel.
Finance Committee — Messrs. Pibr>on, von Gbldbrn, Hill.
Committee on Publication — Messrs. Aitkbn, Sbarbs, von Gbldbrn.
Library Committee— Mes&rs. Sbarbs, Gbo. C. Edwards, Miss O'Halloran.
Committee OH tfu Comet-Medai—Messn. Schabbbrlb {ex-officio)^ Pibrson, Burckhalter.
OFFICERS OF THE CHICAGO SECTION.
Executive Committee— }Au Ruthvbn W. Pikb.
OFFICERS OF THE MEXICAN SECTION.
Executive Committee— M.T, Francisco Rodriguez Rev.
NOTICE.
The attention of new members is called to Article Vlll of the By-Laws, which provides that
the annua) subscription, paid on eleaion, covers the ca/endar year only Subsequent annual
payments are due on January ist of each succeeding calendar year. 1 his rule is necessary in
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Astronomical Society of the Pacific 819 Market Street, San Francisco.
It is intended that each member of the Society shall receive a copy of each one of the Pu6-
lications for the year in which he was elected to membership and for all subsequent years. If
there have been (unfortunately) any omissions in this matter, it is requested that the Secretaries
he at once notified, in order that the missing numbers may be supplied. Members are requested
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The Committee on Publication desires to say that the order in which papers are printed in
the Publications is decided simply by convenience. In a general way, those papers are printed
first which are earliest accepted for publication. It is not possible to send proof sheets of papers
to be printed to authors whose residence is not within the United States. The responsibility {<a
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Society itself.
The titles of papers for reading should be communicated to either of the Secretaries as early
as possible, as well as any changes in addresses. The Secretary in San Francisco will send to
any member of the Society suitable stationery, stamped with the seal of the Society, at cost price,
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PUBLICATIONS ISSUED BIMONTHLY.
( February t Aprils June, August ^ October , December.)
Y U L LI C Li i 1 u\ R Y
AflTOR, LENOX; AND
T.'LOFr P0Urrv\T!OM9.
TflF. NEv7 YORK
PUBLIC LIBRARY
ASTOn, LENOX AND .
TILOEN POUN^T^sfl LIGATIONS
OF TH B
THE NEW YORK
PUBLIC LIBRARY
ASTOR, LENOX. AND
TILOEN POUM0ATION8.
Astronomical Society of the Pacific.
Vol. X. San Francisco, California, August i, 1898. No. 63.
A GENERAL ACCOUNT OF THE LICK OBSERVATORY-
CROCKER ECLIPSE EXPEDITION TO INDIA.
By W. W. Campbell.
The editor of this journal having requested me to furnish an
account of the recent Lick Observatory Eclipse Expedition to
India, I am glad to comply, on the understanding that no
attempt shall be made to include the scientific results. While
the expedition met with abundant success, the photographs have
not yet been studied in the least. With practically every sum-
mer night clear for current observational work, the critical
investigation of the eclipse plates must await the cloudy winter
weather.
It has been the policy of the Lick Observatory to send out
members of its staff to secure observations on the Sun's outer
portions during all the available total solar eclipses. The eclipse
of January i, 1889, was observed in northern California by
Messrs. Keeler, Barnard, Hill, and Leuschner; that of
December 22, 1889, was observed at Cayenne, French Guiana,
by Messrs. Burnham and Schaeberle ; that of April 16,
1893, was observed at Mina Bronces, Chile, by Professor Schae-
berle, and his volunteer assistants from many parts of the world.
The Lick Observatory Expedition sent in Professor Schae-
berle 's charge to observe the eclipse of August 9, 1896, in
Japan, occupied four stations, but clouds obscured the Sun at all
the stations.
The eclipse of January 22, 1898, began at sunrise in central
Africa. The path of the shadow moved eastward to the Indian
Ocean, thence inclining toward the northeast across India, ending
128 Publications of the
at sunset in Mongolia. The duration of totality was longest in
the Indian Ocean, 2" 26*, It decreased slowly from about 2" 5'
on the west coast of India to about i" 20" on the northeastern
frontier of that country. The most available points for observa-
tions were in western India, with Bombay as the port of entry
and base of supplies. Not only was thb region the most acces-
sible from the well-established routes of travel, but, what is more
important, the astronomical conditions were the most favorable.
The altitude of the Sun would be the greatest, from 50° to 52®,
and there was the least probability of interference from clouds.
January is in the ** dry season" of India. The splendid report on
the meteorology of the eclipse path prepared by the English
Government in India showed that the weather in western India
in January is very much like our beautifully clear weather on
Mt. Hamilton in July and August That eclipse parties would
be favored with clear skies was almost a certainty. In view of
these facts, it was not considered that the great dbtance — half-
way around the globe — was an element in the question of send-
ing an expedition to that country.
The late Colonel C. F. Crocker, who had so generously
defrayed the expenses of the earlier expeditions to Cayenne and
Japan, expressed his interest in keeping up this line of work, and
his willingness to provide means not only to send the expedition
to India, but also for securing a substitute at Lick Observatory
for the absent astronomer. This magnificent offer was made only
a few days before his untimely death. The Board of Regents,
of which Colonel Crocker was a member, accepted the offer
with gratitude, and authorized me to proceed to India and estab-
lish a suitable observing-station.
It was thought best not to interrupt my regular work of
determining stellar velocities in the line of sight; and as my
substitute to carry on that work did not arrive until toward the
middle of August, there remained but two months in which to
make preparations. Professor Holden kindly placed the instru-
mental and mechanical resources of the Observatory at my
disposal, so far as they could be spared. Deficiencies in our
equipment were generously filled in by loans from friends of the
Observatory. Thus the excellent Dallmeyer portrait-lens used
at previous eclipses was again placed at our disposal by the
Hon. William M. Pierson. Princeton University, through
Professor Young, loaned us its train of four compound prisms
Astronomical Society of the Pacific. 129
and several minor pieces of apparatus. Aside from the clock in
the 6-inch equatorial mounting, the Observatory could not well
spare other driving-clocks. Two additional ones were impera-
tively needed, and they were supplied by loans from Professor
HussEY and Mr. L. C. Masten. To save time, the four new
spectrographs designed by me for the use of the expedition were
mounted in wood (Spanbh cedar) from my drawings, by the
Observatory carpenter. In transit to India via Singapore and
Colombo, these wooden mountings passed through a climate so
moist and hot that it resembled a steam-bath. In India they
were exposed for six weeks to the direct rays of the blazing sun,
and to a remarkably dry atmosphere. That they worked satis-
fcictorily is due to the quality of the wood and the excellent work-
manship of the carpenter.
The experience of Professor Schaeberle in Chile left no
doubt in my mind that there would be an abundance of willing
and able volunteer assistants in India to man all the instruments
I could take with me. It was decided to take nine instruments,
all for photographic use, as follows: —
A, — Three spectrographs for recording the spectrum of the
Sun*s edge, continuously, for a few seconds at the beginning of
totality, and a few seconds at the end of totality, by means of
plate-holders moving at a uniform rate by clockwork. This was
a process which I had invented for use at the Japan eclipse, but
personal reasons prevented me from taking that trip. As it was
not known how bright the spectrum of the Sun's edge would be,
I devised three instruments, whose proportions were such that
the resulting intensities of their spectra would be very different,
hoping that if one instrument under-exposed the spectrum,
another would give the proper exposure. Two of these instru-
ments were mounted on the 6-inch equatorial mounting, and the
third on a large •* polar axis.**
B, — A spectrograph for recording the bright coronal line
1474 K, using light from the equatorial region of the corona both
east and west of the Sun, to determine the displacement of the
bright line due to motion in the line of sight, and thence to
determine the law of rotation of the corona. Previous attempts
to solve this problem made use of the violet calcium lines H and
K; but as there was good reason to believe that those lines were
not coronal, I decided to use the 1474 K line, which, to a great
extent at least, is truly coronal. This line lies in a part of the
I30 Publications of the
spectrum for which photographic plates are not very sensitive.
Furthermore, to secure the dispersion sufficient for solving this
problem, six prisms were necessary. The loss by reflection and
absorption in such a prism train would be very great. The
brightness of the line itself could not be estimated, since so few
of those who had previously observed the line had published the
constants of their instruments. Again, it was uncertain from the
published observations whether the line was of fairly constant
brightness, or varied widely for different eclipses. The prospect
of photographing the line with my instrument was not promising,
but merited a trial.
C — A very efficient one-prism spectrograph, for recording the
bright-line spectnim of the corona, for recording the continuous
and possible dark-line spectrum of the corona, and incidentally
the position of the maximum photographic brightness of the
continuous spectrum.
D, — The 40- foot camera designed by Professor Schaeberle,
and used by him so successfully at the Chile eclipse. He had
used the Clark 5-inch photo- heliograph lens. It seemed to him
desirable to have a 6-inch lens for this camera, and such a lens
was secured by the Observatory. But, when I tested it, defects
were found to exist, such that its use was not warranted. There
was not time to remedy the defects, and it was decided to use
the 5-inch lens. In designing the carriage and track for the
movable plate-holder, I followed the simple and practical plans
used by Professor Schaeberle. The purpose of this camera
was to secure photographs of the inner corona on a large scale,
with exposures of moderate length. The Moon's image with it
would be nearly 4^/^ inches in diameter.
E. — The Floyd photographic telescope, of ^v^ inches aj>erture
and about sixty-eight inches focal length, mounted on the ** polar
axis,'* for recording the general features of the corona. It is a
splendid instrument for the purpose.
F, — The Dallmeyer portrait-camera, of 6-inch aperture and
33-inch focus. This is a valuable instrument for recording the
outer corona, on a small scale, and for recording any strange
object that may happen to be within a few degrees of the Sun.
This camera was likewise to be mounted on the polar axis.
G, — An ordinary camera of 11 -inch focus and i^-inch aper-
ture, the lens giving splendid definition over a very large field.
This instrument was intended to supplement in a general way
the Dallmeyer lens.
Astronomical Society of the Pcuific. 131
The polar axis, which carried five instruments, was a strong
plank box, twelve by fifteen inches in section, and nine feet long,
mounted parallel to the Earth's axis, on steel pivots at each end,
running in roller bearings. From the middle of one side of the
box a strong arm, thoroughly braced in every direction, ran out
ten feet, at right angles to the box. On the outer end of the arm
a sector of lo-foot radius was fastened. A clock securely
mounted very close to the sector released a cord which pressed
against the face of the sector, and lowered it at a uniform rate.
It will be evident that an astronomical driving-clock applied
at the end of a lo-foot arm would give splendidly uniform
motion to the instruments attached to the axis. The polar axis
formed a packing-case to and from the eclipse.
All the instruments were set up at Mt. Hamilton, and adjusted
as &r as necessary to test thoroughly all the parts. They were
then taken to pieces, and packed as closely as was consistent with
safety, along with sextant and chronometer, American ephemer-
ides, thermometers, barometer, a good set of carpenters* and
machinists* tools, nails, screws, photographic plates, implements
and chemicals, a tent, etc. This whole equipment, in its pack-
ing-cases, formed a volume of only eighty-one cubic feet. It
was so carefully packed, and so delicately handled en route to
camp, that it arrived in perfect condition. The transfers of the
freight occurred under my personal direction, and it may be said
that the freight- handlers at nearly all points were easily persuaded
to move the boxes with great care.
I was accompanied by Mrs. Campbell and Miss Rowena
Beans of San Jose, as volunteer observers traveling at private
expense. We left San Francisco October 21, 1897, on the steam-
ship China of the Pacific Mail Company. The company kindly
offered to stow the instruments in the baggage room of the ship,
where they lay at ease in the roughest weather. The twenty-
eight-day voyage from San Francisco to Hongkong will always
be recalled with the utmost pleasure, in spite of the fact that
essentially all the rough weather experienced by us in our trip
around the world occurred on the Pacific Ocean. The fine
sailing qualities of the China, the superior discipline maintained
by the captain and officers, the splendid service and comfort
provided for all, were more than ever apparent after we had
sailed the Indian Ocean, the Red and Mediterranean seas, and
the North Atlantic.
132 Publications of the
As we sailed into Honolulu on a beautifully clear day, the
water's surface was a mirror, and all the islands above our hori-
zon were in clear view. We saw nothing on our trip to surpass
these islands in natural charm. The extinct volcanoes near the
city of Honolulu, known as the Punch Bowl and Diamond Head,
were wonderfully interesting, though they were, of course,
vastly inferior to the famous living volcano on one of the distant
islands.
Our route westward from the Hawaiian Islands lay close to
the thin chain of islands which extends nearly to Japan. A few
of these islands have been woven into the plots of Robert
Louis Stevenson's novels; and many a traveler on these
waters has broken a spell of oppressive loneliness by recalling
the story of The Wreckers, with blessings on the incompara-
ble Stevenson.
We stopped in Japan as the steamer stopped: one day each
at the ports of Yokohama, Kobe, and Nagasaki. Excursions to
Tokyo, Osaka, and Mogi were made from those points. Our
stay in this fairyland was altogether too short; but the trip was
not for pleasure, and we went on with the instruments. The
weather in Japan had been perfect; and the absolutely unrivaled
sunrise effects on their sacred mountain Fuji on two mornings,
the views of the smoking volcano on Vries Island, of the Inland
Sea, of the people and their art-treasures, these will remain with
us as priceless memories.
The steamer ascended the Yangtse-Kiang River to Woosung,
the port of entry for Shanghai. We spent a day in that interest-
ing city, — mostly in the foreign business quarter, it is unnecessary
to say. A brief trip into the native walled city was a revelation
to me as to how the other half lives, in reckless defiance of all
sanitary laws. Our friends living in the modern quarters of
Shanghai were ready to do anything for our entertainment, except
to accompany us into the native walled city of filth and con-
tagion.
The trip to Hongkong was stormy. We passed through a
genuine typhoon, which was not without its dangers. The ship
was due to arrive at Hongkong on November 19th, and a R & O.
steamer, which we hoped to sail on to Bombay, was to leave there
at noon of the i8th. The China entered the harbor on the i8th,
at 10 A. M., and, thanks to the assistance of Captain Seabury, we
were at once transferred to the P. & O. steamer Ancona, and
Astronomical Society of the Pacific. i33
started on the second stage of our journey, a seventeen-day trip
to Bombay. The instruments were again placed in the baggage-
room, and we were the recipients of many fevors from the kind
and gentiemanly officers. But as to the ship, the discipline, the
service, and the food, the less said the better. The only item
that was first-class was the price of the passage ticket.
Opportunities for seeing Singapore, Penang, and Colombo
very well were afforded by the stopping of the steamer at those
ports. Likewfee, there was time for a quick trip to Kandy, near
the center of the island of Ceylon. The wonderful vegetation of
Ceylon was a revelation, even after seeing Honolulu and Singa-
pore.
We arrived in Bombay on December 5th, having been forty-
five consecutive days on the ocean voyage from San Francisco.
The English Government in India had made every possible
preparation to assist the eclipse expeditions, of which ours was
the first to arrive. Intending observers had been supplied early
in the year with meteorological reports, with large-scale trigo-
nometrical maps covering the regions of possible observing-
stations, with data relating to railway transportation, camping-
outfits, etc. From these I had decided to locate on the central
line of totality a few miles north of Karad, a station about
one hundred miles south of Poona. This would bring us in the
high eastern foothills of the extensive range of mountains known
as the Western Ghats. The contour lines on the maps showed
that there would be no trouble in selecting a steep hillside on
which to mount the 40-foot camera so that the tube of it would
lie near the surface and the lens would require only a short sup-
port. This region would be easily accessible from the Southern
Mahratta Railway and thence by bullock-cart. Water promised
to be plentiful and near at hand. All the mountings of the
instruments had therefore been constructed for the latitude of
Karad, without a thought that the station could not be occupied.
On arriving at Bombay, I was informed by the government
representatives that the bubonic plague was raging at Karad,
and that the idea of locating there must be given up, not only on
account of the danger to ourselves but because it would be out
of the question to retain servants. The small army of servants
whom we would have to employ and depend upon would
stampede without warning if plague threatened the camp. So it
seemed best to select another station. For many reasons the
134 Publications of the
next best station was about one hundred miles northeast of
Karad, where the Great Indian Peninsular Railway crossed the
line of totality, near the village Jeur. In company with Professor
Naegamvala, the government representative, I visited Jeur
as soon as possible. Here we were met by the chief govern-
ment officer of the district, the Mamlatdar of Karmala, with
tongas, two-wheel pony-carts. We examined all the available
territory adjoining the only cart-road in the whole region. To
my surprise, the region was very flat, and no hills could be fou^d
on which to mount the large camera. Water was scarce, since
there had been almost no rain for two years. It was in the
famine district. The plague was epidemic at Sholapur to the
east, and at Poona to the west, with a few sporadic cases just
then at a distance of fifteen miles. I decided to locate at a point
four miles from the railway station of Jeur, two miles from the
central line of totality, and midway between the country villages
of Shelgaon and Wangi. As our nearest neighbors would be at
Wangi and Shelgaon, two miles in either direction from the
camp, it would be possible to quarantine against the plague if it
approached uncomfortably near us. The problem of mounting
the 40-foot camera in level country, — on a level desert, one might
almost say, — at an altitude of 51°, so that it would be secure
against wind-vibrations, was not a light matter. It would be easy
enough in a country where materials and skilled labor were at
command, but in central India it was a formidable problem. The
general features of a practicable mounting were planned before
deciding to locate in the level country, and the details were filled
in later.
The instruments were shipped from Bombay to Jeur by the
G. I. P. Ry., in a special car, under special concessions to
eclipse-observers, a distance of two hundred and sixteen miles.
Bullock-carts were the means of transportation to the camp,
four miles from the railway station. The Government not only
repaired the road over which the instruments were to be hauled,
but employed fifty men to clear the brush and rocks from the
camp-ground. A water-carrier (bhisti) and his buffalo were
supplied by the Government to bring water to the camp from a
well about three-quarters of a mile away, in skin water-bags
thrown across the buffalo's back. The Government also sup-
plied us with a ** sweeper,'* — a low-caste man who is the camp-
scavenger, — with two night-watchmen, and with some of our
camp furniture from their army stores.
THE >;EvV YORK
PUBLIC LIBRARY
A8T0R, LFNOX AND
Astronomical Society of the Pacific. i35
The Mamlatdar of Karmala, the highest official in the Taluka
(district of) Karmala, had been instructed by the Bombay
Government to look after the wants of the eclipse parties in his
district. He was a very aWe man, practical, and constant in
attendance. Our difficulties had a way of dissolving whenever
he appeared. But for him we should have suffered many a dis-
comfort in the desert. The Mamlatdar of Karmala is an Indian
gentieman, of whose friendship we were and are proud. We
shall remember him not only as a most able and faithful official,
but as a friend in need.
The instruments, tents, supplies, and servants arrived in
camp December 13th. After a day or two spent in pitching
tents, establishing camp, etc., I was relieved of all care in regard
t<^ our daily wants and comfort, and that was fortunate, since
the absence of skilled labor in that region required me to do
everything myself that needed any degree of accuracy. The
mounting of the 40-foot camera, which promised to be an easy
matter in the mountains of Karad, was a genuine problem on
the plains at Jeur. The lens at its upper end would be thirty-one
feet higher than the plateholder and about thirty-three feet
above the observer's platform. I decided to sink the plate-
holder end into a deep pit — say twelve feet — and thereby bring
the lens within twenty feet of the ground. Six or eight native
laborers were set to excavating the pit. Their implements were
little picks and hoes poorly mounted, with shallow pans to
remove the dirt from the pit. The government officials instructed
me to pay them two annas — four cents American — each, per
day, and thousands of laborers could have been secured at such
wages. But time was an object with me, and I paid them three
annas each, in consideration of their putting in a long day, of
about seven hours. Six cents a day was a princely sum to these
fellows, and to receive such wages raised them very high in the
estimation of their neighbors. Unconsciously, I was making
trouble; for when the other eclipse expeditions located in that
vicinity, the laborers demanded from them the same wages that
Campbell Sahib was paying. In a couple of weeks, under
my hourly admonition to jildy, — hurry up, — the men had sunk
the 10 X lo-foot pit down to a depth of eight feet. The soil was
dry from lack of rain, and almost rock-like, and I decided to go
no deeper. I had ordered teak lumber and nails from Poona, a
hundred miles away, for the construction of a tower to carry the
136 Publications of the
lens. The native carpenter whom I hired to assist me was very
much in the way, and was kept only three hours. I built a very
strong tower, about twelve feet square at the base, fourteen inches
square at the top, and twenty-four feet high, with diagonal bra-
cing on the four inclined faces and in the interior. Upon the
inclined top a plank was fastened, which projected into the tube
and carried the object-glass. The upper end of the tube did not
touch the tower or lens-support, but was sustained by a separate
wooden pillar. The lower end of the tube was fastened to
the firm soil by iron pins, and the whole tube was held in
place by wire cables in duplicate. The plate-carriage track was
rigidly mounted at the bottom of the pit, quite independent of
the tube. The wind could vibrate the tube without jarring either
the plate-holder or object-glass. It was necessary to protect the
tower from wind-vibrations. The lower end of it was firmly
imbedded in a heavy stone wall, filled in with soil, to a height of
about nine feet. That left the upper fifteen feet still exposed to
the wind. I built a second tower, whose sides were about eighteen
inches from the sides of the inner tower, and slightly higher. It
was held in position by duplicate cables, so that it could not be
blown into contact with the inner tower. A large canvas tent-fly
was stretched over the south, east, and north faces of the outer
tower, extending from above the lens to below the top of the stone
wall. As the prevailing winds were from the southeast and east,
the lens needed no further protection. On several days, just
prior to the eclipse, fairly strong winds were blowing at the time
when the Sun's image swept across the plate-holder, but not the
slightest vibration of the lens could be detected.
The other eight instruments were mounted rapidly, though
many changes and additions were made, involving the use, I
believe, of every tool taken with me. The adjustments to focus,
etc., were completed on January i6th, six days before the eclipse
date.
As stated above, I was trusting to volunteer observers to man
the instruments. When I first arrived at Bombay, many of the
government officials said it would be impossible to secure volun-
teer assistants from among the army, navy, or civil officers, as
they were not accustomed to such service. We had not been in
Bombay many days, however, before offers came in abundance.
Between twenty-five and thirty offers were received from men of
thorough scientific training. The total number of observers
Astronomical Society of the Pacific. ill
required to manage the instruments was twelve, or nine in
addition to the three who had gone out from California. The
abundance of volunteers made a choice almost embarrassing. I
was even obliged to decline offers from two very able and
enthusiastic amateur astronomers residing in India.
In addition to Mrs. Campbell and Miss Beans, I was assisted
by Captain Henry L. Fleet, Royal Navy, in charge of Her
Majesty's marine forces in the Bombay harbor; by the com-
manders of three of his torpedo-boats, Lieutenant Kinehan,
R. N., Lieutenant Mansergh, R. N., and Lieutenant Corbett,
R. N.; by Engineer Garwood, R. N.; by Major Boileau,
Royal Engineer; by the Rev. J. E. Abbott, who had been a
student under Professor Young at Dartmouth College; by the
United States consul at Bombay, Major S. Comfort, and Mrs.
Comfort.
The volunteer observers arrived in camp from January 1 7th to
20th. All of them were assigned to responsible positions, and it
was a pleasure to drill them in the details of the programme. The
final drill occurred the evening of January 21st, with every
observer perfectly at ease in his assigned work.
On the 2 1 St, all the clock cords were carefully examined, and
some of them renewed. The cameras, plate-holders, etc., were
tested for leaks which might let in the light, and all the adjust-
ments were verified. Some mysterious forces had disturbed the
adjustments of the 40-foot camera plate-carriage tracks in the
bottom of the pit, and the very important clock which rotated
the polar axis, on the night of January 20th. Fortunately, the
disturbances were so marked that they were noticed by me just
before beginning the rehearsal on the afternoon of the 21st. As
the Sun passed through the region of the sky which the eclipsed
Sun would occupy the following day, I had time enough, and just
enough, to readjust these very essential parts. I had not been
aware that animals came around the camp at all, but, to guard
against a similar occurrence, on the night of the 21st, Captain
Fleet suggested that he and the other observers should do
guard duty at the instruments throughout the night. Every one
entered into the plan with enthusiasm, and the instruments were
all right on the morning of the eclipse.
The plate-holders were filled the night of the 21st, most of
the plates being *' backed *' with black liquid backing.
The final examination of the instruments was made the morn-
13^ Publications of the
ing of the eclipse, to see that no cobwebs or dust could interfere
with the proper passage of the light. The wind-breaks of floor-
rugs, on bamboo poles, were put up by the naval officers. Sex-
tant observations of the Sun for determining the correction to the
chronometer were made and reduced, and the chronometer times
for the beginning and ending of totality were computed. Our
preparations were completed about two hours before tolality.
Although there were one or two thousand excursionists at Jeur^
from Bombay, Madras, and elsewhere, they were not allowed by
the government officials to come near the eclipse camps, nor
were the natives allowed to leave their villages to come to the
camp, so that our surroundings were favorable. We were in
camp seven weeks, and I should say the eclipse day was the
most perfect of all. There had been more or less wind on previ-
ous days, but the 22d was perfectly calm. The atmospheric
conditions were all that could be wished for. The observers took
their places a few minutes before the time of totality. Captain
Fleet and Engineer Garwood in the 40-foot camera; Lieutenant
CoRBETT at the chronometer, just outside the large camera,
and near the polar axis; Lieutenant Kinehan and Miss Beans at
the Pierson camera; Lieutenant Manse rgh and Major Comfort
at the Floyd telescope; Mrs. Comfort at the ii-inch camera;
Mr. Abbott at the 6-prism spectrograph; Major Boileau, at
the grating spectrograph; and Mrs. Campbell and myself at
the two spectrographs on the equatorial mounting. There was
no nervousness discoverable in the party. Lieutenant Corbett
was to give the signal at twenty seconds before totality, for Major
Boileau and myself to start the moving plate-holders of the
three spectrographs, to record the varying spectrum of the Sun's
edge, as the edge was gradually covered by the Moon. Captain
Fleet, in the 40-foot camera, was to give the signal ** Go " at
the instant when the corona flashed out at the vanishing-point of
the cresent Sun, at which signal the chronometer count was to
begin, along with the programmes of the four cameras and the two
additional spectrographs. The programme of signals and exposures
was carried out by the observers without nervousness or excite-
ment, as well as if they had been professional obser\'ers of eclipses.
The spirit of the observers may be illustrated by one or two cir-
cumstances. I had constructed a small annex tent in the pit of
the 40-foot camera, into which the observers, Captain Fleet
and Mr. Garwood, could go and look a few seconds at the
Astronomical Society of the Pacific. i39
corona. They refused to do so, and did not see the corona
except as it was photographing on the 14 x 17-inch plate. Lieu-
tenant CoRBETT was asked to keep his eye on the chronometer
during the first minute, and then feel free to count by sound as
long as he cared to view the corona during the second minute. He
did not take his eye off the second-hand during the whole of
totality. Other instances of sacrifice of self to the success of
the expedition could be mentioned. The same noble qualities
came out on the days preceding the eclipse, and with such
assistants I laughed at Failure. It is plain that no astronomer
was ever more ably assisted by volunteer observers.
The eclipse began within a half-second of the computed time,
and ended in the same way, lasting i"* 59^^'. The duration, com-
puted from the American Ephemeris, was i^SQ'; and from the
English Nautical Almanac, was 2°* 5'.
It is impossible to describe the beauty of the Sun's surround-
ings. The corona was exquisite, more beautiful by far than
anything else we saw in a journey around the world. It is well
worth a journey to remote regions of the Earth to see.
The first illustration (Frontispiece) is a general view of the
eclipse camp; and the second (page 134), taken a few minutes
after the eclipse, shows the observers at their instruments, except
those who had been in the 40-foot camera.
After the eclipse, the development of the plates was taken
up. Previous experiments had shown that the chemical formulae
used at home could not be used in India. The formulae were
experimented with until one was obtained which gave good
results. The weather in camp was very hot in the daytime, but
grew rapidly colder at night, reaching a minimum about sunrise.
The extremes were such as I had never experienced before.
When the day temperature remains for hours at 92" or 93° Fahr.,
a night temperature of 42° seems bitterly cold. Yet this range
of fifty degrees occurred several times while we were in camp.
The heat was intense during the week following the eclipse, and
greatly affected the photographic development. With a dark
room composed of one tent inside another tent, it was necessary
to wait until the atmosphere cooled down — from i a. m. till sun-
rise, and all the plates were developed in those hours. The
negatives from all the instruments came out almost exactly as
they were expected to, and the expedition was a success.
The instruments were quickly dismounted and repacked, the
HO Publications of the
photographs were packed with special care, and the tents and
camp furniture were made ready for shipping. I can still see
that long line of bullock-carts moving slowly out of our camp to
the station. Our life there was so intense, among a people so
strange and so interesting, that the individucU incidents of the
seven-weeks* camping experiences in central India will remain as
vividly with us as the general effect of the whole.
When the instruments and photographs were safely stored in
the specie-room of the Steamship Socotra at Bombay, en ratUe to
Hongkong, the eclipse was over, and we were ready to enjoy the
wonders of Delhi, Agra, the Himalayas, — but that is not an
astronomical story.
Our route homeward brought us via the observatories at Quro,
Rome, Florence, Milan, Nice, Paris, Greenwich, Tulse Hill,
Kensington, Cambridge, Oxford, and Williams Bay, where we
were the recipients of many kindnesses from busy astronomers.
I cannot close this account without a grateful acknowledg-
ment of the services rendered to the expedition by the United
States consul at Bombay, Major Comfort. I know that our
expedition was continually held in mind by him, both as the rep-
resentative of our government, and as our valued friend. We
were almost daily recipients of his assistance. The continual
kindness shown us by Major and Mrs. Comfort, by Captain and
Mrs. Fleet, and by many others, contributed both to the success
of the expedition, and to the pleasure of our visit in that wonderful
country.
Three other eclipse parties were encamped near our station:
the Japanese Government party from Tokyo; the Indian party
from the Poona College of Science, under Professor K. D.
Naegamvala; and Professor Burckh alter, from the Chabot
Observatory, in charge of the Pierson expedition. Professor
Burckhalter was just as enthusiastic in India as he is at home.
Interchanges of visits between our camps were frequent, and
gave us great pleasure. We were glad of his success, not only
because he was our countryman, but because success was deserved.
Astronomical Society of the Pcuific. 141
THE INFLUENCE OF PHYSIOLOGICAL PHENOMENA
ON VISUAL OBSERVATIONS OF THE SPEC-
TRUM OF THE NEBULA.
Bv James E. Keeler.
THEKEVv ^. .
PUBLIC Lrolv.w.
A8T0R, LENOX AND
TILOEN P0UNDAT(0N9.
According to the view almost universally accepted by astro-
physicists, the stars have been evolved from pre-existing nebulae
by a gradual process of condensation. The view is an old one ;
but before the spectroscope was invented, it was necessarily
based on very simple data, derived from observations of the
forms of nebulae as seen in the telescope. The spectroscope
opened up an entirely new method of attack. Used in connec-
tion with the great telescopes of modern times it has furnished
an immense mass of data, and the study of the different types of
stellar spectra and their probable connection with the order of
stellar evolution has become an exceedingly complicated and
interesting branch of astronomical science.
In a general way, it may be said that the evidence brought to
light by the spectroscope is in harmony with the views which had
already been held, though it would not be difficult to point out
numerous difficulties and contradictions. As the spectrum of the
nebulae is regarded as the signature of the earliest stage of stellar
evolution, it is not surprising that astrophysicists have attached
special importance to it in their studies, and that they view every
discovery or investigation relating to it with the greatest interest.
A discussion has recently been carried on in the Astrophysical
Journal and the Astronomische Nachrichten^ with reference to
the part played by physiological causes in visual observations of
the bright lines in nebular spectra. The spectrum of a nebula
contains many bright lines, most of which are, however, very
faint, and are revealed by long-exposure photographs only.
Ordinarily only a few lines are seen-^one at X 5007, (the * 'chief ''
nebular line), one at X 4959, probably due to the same unknown
substance as the preceding, and in addition to these, some of the
lines of hydrogen and helium. Some years ago. Professor Camp-
bell, while observing the Great Nebula of Orion with the thirty-
six inch telescope, found that the spectrum was different in differ-
ent regions. In the central and brighter parts of the nebula, the
ji;reenish-blue hydrogen line F, or H)3, was about as bright as the
142 Publications of the
second nebular line X 4959. In the faint and remote region sur-
rounding the star Bond 734, all the lines were of course faint, but
the H ^ line was at least five times brighter than even the chief
nebular line, while the second line was quite invisible.
These observations of Professor Campbell (which have been
confirmed by various members of the Lick Observatory staff, and
by the eminent spectrocopist, Professor Runge of Hanover, Ger-
manvi while on a visit to Mt. Hamilton) were regarded by him
as indicating a real difference in the distribution of the materials
of which the nebula is composed. The substance, whatever it
may be, which gives the principal lines in the green, is more
strongly concentrated in the central regions of the nebula; in the
faint and remote regions, hydrogen is predominant. In a pre-
vious number of these Publications,^ I have pointed out the fact
that these differences of distribution of the substances in the
nebula (assuming them to be real), must lead to a difference
between the forms of the nebula as shown in drawings and in
photographs.
Professor Scheiner, of the Astrophysical Observatory at Pots-
dam, holds, on the contrary, that the spectrum of the Orion nebula
is the same in all its parts, and attributes the differences observed
by Professor Campbell to physiological causes. By what is
known as the "Purkinje effect," the maximum of brightness in the
spectrum shifts toward the violet end when the intensity of the
light is diminished. If, therefore, we suppose that two lines, one
red and one blue, are equally bright when the intensity of the
illumination has a certain value, the red line will appear brighter
than the blue if the intensity is increased, and the blue line will
appear brighter than the red if the intensity is diminished. The
blue line may even be distinctly seen after the red line has faded
into invisibility.
In Professor Scheiner's opinion, the observations of Professor
Campbell are sufficiently explained by this physiological effect,
as well as the fact that the r^d hydrogen line C or Ha has been
observed in very few nebulae. His views were confirmed by some
photometric observations which he made on the artificial spectrum
of hydrogen.
In connection with these observations, Professor Scheiner,
extending some earlier researches of Koch, made some experi-
ments in which he sought to ascertain the possible influence on
• No. 44.
Astronomical Society of the Pacific. 143
the spectrum of the temperature of the surroundings under ^hich
hydrogen emits light. The hydrogen was enclosed in a vessel
which was cooled down to a temperature of — 200° C. by means
of liquid air, and it was made luminous by extremely feeble elec-
tric waves. The temperature of the hydrogen under these con-
ditions approached the absolute zero — 273° C, but its spectrum
was the same as that observed at ordinary temperatures. Hence,
there seems to be no reason to suppose that the spectrum of
hydrogen in the nebulae is influenced by the cold of surrounding
space.
It will be seen that the apparent shifting of the brightness in
the spectrum, due to the Purkinje effect, is in the right direction
to explain the observations of Professor Campbell on physiolo-
gical grounds, since these observations showed that the more
refrangible line was relatively brighter in the faint regions of the
nebula. In my opinion, however, the Purkinje eff*ect is inade-
quate to explain the amount of the observed variations of bright-
ness. Professor Scheiner*s experiments dealt with an extreme
case. The lines compared (Ha and H/3) were widely separated,
and the physiological effect was strongly marked. But in Pro-
fessor Campbell's observations, verified by Professor Runge,
the lines compared were in nearly the same spectral region, so
that the physiological effect must have been very much smaller;
yet the variation of the relative brightness of the lines was from
twenty to thirty-fold. It is difficult to avoid the conclusion that
we are here dealing with actual diff*erences in the radiation from
different regions of the nebula.
When the Orion nebula again comes into position for observa-
tion with the great telescope, it will be easy to make an experiment
in which physiological effects are wholly eliminated. With the
spectroscope slit placed on the bright region near the trapezium,
the intensity of the light can be diminished (say by reducing the
vertical aperture of the spectroscope) until the second nebular
line ( X 4959 ) is barely visible, or about as bright as it is with full
aperture in some remote region of the nebula. Under these
circumstances, any considerable differences in the relative bright-
ness of the H /3 line could not be ascribed to physiological causes.
Photography could perhaps be made to furnish a still more satis-
factory test
I am further not quite convinced that the invisibility of the Ha
line in the spectrum of the great majority of nebulae is entirely
144 Publications of the
due to the Purkinje effect. It is easy enough to reduce the
visible hydrogen spectrum, derived from spectrum tubes, to the
single line Hj3, by merely diminishing its brightness; but to my
eye, at least, Hy always disappears before Ha. In the nebulae,
on the other hand, Hy is seen without difficulty, while Ha b gen-
erally invisible. In some stars we find hydrogen exhibiting cer-
tain spectral peculiarities which have not yet been produced art-
ificially, and certainly there is nothing absurd in the supposidon
that hydrogen in the nebulae can have a spectrum which differs
in some respects from that obtained in our laboratories. The
difference, if it is real, as I believe it to be, may be a key which
will finally unlock some of the many mysteries by which the
nature and constitution of the nebulae are still surrounded.
WOLFS PERIODICAL COMET.
By W. J. HussEY.
On the night of June i6th, I turned the 36-inch refractor to the
place given by Thraen's ephemeris of Wolf's periodical
comet {Astro7iomische Nachrichten^ No. 3484), and at once found
it at less than its own diameter from its predicted place. My ob-
servation at the time of rediscovery gives the following position,
which is already corrected for parallax and aberration: —
Greenwich M. T. True a True 5
1898 June 16.95449 2^ 16" i8'.68 4*19° 42' 46".3
For the same epoch, the position which I have obtained by com-
putation from Thraen's elements of the orbit is only i'.3i
larger in right ascension and only i".i smaller in declination.
These residuals are remarkably small, and show that Thraen
has reached most excellent results in his determination of the de-
finitive elements of the orbit.
This comet was first seen as a nebulous body by Max Wolf
at Heidelberg, September 17, 1884, 21^^ i^ cometary nature was
fully established by him on September i8th and 19th. He then
notified the Strassburg Observatory of his discovery, and the first
accurate position of the comet was obtained there on September
2oth. On September 2 2d the comet was discovered indei>end-
endy at the Dun Echt Observatory by Ralph Cope land, who
detected it *'as a gaseous body with the spectroscope." The
Astronomical Society of the Pacific. i45
telegram announcing the discovery by Wolf was not delivered
at the Dun Echt Observatory until the morning of September 23d.
It is of interest to note that the first observation of the comet in
this country was that obtained at Washington by Commander
(now Acting Rear-Admiral) Wm. T. Sampson, of the U. S. Navy,
who was then in charge of the 9.6-inch telescope of the Naval Ob-
servatory.
At the first apparition the various observers described the
comet as a bright nebulous body, about 2' in diameter, having a
strong central condensation, almost stellar in appearaqce, and
equal in brightness to a star of from the 8th to nth magnitude.
It had scarcely a trace of a tail; many observers did not note any
at all, but described the comet as being very nearly round.
Spectroscopic observations were made at Nice and Rome. The
observations at Nice, towards the end of September, showed a
bright continuous spectrum crossed by the ihree usual carbon
bands. At Rome apparently only the middle (and brightest) ol
these bands was seen.
The comet had been under observation only a short time, when
it was found that the observed places could not be satisfactorily
represented on the supposition of parabolic motion. Elliptic
element? were accordingly computed by Krueger, Chandler,
Wendell, Zelbr and Thraen. Their results showed the
comet to be one of short period, requiring about 6^ years to
complete a revolution about the sun. It was also noticed that
the comet had been so nt^x Jupiter from March to August, 1875,
as to experience very marked perturbations. Lehmann-Filhes
undertook the investigation of the changes in the elements result-
ing fi-om these perturbations. Basing his work on Krueger' s
elements, which were admittedly only approximately true, he
found that the axis of the orbit had been turned through an angle
of nearly 27°, that the inclination had been diminished more than
2°, the eccentricity had been doubled and the periodic time
shortened over two years. Moreover, the perihelion distance had
been changed from about 309,000,000 to 146,000,000 miles,
showing that prior to 1875, the comet had at all times been so dis-
tant from the earth as to be either invisible or at least be so faint
as to be readily overlooked, thus accounting for its not having
been discovered before that time.
These circumstances gave the comet a wide interest among
astronomers. It was observed a long time at many observatories.
146 Publications of the
During the first apparition no less than 950 observations were se-
cured at some fifty-four different observatories, from September
20, 1884, to April 6, 1885. During these six and one-half
months the comet described 106 degrees of its heliocentric arc,
35° before and 71° after perihelion passage. Numerous observa-
tions were obtained toward the close of the apparition, thus
strengthening greatly that part of the arc and giving the final ele-
ments greater security. The definitive elements were computed
by Thraen, and both he and L» Struve computed the pertur-
bations between the first and second apparitions, and provided
ephemerides by means of which Spitaler rediscovered the
comet, May i, 1891.
At the second apparition the comet again remained visible
for a long time, until March 31, 1892, and no less than 681 obser-
vations at thirty-three different observatories were obtained.
Thraen again computed the definitive elements, making use of
the data of both the first and second apparitions and taking into
account the perturbations of the Earth, Mars, Jupiter ^vi^ ScUurtu
The elements which he finally obtained, when referred to the
ecliptic and the mean equinox of 1898.0, are as follows:^—
Epoch and Osculation 1898 August 22.0 Berlin M. T.
M = 6° 58' ii".03^
;:>= 172 52 35.77 Ecliptic and
O = 206 27 22 .26 J- -- T- • r « o
' /= 25 12 16 .59 I MeanEqumoxof 1898.0
<A= 33 44 2 .15J
\^ = 518"- 36764
log a = 0.5569125
The accuracy of these elements is very great, as is shown by
the close agreement of the computed and observed places of the
comet at the time of its rediscovery this year, and they reflect
great credit upoil th^ir author.
Mt. Hamilton, July II, 1898.
COMET c, 1898 (CODDINGTON).
By E. F. Coddington.
On the evening of June 9th, I made an exposure of two hours
with the Crocker photographic telescope, for the purpose of
obtaining a photograph of the extensive nebulous region to the
i'OJLICLIjRAKyI
ASTOR, LENOX AND
TILDEN POUNDATrON/.Q
Astronomical Society of the Pacific, i47
north of Antares in the constellation Scorpio, At the time
changes were being made in my darkroom, and it was not until
June nth that I had an opportunity to develop the plate. When
the plate was developed a strong trail, about one-sixteenth inch
in length, was found upon it, some two or three degrees north-
east of Antares, The length and direction of the trail indicated
the possible positions in which the object might be found, and on
turning the 12-inch telescope to the proper region the comet was
picked up immediately, and observed for position by Professor
HUSSEY.
At the time of discovery, the comet had a bright nucleus of
about the 8th magnitude, surrounded by a nebulosity somewhat
less than a minute of arc in diameter. The nucleus was very
nearly stellar, and when examined with the 36-inch refractor,
using a power of 1000, it presented a uniform appearance.
There was a slight indication of a tail on one side of the nebu-
losity, but the comet was so near opposition that whatever tail it
may have had, extended almost directly away from the comet in
the line of sight. When discovered the comet was near Antares
and since then it has been moving steadily towards the south-
west, a little more than a degree per day. It is already too far
south to be observed at most northern observatories. By the
middle of August it will have reached a southern declination of
50 degrees and will then be in the constellation Ceniaurus, It
will remain visible for some time to the observatories of the
southern hemisphere.
This is the third comet which has been discovered by pho-
tography. On October 12, 1892, Professor Barnard found the
trail of a hitherto unknown comet upon a photograph of the
Milky Way, which he had just obtained with the Crocker tele-
scope.
Professor Schaeberle was the next to discover a comet by
means of photography. He found the image of some strange
object on some of his eclipse negatives taken at Mina Bronces,
Chile, in 1893, and verified its cometary nature by means of the
plates taken by other eclipse parties. This comet was never ob-
served visually, and its orbit is unknown.
The accompanying half-tone shows the trail of the comet and
ako gives a fair representation of a very remarkable region of the
sky. At the lower central part of the reproduction is the bright
star Antares with the cluster. Messier 4, just to the right. Just
^48 Publications of the
above we find an area which stands out in a marked contrast to
the surrounding region, by being almost void of faint stars. In-
stead we find a large nebula with its principal condensations
surrounding the few bright stars that are situated here. A great
deal of delicate detail can be traced on the original negative and
the vacant lanes running eastward from this region are prominent
features. The comet was crossing one of these lanes at the time
of exposure. And it may be found on the accompanying illus-
tration near the left margin. I hope to secure a better negative
of this region. This one is reproduced on account of the comet
trail.
Using the following observations: —
Mt. Ham. M. T. app a app I Observer
June II, 9** 13" 7' 16*" 24" 56'.2i — 25^ 14' 2o".o Hussey
13, 10 47 36 16 17 58.38 — 26 33 3 .3 Tucker
15, 8 43 30 16 II 23.71 —27 45 12 .7 Hussey
Professor Hussey and I computed the following preliminary
elements: —
T = 1898 Sept 10.3054 Gr. M. T.
0) = 229° 28' II" ^ ^ ,. .
0= 73 59 51 Ecliptic and
i Mean Equinox of 1898.0
2 = 71 17 49 ) ^ ^
log q = 0.24760
(O— C): AX' cos i3' = + 4", A^' = + 2"
From Mt. Hamilton observations of June nth, i8th and 26th,
I have computed the following elements of this comet. The mean
of three observations was used in forming the middle place, and
the mean of two observations for the last place.
T = 1898 Sept. 13.97347 Gr. M. T.
CO = 233^ 10' 3i".4 ) T, r .. .
«= 73 59 19 .8 5 Ecliptic and
i = 69 56 47 .3 ( ^^^^ Equinox of 1898.0
log q = 0.231178
(O— C): AX' cos i3' = -f 4".7, A^S' = + i".8
Mt. Hamilton, July 11, 1898.
Astronomical Society of the Pacific, i49
PLANETARY PHENOMENA FOR SEPTEMBER AND
OCTOBER, 1898.
By Professor Malcolm McNeill.
September.
The Sun crosses the equator and autumn begins September,
22d, 4 P.M., P. S. T.
Mercury passes inferior conjunction on September 5th, and
moves rapidly out toward greatest western elongation, which it
reaches on September 21st. It may be seen as a morning star in
the eastern twilight during the latter half of the month.
Venus is still an evening star and comes to greatest elongation
on September 22d. Throughout the month it sets less than two
hours after sunset. When a greatest eastern elongation occurs in
the spring, the planet remains above the horizon more than
twice as long after sunset The reason for the difference is, that
for an eastern elongation in the spring, the planet is far north of
the Sun, and in the autumn it is far south, nineteen degrees on
September 30th.
Mars is getting into more convenient position for observation,
rising before midnight on September ist, and nearly an hour
earlier at the close of the month. It moves nineteen degrees
eastward during the month through the constellation Gemini,
and at the close of the month is only one degree from the third
magnitude star 8 Geminorum, The Moon makes a very close
approach to Mars on the morning of September 9th, but will
hardly occult it in this country, except possibly in the extreme
southwestern portions. The planet is beginning to grow more
conspicuous, and its distance from the Earth diminishes from
137,000,000 miles to 120,000,000 during the month.
Jupiter is still an evening star, but its distance from the Sun is
rapidly diminishing, and it will scarcely be possible to see it
with the naked eye after the first half of the month. It moves
eastward and southward about seven degrees during the month,
and is in the western part of the constellation Virgo, not far from
Spica, the brightest star of the constellation.
Saturn is also an evening star and sets at 8:36 p.m., September
30th. It is in the constellation Scorpio, about seven degrees
I50 Publications of the
to the north of the first magnitude red star Antares, and moves
about two degrees eastward and southward during the month.
Uranus precedes Saturn^ setting about half an hour earlier.
It is not bright enough to be easily seen at the low altitude it
reaches before the disappearance of the evening twilight.
Neptune is on the border on the constellations Taurus and
Gemini, and rises before lo p.m at the end of the month.
October.
Mercury remains a morning star until October 19th, when it
passes superior conjunction and becomes an evening star. It
may be seen in the early twilight for a few days after the begin-
ning of the month, but it soon reaches a point too near the Sun
for naked-eye observation.
Venus is an evening star. It is at its greatest possible southern
latitude as seen from the Sun on October 9th, and this, combined
with its position in regard to the ecliptic as seen from the Earth,
gives it its nearly maximum southern declination. At the end of
the month, it sets only an hour and a half after sunset. During
October and November it will be very bright, the time of greatest
brilliancy being about the end of October. For several weeks
before and after that time, it will be bright enough to be seen in
full dayligl^t with the naked eye, if the low altitude of the planet
due to its great southern declination does not interfere too much.
JkTars rises about an hour earlier tlfan during September, at a
little after 10 p.m. on October 31st. It is in quadrature with the
Sun on October 1 7th. It moves about fifteen degrees eastward and
two degrees southward during the month through the constella-
tion Gemini into Cancer, At the end of the month it will have
diminished its distance from the Eaxth to less than 100,000,000
miles, and its brightness will increase about forty per cent during
the month.
Jupiter begins the month as an evening star, too near the
Sun to be seen without a telescope, and passes conjunction on
October 13th. Toward the close of the month, it rises more than
an hour before sunrise, the interval between the rising of the
planet and Sun increasing quite rapidly, owing to the rapid
motion of the Sun eastward and southward.
Saturn is still an evening star, but is not in very good position
for observation, owing to its nearness to the Sun and its low
altitude after sunset. At the end of the month, it sets less than
two hours after the Sun.
Astronomical Society of the Pacific,
151
Uranus is also an evening star, but as it sets half an hour
earlier than Saturn, and is so faint, it can scarcely be seen with-
out a telescope.
Neptune rbes two hours earlier than in September, and is on
the border of the constellations Taurus and Gemini,
Phases of the Moon. P.
Last Quarter,
New Moon,
First Quarter,
Full Moon,
Last Quarter,
New Moon,
First Quarter,
Full Moon,
Sept.
7»
2
Sept.
15,
4
Sept.
22,
6
Sept.
29»
3
Oct.
7»
10
Oct.
I5»
4
Oct.
22,
I
Oct.
29»
4
S. T.
M.
51 P. M.
10 P. M.
39 P- Mf
10 P. M
5 A. M
37 A. M
9 A. M
18 A. M
Asrc,<. Lr^'ox AND
TluObN P- 'JNOATIONS. j
The Sun.
1898.
Sept I.
II.
21.
Oct. I.
II.
21.
31.
R. A.
H. M.
10 43
11 19
11 55
12 31
13 7
13 44
14 23
Declination.
+
+
+
8 II
4 27
o 36
- 3 18
- 7 8
— 10 49
— 14 13
Rises.
Transits.
32 A. M. 12 O M.
41
51
I
II
22
33
II 56 A.M.
II 53
II 50
II 47
II 45
II 44
Sets.
28 P. M.
II
55
39
23
8
55
Mercury.
Sept I.
ll
6
+
I
4
6 20 A.M.
12
23 P.M.
6 26P.M
II.
10
37
+
6
31
4 53
II
15 A.M.
5 37
21.
lO
50
+
8
20
4 20
10
48
5 16
Oct. 1.
II
44
+
3
49
4 51
II
3
5 15
n.
12
48
—
3
28
5 38
II
27
5 16
21.
13
50
—
10
44
6 27
II
50
5 13
31-
14
51
17
2
7 "
Venus.
12
12 P.M.
5 13
Sept. I.
13
28
—
10
45
9 22 A.M.
2
45 PM.
8 8P.M
II.
14
7
—
15
18
9 38
2
45
7 52
21.
14
46
—
19
21
9 53
2
45
7 37
Oct. I.
15
24
—
22
45
10 5
2
43
7 21
II.
15
59
—
25
21
10 13
2
39
7 5
21.
16
30
—
27
6
10 11
2
30
6 49
Si-
16
53
—
27
55
9 59
2
13
6 27
152 Publications of the
Mars,
Sept I. 5 56 + 23 28 II 49 P.M. 7 14 A.M. 2 39P.M.
Oct.
II.
6 23
+ 23 33
II 35
7 I
2 27
21.
6 48
+ 23 24
II 21
6 46
2 II
7 II
+ 23 4
II 8
631
I 54
II.
7 33
+ 22 36
10 52
6 13
I 34
21.
7 53
-H 22 4
10 35
5 54
I 13
31. 8 II +21 31 10 15 5 32 12 49
Jupiter,
Sept. I.
Oct. I.
31.
12 45
13 8
13 32
— 3 35 8 14 A.M.
— 6 2 6 47
— 8 28 5 22
Saturn.
2
12
10
2 P.M.
27
53 A.M.
7
6
4
50 P.M.
7
24
Sept. I.
Oct. I.
31.
16 18
16 25
16 37
— 19 43 12 46 P.M.
— 20 7 10 55 A.M.
— 20 37 9 10
Uranus,
5
3
I
34 P.M.
44
57
10
8
6
22 P. M
33
44
Sept. I.
Oct. I.
31.
15 50
15 54
16 I
— 19 58 12 18 P.M.
— 20 II 10 25 A.M.
— 20 30 8 34
Neptune
5
3
I
7 P.M.
13
21
9
8
6
56 P. M
I
8
Sept. I.
Oct. I.
31.
5 37
5 38
5 36
+ 22 2 II 35P.M.
+ 22 I 9 39
4- 22 7 39
6
4
2
54 A.M.
58
58
2
12
10
13P.M
17
17 A.M
Astronomical Society of the Pacific. i53
NOTICES FROM THE LICK OBSERVATORY.*
Prepared bv Members of the Staff.
r
I ( :
TILOcN p;
The November Meteors.
Harvard College Observalory Circular No, 31,
On the night of November 13, 1897, 91 meteors were ob-
served at the Harvard College Observatory, and 47 meteors at
an auxiliary station 12 miles south, the Blue Hill Meteorological
Observatory. A discussion of these observations by Professor
W. H. Pickering will be found in the Annals of this Observa-
tory, Volume XLI, No. 5. A much greater display of meteors
is expected next year, and it is very important that a continuous
watch should be kept during the two or three days in which the
Earth is passing through the denser portion of the meteor
stream. This can only be done by establishing a series of sta-
tions in various longitudes, so that during the entire time one or
more of these stations shall fulfill the conditions that the radiant
point shall be above the horizon and the Sun below. Corre-
spondence is invited with astronomers and others willing to partici-
pate in this work, especially with those who will be in the less
frequented longitudes. If the weather is favorable, and the plan
here proposed is carried out satisfactorily, it is expected that all
the observations will be discussed here and published in the
Annals of this Observatory. To secure the best results, a uniform
plan of work is essential. Maps and forms of record will be
sent to all who early signify their readiness to take part in this
work. The radiant point of the meteors indicated by the cross
in the accompanying map [here omitted], will not rise in this
latitude until lo** 30", and twilight interferes at about 5' 30° in the
morning. As the shower sometimes begins before the predicted
jnoations
* Lick Astronomical Department of the University of California.
154 Publications of the
date, a watch should be kept on November ii and 12, from 11
to I o'clock, and if many meteors are seen, the observations
described below, for November 13, should be made on these
nights, and also on the nights following the shower.
Each observer is requested to devote his attention to the
region within 25° of the radiant point, and included in the map,
and to send the following data regarding his observations : —
Name of observer, location of station, post-office address, time
of beginning and ending of observations, interruptions by clouds
or other causes, condition of sky, as clear, hazy, passing clouds,
etc.
The observations most desired are those required to determine
the frequency of the meteors. They are of extreme simplicity,
and need only care, system, and perseverance. Once an hour,
or, better, once every half-hour, observe and record the time
during which ten meteors appear. This is most easily done by
noting the time by a watch and at exactly the beginning of a
minute looking at the sky, giving it undivided attention and
counting the meteors seen, not including those appearing outside
the region covered by the map. If great numbers of meteors
appear, it may be better to count a larger number, as twenty or
even fifty. If the interval between the meteors is long, the
number to be counted may be reduced. These observations
should be repeated until dawn, or over as long an interval as
possible. Between these observations, the observer may rest, or
may make special observations of individual meteors. Thus,
when a meteor is seen, record the hour and minute, the bright-
ness on a scale of stellar magnitudes, —2, equals the brightness
o{ Jupiter, or Sinus; o, Arcturus, or Fe£^a; 2, the PoU-Star; 4,
the Pleiades; 6, the faintest star visible; the color, B=blue,
G=green, Y = yellow, W = white, and R = red; the class.
h=^Leonid, if path prolonged would pass through center of
map, N = other meteors. Thus, L 5 Y, 12' 26°, indicates that
a Leonid, magnitude 5, yellow in color, was seen at 12** 26".
Find by trial beforehand how many seconds are required to
make each record. Again, the path of each meteor may be
marked upon the map by noting its position in relation to the
adjacent stars. Such work can be done equally well elsewhere,
and should not interfere with the hourly count mentioned above.
Edward C. Pickering.
May 30, 1898.
Astronomical Society of the Pacific, 155
Discovery of Comet e 1898 (Perrine).
This comet was discovered in the morning of June 15th, in the
constellation Camelopardalis, At 23^ 22'° 34' G. M. T. of June
14th, the comet's position was a= 3** 29°* o'.99, 8= + 58° 35'
22. "3. It was then moving^ slowly south and more rapidly
east. The elements as computed from the first three observations
will be found elsewhere in this number of the Publications. These
elements bear considerable resemblance to those of the comet
1785 I, especially with regard to o) and i, the resemblance being
closer than was the case with the comet b 1898, pointed out in
No. 62 of these Publications. Comet e 1898 appears to be another
member of this same family.
At the time of discovery the comet was not so bright as Comet
b, its brightness being estimated at about 10 or a little fainter.
It has been steadily increasing in brightness and is now estimated
to be 9 or 9)4 magnitude, brighter than Comet b, A rather
sharp nCicleus has developed within the past week and is now
estimated to be about 13th magnitude.
Comet e has been moving in the same general direction as
Comet b, and as its geocentric motion has been much more rapid
it has overtaken the latter and passed it in both co-ordinates.
On the morning of June 27th, the two comets were within about
one- quarter degree of each other, both visible in the lowest
power field of the 1 2-inch telescope.
Comet e is moving rapidly south and east, and hence its loca-
tion is becoming more unfavorable for observation. Towards
the middle of August it will pass the Sun going south, after which
it will soon be lost to northern observers. Owing to the resem-
blance already pointed out, it seems important to observe it as
long as possible. C. D. Perrine.
Mt. Hamilton, Gal, 1898, June 29.
Errata in Star Catalogues.
LcUande 31379. The declination of this star appears to be in
error by i'. A micrometer comparison with Radcliffcj; 4514
on June 2d indicates that the N. P. D. of Lalande 31379 should
be 100° 25' 39". 8.
Weisse*s Bessel XVIII, 1327 appears to be in error in dec-
lination by 2'. A micrometer comparison with 1323 on June 2d
shows that the declination of 1327 should be —13° 44' io".5.
C D. Perrine.
Mt. Hamilton, Gal., June 7, 1898.
156 Publications of the
Two Bright Meteors, June 24 and June 29, 1898.
On the morning of June 24, at i** ly" 53" P. S. T., a very
brilliant meteor was seen to pass southeast through the constel-
lations Cassiopeia and Perseus^ bursting a little southwest of the
star y Fersei. This meteor was a brilliant bluish-white, and
fully ten times as bright as Venus at the present time.
At 8** 16* 26" P. S. T., in the evening of June 29th, while it
was yet very bright twilight, an unusually large meteor was seen
in the southwest. When first seen it was at an altitude of about
20° above the horizon. It passed slowly toward the west, mak-
ing a small angle with the horizontal, disappearing almost due
west and but litde above the horizon. A few seconds after it was
first noticed several fragments were thrown off— the main body
being diminished but litde in brightness, however, and continu-
ing in the same course.
It was of the usual brilliant bluish- white type, and fully twenty
to thirty times as bright as Venus, which was visible in the north-
west. The meteor was seen for eight seconds — the time given
being that of disappearance. C. D. Perrine.
Mt. Hamilton, Cal, 1898, June 30.
Comet c 1898 (Coddington).
A letter, dated June 16, 1898, received from Harvard College
Observatory, states that photographs of Comet Coddington
were obtained at the Harvard College Observatory by Mr. King
on June 14 and 15, 1898. A measurement by Mr. Wendell
of the light of the nucleus of this comet showed that its intrinsic
brightness was equal to that of a star of magnitude 7.7 when
spread over a circle one minute of arc in diameter.
The following letter, dated June 18, 1898, has also been
received: "A telegram has been received at Harvard College
Observatory from Professor Kreutz. at Kiel Observatory, stating
that the following elements and ephemeris* of Comet c 1898
were computed by Berberich:—
T = 1898, August 4.44 G. M. T.
0) = 206° 09'
"= 73 59
/= 76 48
q = 2.0821 ''
•The ephemera is here omitted.
Astronomical Society of the Pacific. 157
Elements of Comet e 1898 (Perrine).
From the Mt. Hamilton observations of June 14, 15 and 16,
we have computed the following elements of Cometh, 1898: —
T = 1898, August 17.400.
0, = 196° 45' 48" \ ^y . A
^ , f Ecliptic and
( Mean Equinox of 1898.0
2 = 69 42 23 ;
log q = 9.87026
Residuals for the middle place. (O— C):
A A = + 2", A i8 = - 5".
C. D. Perrine and R. G. Aitken.
Elements of Comet 1898 g (Giacobini).
This comet was discovered by Mr. Giacobini, of the Nice
Observatory, June i8th. From the Nice observation of June
19th, and my observations of June 23d and 27th, I have com-
puted the following elements of the orbit: —
T = 1898 July 25.84828 G. M. T.
co= 220 41' 26". 5 I Ecliptic and
O — 278 17 30 .3 V j^^^ Equinox of 1898.0
i = 166 50 58 . 1 ;
log^ = 0.175956
(O-C): AA' cos r = - i".8; A^S' = + 2".i
The comet is telescopic. When discovered it had a stellar
nucleus of about the 9th magnitude and scarcely a trace of a tail.
It was then near opposition, and consequently its tail was very
unfavorably situated for observation. The comet has been dimin-
bhing in brightness; it has also been moving rapidly westward,
and by the end of the present month it will be reaching a position
unfavorable for observation.
On the evening of July 14th, I examined the comet with the
36-inch refractor and found the nucleus small, stellar in appear-
ance, and not brighter than a star of the nth magnitude. The
coma was some 30" or 40" in diameter and a well-developed tail,
some 5' or 6' in length, was visible. The tail was narrow, toler-
ably bright near the nucleus, but becoming rapidly fainter as the
distance from the nucleus increased. W. J. Hussey.
July 18, 1898.
15^ Publications of the
Elements of Comet e 1898 (Perrine).
From my observations of this comet on June 17th and 24th
and July ist, I have computed the following system of parabolic
elements: —
T= 1898, August 16.23874 G. M. T.
0) = 205° 12' l8".2) -. ,. . , ..
^ , f Ecliptic and Mean
^ = 259 10 16 .4 > -, r r ^ o
^ I Equinox of 1898.0
f = 70 o 10 .8 ; ^ ^
log q = 9.800186
Residuals for the middle place are —
O— C: AA' cos /3' = — 2".5; ^^ cos p' = -f 4".o
These elements do not differ materially from the first set
obtained. The comet has grown much brighter, has increased
in size, and now has a short brush of a tail, extending away from
the Sun. A nucleus has developed, and is at present fully as
bright as a tenth-magnitude star. The entire comet is about
equal in brightness to an eighth-magnitude star.
Its rapid motion south and east will soon cause it to be lost in
the Sun's rays. It should become visible to observers in the
southern hemisphere towards the end of August, and should be
even brighter then than now. C. D. Perrine,
Mt. Hamilton, California, July 26, 1898.
Fellowships at the Lick Observatory.
Messrs. Russell T. Crawford, Frank E. Ross, and
Harold K. Palmer, all graduates of the University of Cali-
fornia, have been appointed to Fellowships in Astronomy at the
Lick Observatory for one year, beginning on the ist of August,
1898. Mr. E. F. CoDDiNGTON has also been reappointed Fellow
in Astronomy.
The Large Refractors of the World.
The following list of large telescopes has been taken from the
list published in The Odsefvatory for June, 1898, which includes
all refractors having aperture of 13.4 inches or over. One or
two corrections have been made in the third column.
The fourth column gives the name of the maker of the object-
glass; when it is known that the mounting was made by a second
firm, a number is affixed, signifying respectively: (i) Warner
& SwASEV; (2) Gautier; (3) Repsold; (4) Ransome and
SiMMs; (5) Saegmuller.
Astronomical Society of the Pacific,
159
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i6o Publications of the
Astronomical Telegrams {Translation),
Lick Observatory, June 12, 1898.
To Harvard College Observatory: ) /^c .
To Students* Observatory, Berkeley: J ^ • • v
A bright comet was discovered by E. F. Coddington by
photography. It was observed by W. J. HussEV, June 11.7220
G. M. T.; R. A. i6*» 24- ^s'.g; Decl. — 25° 14' 20".
The daily motion of the comet is + 51' in R. A. and — 36'
in Decl.
Lick Observatory, June 13, 1898.
To Harvard College Observatory: ) ^h _» . „ >.
To Students' Observatory, Berkeley: ) '^^'^^^ ^ 55 a.m.;
Comet c 1898 (Coddington) was observed by E. F. Cod-
dington, June 12.7288 G. M. T.; R. A. iC* 21" 34". i; DecL
- 25° 52' 43".
Lick Observatory, June 14, 1898.
To Harvard College Observatory: ) ^^ . ^n « x
To Students' Observatory, Berkeley: ) ^^^"^ ^ ^^ ^' ^'^
Comet c 1898 (Coddington) was observed by E. F. Cod-
dington, June 13.7583 G. M. T.; R. A. 16*^ i8- sVo; Decl.
-26° 31' 48".
Boston, Mass., June 14, 1898.
To Lick Observatory: (Received i* lo" P. M.)
Encke's periodic comet has been observed on its return by
Tebbutt, at Windsor. Its position on June 11.8435 G. M. T.
was R. A. 6** 53™ 29'.o; Decl. + 11° 34' 00".
(Signed) John Ritchie, Jr.
Lick Observatory, June 15, 1898.
To Harvard College Observatory: ) (gent 3*^ 25- P. M.)
To Students' Observatory, Berkeley:) ^ ^ ^
Comet c 1898 (Coddington) was observed by R. H. Tucker
with the Meridian Circle, June 13.7876 G. M. T.; R. A. 16*^ 17"
58V4; Decl. - 26° 33' 3".
Lick Observatory, June 15, 1898.
To Harvard College Observatory: \ ^^, ^
To Students Observatory, Berkeley:)
A faint comet was discovered by C. D. Perrine on June
14.974 G. M. T. in R. A. 3*' 29-; Decl. + 58° 36'. Its daily
motion is -h 1° 34' in R. A. and + 12' in Decl.
Astronomical Society of the Pacific. i6i
Lick Observatory, June i6, 1898.
To Harvard College Observatory: | ,q h m \
To Students* Observatory, Berkeley:) • •/
Comet e 1898 (Perrine) was observed by C. D. Perrine,
June 14.9740 G. M. T.; R. A. 3^ 29- iVo; Decl. + 58° 35' 25";
and June 15.9296 G. M. T.; R. A. 3^ 34" sy'.y; Decl. 58°
24' 2".
Lick Observatory, June 17, 1898.
To Harvard College Observatory: ) ^q h ■
To Students' Observatory, Berkeley:) '^^^''^ '^ "^^ ^'^'^
Comet e 1898 was observed by C. D. Perrine, June 16.9376
G. M. T.; R. A. 3** 41"* ii'.9; Decl. + 58° 10' 49".
Lick Observatory, June 17, 1898.
To Harvard College Observatory: (Sent lo*" 40"* a. m.)
Wolf's periodic comet has been observed on its return by
W.J. HussEY,June 16.9666 G. M. T.; R. A. 2>» i6°» i8'.9; Decl.
+ 19^ 42' 44".
Lick Observatory, June 17, 1898.
To Harvard College Observatory: (Sent 3* 35" p. M.)
Elements and ephemeris* of Comet e 1898 (Perrine) were
computed by C. D. Perrine andR . G. Aitken as follows :
T = 1898, August 17.400 G. M. T.
0, = 196° 46' ) T7 r .• ^
^ , ^ f Ecliptic and
O = 260 06 > . . T- . r « «
i Mean Equinox of 1898.0
t= 69 42 )
q =z 0.7418
Lick Observatory, June 18, 1898.
To Har\'ard College Observatory: (Sent 10:20 a.m.)
Elements and ephemerisf of Comet r, 1898 (Coddington)
were computed by W. J. Hussey and E. F. Coddington as
follows: —
T = 1898, September 10:31 G. M. T.
"^ r Ecliptic and
73 59 / Mean Equinox of 1898.0
z= 71 18 )
g= 1.7685
* The ephemeris is here omitted,
t The ephemeris is here omitted.
i62 Publications of the
Boston, Mass., June 21, 1898.
To Lick Observatory: (Received 4:30 P. m.)
Comet g 1898 (GiACOBiNi) was observed at Nice. June
19.5079 G. M. T.; R. A. 20*^ 26- 40-.8; Decl. —21° 27' 6".
The daily motion is — 2° 52' in R. A. and — 20' in Decl.
(Signed) John Ritchie, Jr.
Boston, Mass., June 27, 1898.
To Lick Observatory: (Received 9.00 p. M.)
Elements and ephemeris* of Cornet^ 1898 (Giacobini) were
computed by Professor Kreutz as follows: —
T= 1898, July 6.23 G. M. T.
0,= 7° 36' \
0=278 31 \ Ecliptic and
. ^ i Mean Equinox of 1898.0
q= 1.5864
This is a rough approximation.
(Signed) John Ritchie, Jr.
Independent Discovery of Comet c 1898.
From a note in the Astranomiscke Nachrichien, No. 3500, it
appears that Comet c 1898 (Coddington), discovered at the
Lick Observatory on June nth, was discovered independently
in Bukarest, on June 14th, by Mr. W. Pauly. Qouds inter-
fered before he was certain of the cometary nature of the object;
and it was not until June i6th that he telegraphed his discovery
to the Central Stelle, at Kiel. As Mr. Pauly does not receive
the astronomical telegrams distributed from Kiel, he was not
aware that his discovery had been anticipated, though the comet
was observed at various European observatories on June 13th
and 14th.
Conference of Astronomers and Physicists.
The conference of astronomers and physicists held at the
dedication of the Yerkes Observatory in October, 1897, ^^^ so
successful that it has been decided to hold a second meeting this
year, the meeting- place to be the Harvard College Observatory.
The days of meeting are Thursday, Friday, and Saturday,
August 1 8th, 19th, and 20th, 1898. These days were selected
in order that vbiting astronomers might attend the meeting of
* The ephemeris it here omitted.
Astronomical Society of the Pacific. 163
the American Association for the Advancement of Science which
will be held in Boston during the week beginning Monday,
August 22d.
According to Professor E. C. Pickering's circular letter, it
is expected that numerous short papers will be presented infor-
mally, illustrated, when desired, by lantern slides, and fully
discussed. The work of the various departments of the Harvard
College Observatory will be shown, and excursions will be
planned to various neighboring scientific institutions.
Obituary Notice.*
William Augustus Rogers, Professor of Physics and As-
tronomy in Colby University, Waterville, Maine, died at that
place on March i, 1898, after an illness of several weeks, brought
on by a severe fall.
He was bom at Waterford, Connecticut, on November 13,
1832. and graduated at Brown University in 1857. Soon after-
wards he became Professor of Mathematics and Astronomy at
Alfred University, in the State of New York. During his tenure
of this office, he passed some time at the Observatory of Harvard
College, and took part in its work under the direction of Pro-
fessor Bond ; and he was subsequently engaged for fourteen
months in the naval service of the United States during the
Civil War, which broke out in 1861. In 1870, after much suc-
cess at Alfred University, both as a teacher and as an investigator,
he returned to Harvard College Observatory, under the direction
of Professor Winlock, and was soon placed in exclusive charge
of the new meridian circle mounted in that year. With this in-
strument he undertook the observation of the zone from 49° 50'
to 55° 10' north declination, as a part of the general revision of
the Durchmusterungy proposed by the Astronomische Gesellschaft.
The results of this work ai^e published in Vols. XV, XVI, XXV,
XXXV and XXXVI of the Annals of the Astronomical Obser-
vatory of Harvard College. Volumes X and XII of the same
series contain the results of observations made in connection with
the zone observations upon a selected list of stars in various
declinations. Professor Rogers also made a series of observations
for determining the absolute positions of certain stars, the re-
duction of which he did not live to complete; but it is hoped that
it can be finished in accordance with his intentions.
• From AstrxmomUche Nachrichien^ No. 3499.
1^4 Publications of the
In making transit observations, Professor Rogers preferred to
use double lines etched or ruled upon glass plates instead of
spider lines. The experiments which he undertook in preparing
such plates led him by degrees to elaborate investigations in the
exact measurement of standards of length. He carried on these
researches with great energy and perseverance, at the same time
with his astronomical work, and with unusual success. It would
be impracticable in the present notice to give even a brief account
of this section of his labors, the results of which are, however, well
known and appreciated among physicists.
He was appointed Assbtant Professor of Astronomy at the
Observatory in 1877, and held that office till 1886, when he re-
signed it to accept the professorship at Colby University, where
he spent the remainder of his life in the same active and zealous
devotion to scientific pursuits by which he had always been dis-
tinguished. While continuing to superintend the reduction of
the observations which he had made at Cambridge, he also found
time, not only for teaching, but for the pursuit of many physical
investigations. Among others may be mentioned the study of
the so-called X-rays, in which he engaged with an ardor which
may perhaps have contributed to enfeeble his naturally vigorous
constitution.
Numerous contributions to scientific periodicals and to the
proceedings of the learned societies of which he was a member,
as well as the larger publications already mentioned, remain to
attest his industry and capacity as a man of science, while the
remembrance of his high character and cordial manners will long
be cherished by those who knew him.
Arthur Searle.
Harvard College Observatory, May 6, 1898.
Astronomical Society of the Pacific, 165
OFFICERS OF THE SOCIETY.
Mr. R. G. AiTKKN President
Mr. C. B. Hill First Vice-President
Miss R. O'Halloran . Second Vice-President
Mr. F. H. Sbarrs Third Vice-Presidtnt
Mr. C. D. Pbrrine ; c ^ •
Mr. F. R. ZiBL t Secretaries
Mr. F. R. ZiBL Treasurer
Boitrd 0/ Directors— ^\^iAx%. Aitkbn, Hill, Kbbler, Molbra, Miss O'Halloran, Messrs.
Pbrrine, Pibrson, Sbarbs, St. John, von Gbldern, Ziel.
Finance Committee — Messrs. Pibrson, von Gblobrn, Hill.
Committee on Publication — Messrs. Aitken, Shares, von Gbldern.
Library Committee— lAcssn, Sbarbs, Geo. C. Edwards, Miss O'Halloran.
Cammittee on the Comet- Medai— Messrs. Keeler (ex-o^cio), Pierson, BtRCKHALTkR.
OFFICERS OF THE CHICAGO SECTION.
Executive Committee — Mr. Ruthven W. Pike.
OFFICERS OF THE MEXICAN SECTION.
Executive Committee^Mr. Francisco Rodriguez Rev.
NOTICE.
The atteniion of new members is called to Article VIII of the By-Laws, which provides that
the annual subscription, paid on election, covers the calendar year only Subsequent annual
payments are due on January ist of each succeeding calendar year. This rule is necessary in
order to make our book>keeping as simple as possible. Dues sent by mail should be directed to
Astronomical Society of the Pacific Siq Market Street, San Francisco.
It is intended that each member of the Society shall receive a copy of each one of the Pub-
licatians for the year in which he was elected to membership and for all subsequent years. If
there have been (unfortunately) any omissions in this matter, it is requested that the Secretaries
he at once notified, iu order that the missing numbers may be supplied. Members are requested
to preserve the copies of the Publications of the Society as sent to them. Once each year a title*
page and contents of the preceding numbers will also be sent to the members, who can then bind
the numbers together into a volume. Complete volumes for past years will also be supplied, to
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books from the Society's library by sending his library card with ten cents in stamps to the
Secretary A. S. P., 819 Market Street, San Francisco, who will return the book and the card.
The Committee on Publication desires to say that the order in which papers are printed in
the Publications is decided simply by convenience. In a general way, those papers are printed
first which are earliest accepted for publication. It is not pos!>ible to send proof sheets of papers
to be printed to authors whose residence is not within the United Stales. The responsibility for
tne views expressed in the papers printed rests with the writers, and is not assumed by the
Society itselt.
The titles of papers for reading should be communicated to either of the Secretaries as early
as possible, as well as any changes in addresses. The Secretary in San Francisco will send to
any member of the Society suitable stationery, stamped with the seal of the Society, at cost price,
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Those members who propose to attend the meetings at Mount Hamilton during the summer
should communicate with "The Secretary Astronomical Society of the Pacific " at the rooms of
the Society, 810 Market Street, San Francisco, in order that arrangements may be made for
transportation, lodging, etc.
PUBLICATIONS ISSUED BIMONTHLW
( February ^ Aprils Jttne, August ^ October^ December.)
PUBLICATION
Astronomical Society of the Pacific
Vol. IX. San Francisco, October i, 1898. No. 64.
THE TEMPERATURE OF THE SUN. I.
By Prof. Dr. J. Scheiner.
[Translated from the German in Himmel und Erde^ by Frbdrrick H. Shares.]
The problem of determining the temperature of the Sun
appears at first glance to be quite insolvable. It is well known
that difficulties, scarcely to be overcome, oppose the attempts
to determine accurate values for the high temperatures occur-
ring in laboratory work and in technology; while for the
highest temperatures which can be produced on the Earth, the
problem has in no way been solved with satisfactory accuracy.
How much greater, therefore, must be the difficulties when we
attempt to determine the temperature of a body separated from
us by nearly 100,000,000 miles, and which in consequence
cannot be handled and manipulated as the burning or glowing
object in the laboratory. In truth, the difficulties confronting
the investigator are great, and so far they have in part proved
insurmountable.
But when have the mere difficulties of a problem prevented
men from attempting a solution? On the contrary, they have
proved an allurement; for the satisfaction incident upon the suc-
cessful solution of a problem increases with the expenditure of
energy necessary to obtain the result ; and with the great multi-
tude the profit to be expected in fame and honor, and eventually
in power and wealth, is a sufficient inducement.
In the extraordinarily numerous attempts to determine the
solar temperature this last incitement has not been present; for the
result can have only a purely scientific, or at the most, a general
The temperature scale used in this article is the Centigrade.— Translator,
1 68 Publications of the
interest for mankind — never such an interest as is aroused by the
opening of new lines in technology, or by the introduction of
new industrial methods.
In the earliest times it was recognized that man owed his very
existence to the Sun, the dispenser of light and heat. This
dependence has been acknowledged in various ways : by the
universal division of time into days and years according to the
motion of the Sun, a custom dating from the remotest antiquity ;
by his introduction as the source of life into the mythologies of
many peoples; and even at the present day by his presence as
the central idea in the religion of the Sun Worshipers.
In astronomical science the Sun was considered for centuries
as a burning heavenly body, burning as a piece of wood bums
in our own atmosphere; but at the beginning of the present century
this idea fell into disrepute through the influence of Herschel,
who assumed the Sun itself to be a dark body surrounded by an
intensely luminous and radiant atmospheric shell. In apparent
agreement with this theory was the evidence aflforded by sun-
spots, whose dark centers were thought to be layers of clouds
seen through openings in the photosphere protecting the solar
surface from the intense radiation of the atmosphere above.
With a means of protection from heat thus provided, it was
characteristic of the thought of the time to fancy the Sun inhabit-
able. The living being able to recognize the all-ruling God, and
therefore in a position to attain the highest goal of nature, was,
according to that thought, the crown of creation, and an uninhab-
itable world was therefore without reason. To-day such specula-
tions are without influence for the majority of investigators. We
admire no longer the harmonious ordering of the universe without
recognizing the existing arrangement as only one of an infinitely
great number of possible arrangements — the one which best con-
forms to the conditions of nature, or which can best adjust itself
to them.
Another idea in harmony with Herschel's theory was that
the shining envelope of the Sun did not possess an especially
high temperature, that it merely shone, and that heat was gener-
ated only when the rays fell upon some body.
In the middle of the century two great revolutionary discoveries
were made which dispatched with a single blow all such ideas.
They were the law of conservation of energy with the related
mechanical theory of heat, and the principles of spectrum analysis.
Astronomical Society of the Pacific, 169
It would lead too far to explain these in detail here, and merely
the final results in their relation to the solar constitution as
accepted by the majority of scientists will be given, with the risk
that such a procedure will be unsatisfactory to many.
We are to imagine the Sun as an enormous glowing ball of
gas, whose temperature diminishes from the center outward. At
a certain depth, and in consequence of causes analogous to those
acting in our own atmosphere, a part of one or more of the
glowing gases is condensed into cloudlike forms. The layer
containing these is called the photosphere ; it is the region from
which the bulk of the heat and light are emitted, and forms at the
same time the visible sharp outline of the Sun. With this idea
of the solar constitution it appears that properly one cannot speak
of a temperature of the Sun, since for different parts the tempera-
ture is quite different ; and if from the solar radiation we determine
a temperature, it must refer to the point of emission, namely, the
photosphere. Our problem is therefore limited to the determi-
nation of the temperature of the photosphere. Here we meet
difficulties at once; for in the study of radiation the constitution
of the radiating body is by no means immaterial. This has been
shown in a previous article in this periodical {Himmel und Erde,
Bd. IX, Heft 6) in connection with the subject of emission, and
may be assumed for the present purpose. There need be remem-
bered only the instance where particles of glass and metal were
subjected to the same temperature. Although the two substances
were of the same temperature, the glass radiated but little heat
and light as compared with the metal, or as it may be stated,
the luminous power of the glass was far less than that of the
metal. Since the emissive power of the particles of the photo-
sphere is unknown, it is necessary to make an assumption as to
its value, if we are to determine the temperature of the photo-
sphere from the intensity of its radiation. The simplest assump-
tion for this value is unity — /. e. equal to the emissive power of
an absolutely black body. It is commonly known that upon
this assumption we obtain the minimum value for the solar tem-
p)erature. If the emissive power is less than i, the temperature
is higher. In what follows it is to be understood that the term
solar temperature refers to that temperature which the photo-
sphere would have in case its emissive power were unity. This
does not remove all of the difficulties, however.
According to our assumptions the photosphere consists not
lyo Publications of the
of a solid body, but of a layer of gas in which solid particles are
suspended. This layer itself can scarcely possess a uniform
temperature ; the inner portions must be much hotter than the
outer. Further, the inner portions emit radiation, which in its
passage through the outer layers is only partially absorbed, and
therefore we cannot speak of a definite temperature as belonging
to the photosphere, but only of an average temp>erature which
may be defined as the sum of the radiation effects from all parts of
the photospheric layer. But with such a constitution there enters
a variation in the emissive power. That quantity for the whole
photosphere depends upon two factors, namely, the number of
solid particles per unit area in the photosphere, and the absorbing
power of the overlying layers of gas. If the emissive power
of the particles themselves be unity, that of the photosphere,
as a whole, will always be less than unity. The greater the
number of particles, the greater will be the emissive power ; but
by increasing the number of particles the emissive power can be
made i only when the absorptive power of the outer layers is
infinitesimal.
It is not easy to see to what extent these factors are operative ;
it results, however, that the assumption, emissive power = i >
is not accurate, but that the value is too large.
From the observation of solar radiation, therefore, we can
solve only the following : To determine the temperature of an
absolutely black body having the same apparent diameter as the
Sun, and the same radiation effects.
We are now in a position to understand what will be meant
in future by temperature of the Sun. There are already con-
siderable difficulties to Ije encountered in the solution of the
problem, and they will increase quite extraordinarily as the
solution progresses.
It must now be asssumed that we are able with appropriate
apparatus to determine with accuracy the intensity of solar radia-
tion. In fact, this determination must be made at the bottom of
our atmosphere, in which the rays have lost a portion of their
energy by absorption. That this loss is not inconsiderable is a
matter of common experience. The rising and setting Sun, for
example, exercise but slight heating effect on account of the great
absorption taking place in the long path through the atmosphere
which the rays must traverse.
We must then determine the exact diminution in the energy
Astronomical Society of the Pacific, 171
of radiation corresponding to a given altitude of the Sun. With
the theoretical part of this determination we cannot here concern
ourselves ; it is closely related to the theory of refraction in our
atmosphere, and its comprehension presupposes a knowledge of
mathematics not to be expected of the general reader. Such an
understanding is unnecessary, for in practice we can do without
the theory of extinction. We need only apparatus for measuring
the intensity of solar radiation for all altitudes of the Sun from
horizon to zenith. The values thus obtained for the loss by
absorption can be plotted as ordinates on co-ordinate paper, with
the corresponding altitudes as abscissae, and a curve can be drawn
through the plotted points. If for a later observation the loss
by absorption for a certain altitude is desired, it can be read from
the curve. A graphical method of this sort leads to the same
results as those obtained by theory combined with observations,
but even this simple procedure becomes exceedingly complicated
on account of the variable absorptive power of air. At the out-
set the absorptive power varies with the barometric height, but
since absorption depends upon the number of particles encoun-
tered by the ray, it is possible to consider the absorptive power
proportional to the barometric height, which leads to a simple
reduction. In a similar manner the altitude of the observer
above sea-level can be taken into account. But far more uncertain
is the dependence of absorption upon water vapor, the amount
of which in the atmosphere is subject to sudden and extreme
variations. It cannot be taken into account with accuracy since
its value can be determined only for points near the surface of
the earth, and not for the upper layers through which the solar
rays must also pass. Again, the effect of the light cloudlike
formations of the upper atmosphere, recognized by their whitish
ap(>earance on the blue sky, is uncertain, and cannot be allowed
for numerically. Thus the actual absorption for each day, often-
times for each hour, is different, and inasmuch as only mean
values can be found, important errors enter into individual deter-
minations whose effect can be eliminated, in a measure, only by
the use of a great number of observations.
At the present day it is possible to determine the effect of
absorption accurately to within, perhaps, ten per cent, of its true
value, so that the corrected radiation values corresponding to the
true solar radiation without an atmosphere are accurate, so far as
they are affected by this one uncertainty, to a proportional amount
172 Publications of the
We have proceeded so far as to get values for the solar radia-
tion unaffected by our atmosphere, and we now come to a descrip-
tion of one of the most important points of the whole problem,
the measurement of the radiation. At first sight this does not
appear difficult \ e. g, ^ thermometer which has been in the shade
can be read and then exposed to the solar radiation; the column
of mercury immediately rises and comes to rest 12° to 14° higher
up. Radiation has increased the reading by this amount, and
fi-om this data we can determine a value for the amount of radiation,
but the value would be only approximate at best; it may be in
error one hundred per cent., or more.
It is an inviolable physical law that every body radiates heat
in all directions, the amount of which depends only on the tem-
perature of the radiating body, and not upon the temperature of
those surrounding it. The higher the temperature, the greater
is the amount of radiation. The same law holds equally for the
surrounding bodies, and it thereby follows that a body of a tem-
perature higher than its neighbors must lose heat, while those of
a lower temperature must gain. The tendency is to set up a uni-
formity of temperature throughout all the bodies in question. It
may be remarked incidentally that this is the condition toward
which the whole universe tends — to an equality of temperature
for all bodies and parts of bodies, be they large or small. The
outlook for the future is a dismal one; for ultimately every source
of energy, whether it lie in animate or in inanimate material, must
become exhausted. We may console ourselves with the thought
that an infinitely long time will be required for this condition of
things to come about.
If now we subject a thermometer to solar radiation, and find,
after a time, that the column of mercury comes to rest in a
higher position than in shadow, it can be said that from this
moment on, the radiation of the thermometer is equal to the
energy received from the surrounding objects, not merely from
the Sun, but also from the ground, from the clouds, from build-
ings, etc. The slightest variation in the position of the instrument
changes its distance from some of the radiating bodies, and con-
sequently the indicated temperature. Even the radiation from
the screen used to protect the thermometer in determining the
difference between shade and sunlight modifies the result.
The observations must be made in open air; for the introduc-
tion of glass into the path of the rays would seriously affect the
Astronomical Society of the PcLcific. i73
result. But here air-currents, even the lightest puff, prove dis-
turbing sources of error, since, in general, they are of a different
temperature from the thermometer, and either give up or take
away heat.
Besides these external sources of error, there is a whole series
of internal ones, depending upon, and varying with, the construc-
tion of the apparatus used. It is, therefore, not surprising that
the accurate measurement of radiation of the Sun is far from a
satisfactory solution — satisfactory to the scientist who desires to
obtain in his investigations the highest possible degree of accuracy.
•If in the measurement of solar radiation we are satisfied to accept
an accuracy of twenty per cent., as will be done in what follows,
in order to gain some insight into the matter^ the problem may
be considered as solved. Instruments designed for the measure-
ment of solar radiation are collected together under the name of
actinometers, of which certain forms are called pyrheliometers.
These instruments are best classified according to whether they
are arranged to give absolute or relative measurements of the
energy of radiation.
With the latter sort is to be included the simple thermometer,
alternately exposed to light and shadow, and also thermo-electric
apparatus, the bolometer,- etc., whose purpose is understood
without further explanation, since they give only differences of
temperature. Instruments of the first sort, for our purpose, are
of greater importance. They indicate not how much the tem-
perature of a body is increased by solar radiation, but how much
heat is conducted to the apparatus by the radiation; they serve
to measure the energy of the solar radiation. The temperature
degree is a measure of the intensity of the heat; while for the
energy a much more complicated unit must be introduced,
namely, the calorie, by which we mean the amount of heat which
must be applied to one gram of water at o°, in order to raise its
temperature to i°. Ten calories, therefore, can be used in an
infinite number of ways; e, g. i gram of water can be raised to
io°, or ID grams of water to i °, or 5 grams of water to 2*^, etc.
Water is chosen as a standard, each substance requiring a rela-
tively different amount of heat to produce a given temperature
effect. Much less heat is required to raise a gram of iron 1° than
a gram of water, and the number expressing the ratio of the
amounts of heat required to produce the same increase in tem-
perature in the same amounts of water and a given substance is
174 Publications of the
called the specific heat of the substance. For example, the
specific heat of iron is o.ii, which means that, to raise i gram of
iron 1° o. II calories is required.
The determination of the number of calories alone is not sufli-
cient for the determination of the heat conducted by radiation;
for the amount received increases with the time during which the
radiation acts, and with the increase of the surface exposed to
the rays.
The energy of radiation is therefore expressed in calories,
referred to i square centimeter of surface and to a duration of
radiation of one minute. Every actinometer must have as an essen--
tial part a surface which is exposed to the radiation, and whose
area and specific heat are accurately known. It is very important
that the surface should absorb as much as possible of the radia-
tion, which means that it must be rough and black; a polished
silver mirror, for example, is scarcely affected by the solar rays.
The first to concern himself with this problem was Pouillet,
who made his experiments in 1838. The pyrheliometer used by
him was of the following construction: —
One end of a flat cylindrical vessel of sheet-silver was black-
ened with soot, and placed so that the solar rays fell perpen-
dicularly upon it. The vessel was filled with about 100 grams of
water, whose increase in temperature was measured by a ther-
mometer projecting into the vessel. During the observation the
vessel was rotated about its axis, in order that the contents
might become of the same temperature throughout. Many later
observers have retained Pouillet's method in its essentials, and
have introduced only slight modifications; for example, Crova
used mercury instead of water.
Of an entirely different construction was the actinometer of
ViOLLE. The surface exposed to radiation was small, and was
protected from wind and the radiation of surrounding objects by
a complete covering of constant temperature. The blackened
bulb of a thermometer served as the surface, and it was placed in
the center of a large double-walled sphere, which was kept at a
constant temperature by flowing water. The exposure of the
thermometer bulb to radiation was made possible by a tube pass-
ing from the center outward, which contained a diaphragm of the
same diameter as the thermometer bulb. When the tube was
directed toward the Sun, the bulb lay in the path of the rays.
As a third fundamental type of actinometer, we may consider
Astronomical Society of the Pacific. i75
that of Angst 6m. It consisted essentially of two equal copper
discs, blackened upon one side and exposed to the Sun. In the
centers of the unexposed surfaces of these discs were attached
thermo-elements, which connected with a galvanometer gave
accurately the temperature of the discs. The two discs were
alternately exposed to the radiation and their differences of tem-
perature measured. An especial advantage of this apparatus
(constructed in 1887) over the others is its symmetrical arrange-
ment, by means of which several external sources of error are
excluded.
It may be further stated, that with none of these apparatus is
it necessary to allow the radiation to act until no further increase
of temperature is perceptible. With short intervals of alternation
between light and shade, it is possible to deduce the desired
quantities from appropriate formulae.
There is yet a whole series of aclinometers which have been
used, but they can all be referred to one of the three types above,
and do not need further explanation. On the contrary, of especial
interest are the numbers which have been obtained for the energy
of radiation of the Sun by means of these various instruments.
Arranged chronologically, they show a decided increase, corres-
ponding to the development of apparatus and methods of obser-
vation.
Obsbrvbr. Year.« Calories.
pouillet 1838 1.76
Forbes 1842 1.82
Hagen i860 1.9
ViOLLE 1875 2.54
Crova 1878 2.3
Langley 1884 3.07
Savelief 1880-1890 3.47
Pernter 1880-1890 3.28
Angstrom 1894 4.0
From this series of values, there appears to be no question
but that the true value of the energy of solar radiation, or the so-
called solar constant, lies between 3.5 and 4.0 calories, and that
we may take, as the most probable value, 3.75, which it will be
noticed, is about double the first determinations.
At the end of this article, several interesting computations
will be carried through with the aid of this constant, but we will
now proceed with the main problem.
176 Publications of the
With a variation of only fifty per cent, in the deter-
minations of solar radiation, a similar variation in the deduced
values of the solar temperature might be expected. This is
not the case, however; the determinations of this tempera-
ture differ from each other so enormously, that in conse-
quence the results have long since been viewed with a certain
contempt For example, it may be noted that Pouillet
deduced the round number 1,500° for the solar temperature,
while Secchi, early in 1870, with a similar apparatus, found
the value 10,000,000°.
Wherein, then, do these inconceivable differences enter ? The
answer to this question leads us at once to the most difficult, and
at the same time the most interesting, part of our problem. It
is required to determine from relatively small differences of tem-
perature the value of an extremely high temperature, and naturally
any error in the temperature difference appears enormously multi-
plied in the result. Let us begin, for example, with an error of
1° in a temperature difference of 10°; if the true result should be
10,000°, it will appear, in consequence of the error, increased by
1,000° This, however, in itself is insufficient to explain the great
discrepancies which occur; a much more uncertain source of error
arises from a lack of knowledge concerning the law of radiation —
the law connecting the temperature of the radiating body with
the energy of the radiation emitted. A law of this sort can be
deduced from observations ,in the laboratory. A sheet of plati-
num, for example, can be heated to a temperature of 1,000°,
and then its radiation can be studied. But aside from the great
practical difficulties which oppose such investigations, there is the
unfortunate circumstance that the temperature of the Sun is
doubtless far hig^her than any temp)erature which can be produced
for measurement in the laboratory; from the relation between
radiation and temperature from 0° to 1,000° must be inferred the
relation for temperatures from 1,000° to 10,000°.
If the relation between temperature and radiation be plotted
as a curve, with temperatures as abscissae, that part of the curve
between 0° and 1,000° can be accurately determined by observa-
tion. The course of the nine-tenths of the curve beyond 1,000°
can be judged only from the course of the first tenth, and it is
evident that beginning with 1,000°, it may take courses whose
ordinates for higher temperatures vary enormously. Such an
uncertainty it was which affected Secchi's determination; and
Astronomical Society of the Pacific, ^77
most significant is the result when Secchi*s observations are
reduced by the same law as used by Pouillet. A temperature
of 1,400° is thus obtained from the same numbers, which with
the application of another law by Secchi gave 10,000,000°.
The famous Newton was the first to investigate the relation
between radiation and the temperature of the radiating body.
He came to the conclusion that the rate of cooling of a radiating
body is directly proportional to the difference in temperature
between the radiating body and the bodies surrounding it. It is
assumed here that the radiating body is of a uniform temperature
throughout, and that its power of emitting heat is infinitely great.
These ideal conditions are the more nearly satisfied the slower
is the cooling of the surface, i, e, the smaller is the temperature
difference. They are not satisfied in the case of the Sun,
although it cannot be denied that with a body gaseous at the
surface, like the Sun, the convection currents of the gas may
afford a certain approximation to the ideal conditions.
It has been shown that Newton's law of cooling can be con-
sidered only as a rough approximation, applicable for small
temperature differences, but quite misleading when these differ-
ences are large. In recent times the most various attempts have
been made to determine a law which should be valid for the
highest temperatures. The most important of these will now be
noticed.
First are the French physicists Dulong and Petit, who con-
tinued Newton's investigations. They found as a satisfactory
law for the temperature interval of 280° used by them, that the
amount of heat radiated by a body diminished according to a
geometrical progression with a uniform diminution of tempera-
ture. No theoretical considerations can be advanced in favor of
the applicability of this purely empirical law to higher tempera-
tures; and to-day there is no doubt that values of the solar
temperature extrapolated by means of this law are too small, but
not in the degree in which values obtained by Newton's law are
too large. It may be remarked that Pouillet computed
according to the law of Dulong and Petit, while Secchi used
Newton's law.
A second law applicable to temperatures between 0° and 300°
was deduced by Rosetti; its form involves a mathematical
expression not easily expressed in words.
Only during the last decades have considerable advances been
i?^ Publications of the
made in the determination of the form of this law. First among
them is the somewhat complicated mathematical form found by
Weber, a Swiss, which represents satisfactorily all the experi-
mentally deduced relations up to i,ooo°, but which is not suscep-
tible of a theoretical interpretation. The Austrian physicist
Stefan has determined an extremely simple law, which, with a
slight modification, retains its validity to 1,300^, as shown by
recent tests by the Berlin physicists 'Lum me R and Pringsheim.
Stefan's law states simply: The amount of heat radiated by a
body is proportional to the fourth power of its absolute tempera-
ture — to the 3.96 power according to Lummer and Pringsheim.
Besides the extreme simplicity of this law, there is the circumstance
that Boltzmann has been able to establish it theoretically, from
the electro-magnetic theory of light and the mechanical theory of
heat.
It is of especial importance to note that the two last-named
laws of Weber and Stefan differ so slightly for the highest
temperatures yet investigated, that it is extremely probable the
values obtained by extrapolation in their application to the Sun
will be near the true values.
It is possible to conclude from the agreement of the laboratory
experiments that the resulting solar temperatures will not vary
by more than half the true value, which, in view of the difficulties
of the problem, is really a satisfactory solution. With the appli-
cation of one of these laws, it is therefore possible to bring order
into the chaos of solar temperatures, as is shown by the follow-
ing list, computed according to Stefan's law: —
Obsbrvbr. Solar Tbmpbraturb.
pouillet 5,600°
Secchi 5,400
ViOLLE 6,200
SORET 5*500
Langley 6,000
Wilson and Gray 6,200
Paschen 5,000
RosETTi io,ooo{;s:^i;
There is here doubtless justification for the assumption that
the solar temperature is greater than 5,000° and less than
10,000°; the value T = 6,25o° corresponds to the mean of the
above determinations.
Astronomical Society of the Pacific, i79
The reader will perhaps breathe again in the hope that he is
now to be released from the difficulties of the discussion of the
solar temperature; but this hope is unfortunately not to be
satisfied, for the value T thus obtained represents in no way the
temperature of the photosphere as it was in the beginning
defined, but only that temperature which the photosphere would
have on the assumption that the radiation has come unimpeded
to the Earth. But the Sun possesses an atmosphere which,
similarly to that of the Earth, absorbs a portion of the radiation;
the actual temperature is therefore higher than the value we have
obtained. That such an atmosphere exists is shown by the direct
view of the Sun through a telescope. Thus seen, the disc is not
uniformly bright, as it must be in the case of a simple glowing
sphere, but at the edges is much darker, owing to the longer path
through the Sun*s atmosphere which must be traversed by the
rays here than at the center. It is possible to compute the
relative lengths of the latter through the atmosphere for different
points of the disc, which, combined with the directly observed
increase in absorption toward the limb, leads to the law of absorp-
tion, and thus it is possible to compute the total absorption of
heat rays due to the Sun's atmosphere. Observations have
shown that, as in the case of the Earth's atmosphere, different
kinds of rays are very differently absorbed — the nearer they lie
to the violet end of the spectrum, the greater is the absorption.
The rays lying at the other end of the spectrum are least
absorbed, though even here very considerably, since the most
careful observations by H. C. Vogel, and the recent determina-
tion of Frost show that the transmission coefficient lies between
0.72 and 0.79. It is therefore necessary to multiply the deter-
mined radiation by 1.5 in order to get the true value, which
increases the solar constant to 5.6 calories. How the solar
temperature is now to be computed is as yet undetermined, for
Stefan's law is no longer applicable; we may assume that T lies
between 7,000° and 10,000°.
For a comparison with terrestrial temperatures, it may be
remarked that the temperature of the electric arc varies from
3,000° to 3,500°; the temperature of a very long electric spark
is much higher, running up to 20,000°, and even higher.
(To be concluded in No. 65.)
i8o Publications of the
NEW OBSERVATIONS OF THE OTTO STRUVE
DOUBLE STARS.
By W. J. HussKY.
Early in the history of the Pulkowa Observatory a plan of
work for the meridian -circle, afterwards materially modified, con-
templated the exact determination of the places of all stars of
the Northern Hemisphere to the seventh magnitude, inclusive.
At that time there was no complete Hst of such stars, and to form
one, giving their approximate places, was the first step in this
piece of work. The formation of this preliminary catalogue was
undertaken by Otto Struve. With the help of two assistants,
he made the necessary observations, with the 15-inch refractor,
between August 26, 1841, and December 7, 1842. In this short
interval he examined with the finder of the large telescof>e every
portion of the sky north of the celestial equator, and selected
the stars (about 17,000 in number) to be included in the cata-
logue. Each one selected was brought to the center of the field
of view of the large telescope, and its approximate position was
obtained by noting the time and the readings of the hour and
declination circles; at the same time it was carefully examined,
to see whether it was double. This examination resulted in a
list of 514 objects known, or thought to be, double or multiple,
and new to science. In this list, the distances between the com-
ponents were all to be less than 32", and the magnitude of the
principal star, or, in the case of close doubles, the combined
magnitudes of the two, did not descend below 7.8. As compan-
ions, all objects at distances less than 16", and bright enough to
be readily measurable with the 15-inch telescope, were admitted;
while for distances between 16" and 32" the limiting inferior
magnitude of the companion adopted was 8.9.
This list of double stars, discovered at Pulkowa, was first pub-
lished in 1843. Between this time and 1850, sixteen additional
pairs were discovered, and were included in the second edition,
published in 1850, under the title ** Catalogue revu et corrig6
des ^toiles doubles, decouvertes ^ Poulkowa." Subsequently
other discoveries were made, increasing the list to a total of 547
objects, which are now known as the Otto Struve double stars,
or as the double stars of the Pulkowa catalogue. They are
denoted by the symbol 02.
Astronomical Society of the Pacific, i8i
Many of the 17,000 stars of the preliminary catalogue were
examined under poor atmospheric conditions. On this account
a large number of important pairs were overlooked, and on the
other hand a considerable number of stars were admitted to the
list of 514 which were of a very doubtful character. A careful
examination of these under better atmospheric conditions led to
the rejection of 106 of them, either on account of their being
single or having distances surpassing the limits adopted, or hav-
ing companions too faint for exact micrometric measurement
with the 15-inch telescope, or because of clerical errors in the
readings or records, due in part, perhaps, to the notation em-
ployed in the formation of the catalogue. These 106 stars were
omitted in the second (1850) edition of the Pulkowa catalogue,
and are known as the Otto Struve rejected stars.
Volume IX of the Pulkowa Publications contains the double-
star observations made by Otto Struve during a period of
thirty-seven years, from the establishment of the Pulkowa Observ-
atory, in 1839, to 1875. A section of this work is devoted to the
441 Otto Struve stars not rejected, and contains about 2,080
observations of them. Nearly all these stars were first ob-
served in the three or four years immediately following 1843.
After the beginning of 1852 only about half of the stars were
observed, after i860 less than a third, and after 1870 less than
one-fifth.
A second series of measures of equal importance was made
by Baron Dembowski between 1865 and 1878. In spite of the
small size of his instrument (7)4 inches aperture) he succeeded
in obtaining excellent measures of all but the most difficult of
these stars. Out of the 547 objects enumerated in the Pulkowa
catalogue, he measured 432, making altogether 2,155 observa-
tions of them.
These are the only large, and in a measure complete, series of
observations of these stars that have been published. Certain of
them have been observed many times by different observers.
These are, in general, those which have proved to be binaries,
and those which have shown sufficient motion to make it desira-
ble to have a fairly continuous series of measures of them.
Early in the present year, I began to measure the Otto
Struve stars for the purpose of obtaining for this epoch determi-
nations of the relative positions of all of them that are given in
Vol. IX of the Pulkowa Publications. I subsequently added to
i82 Publications of the
this list such of the rejected stars as were measured by Dembow-
SKI, and some others which Otto Struve rejected as single,
but which other observers have since found to be double. The
observing list, as thus made up, contains nearly five hundred
stars, and it will require some 1,700 or 1,800 observations to
obtain complete sets of measures of all of them.
The conditions have been favorable for the prosecution of this
piece of work. During the past eight months I have made
about 1,350 observations of 414 different stars. Three hundred
and forty-one stars have been observed on three or four nights
each, and are regarded as finished. It is the plan to continue
the work until, in general, each star has been measured on at
least three different nights.
Most of the observations are being made with the 12-inch
telescope. All difficult pairs are, however, measured with the
36- inch refractor. Measurements are made only on nights when
the conditions are favorable for securing good results.
The following notes relate to some of the stars that I have
found of interest:
The observations of 02 283, by Otto Struve and Dem-
BOWSKi, give rather discordant distances. I attempted to mea-
sure it with the 12-inch telescope, but found it difficult to obtain
satisfactory measures of distance with that instrument. On
examining it with the 36-inch refractor, I found the faint star a
close double; distance, i".27; magnitudes, 11^ and 12; and the
line joining them making an angle of about 10^ with that which
connects the principal star with the brighter of the faint compo-
nents. With this configuration, it is probable that the presence
of the fainter companion, by reason of its not being clearly seen,
has an influence on the distance measures made with small
telescopes.
Some months ago, I found 02 341 single (see these Publica-
tions^ Vol. X, p. 121,) whereas the observations from 1845 to
1886 had seemed to indicate that jthe two components were rela-
tively fixed at a distance of about o".4 or o".5. A recent obser-
vation, 1898, 707, shows an elongation ©".09, and a change of
quadrant, 254^.3. The smaller star has already passed perias-
tron, and an increase of distance may now be expected.
While observing OS 351, I discovered the south component
to be a close double, of which I have made the following
measures:—
Astronomical Society of the Pcuific. 183
1898.572
309°-9
o".33
592
307 .6
.36
595
312 .9
.32
707
309 -6
.36
1898.62
3io°.o
^9f m A
.34
The north star A is decidedly brighter than B, though less
bright than B and C combined. These considerations reverse the
quadrant of the OS pair as given by previous measures. The
Otto Struve pair has a distance of about o".6, and its components
have shown no certain motion. In a private letter, Professor
BuRNHAM states that he can recall no other instance of three
stars so close together. I have, however, more recently found
another case. It is that of OS 476.
The north component of OS 476 is a very close double. My
measures are as follows : —
1898.630 227^.7 o".i5
690 229 .5 o .17
707 224 .4 o .13
1898.68 227°. 2 o".i5
In this case the Otto Struve pair has a distance of ©".54,
and has shown no motion.
I have looked very carefully for OS 546 on several occasions
with both the 12- and 36-inch telescopes without finding it.
Dembowski had a similar experience. In the Pulkowa catalogue
of 5,634 stars, Romberg gives number 4093 as OS 546. I have
examined this star, and do not find it double. Otto Struve
measured OS 546 but once, and speaks of its being near S 2396.
The measure he gives, including position angle, distance, magni-
tudes of components, and position in the sky, all agree so closely
with those of OS 362 as to make it highly probable that it is
identical with the latter.
Lick Observatory, September 18, 1898.
1 84 Publications of the
THE MOTION OF ^CEPHEI IN THE LINE OF SIGHT.
By W. W. Campbell.
In the course of our determinations of stellar velocities in the
line of sight, I have found that the star i\ Cephei has a very-
great velocity toward the solar system. Four spectrum plates
of this star have been secured and measured by Mr. Wright
and myself. They yield the following velocities in kilometers
per second:— _ g^^
- 87.2*
-86.2
-86.9
-86.2
Mean — 86.8
The equivalent in English miles is — 53.9.
The motion of i\ Cephei at right angles to the line of sight is
about 0.8 second of arc annually.
We have confirmed the resultsf obtained by Dr. Belopolskv,
at Pulkowa, for the star £ Mer cutis. Our results from four plates,
together with those previously obtained by Dr. Belopolsky
from seven plates, are as follows: —
Belopolsky. Campbell.
— 68 km. — 69. 1 km.
- 84 - 70.4
- 75 - 70.0
-67 -7i-it
— 66 — 70.9
-64
-69
Means — 70 km. — 70.3 km.
The equivalent result in English miles is — 43.7.
It should be noticed that these stars are situated in the part of
the sky toward which the solar system is moving, and the above
results are the sums of the stars* motion toward our system, and
of our system toward them. If we assume that the solar system is
♦Measure of the same plate by Mr. Wright.
t Published in Astronomische Nachrichten, No. 3184.
\ Measure of the same plate hv Mr. Wright.
Astronomical Society of the Pacific. 185
moving toward the point in the sky whose Right Ascension is
267° and whose Declination is + 3i°> with a velocity of 17 kilo-
meters per second, then the solar components toward ly Cephei
and £ Herculis are respectively 12.7 and 16.4 kilometers per
second. Applying these corrections, the velocities of these stars
with reference to the sidereal system become —
for -q Cephei^ — 74. i km. per second.
for Ji Herculis, —53.9 km. per second.
Their equivalents in English miles are —46.0 and — 33.5.
(THIRTIETH) AWARD OF THE DONOHOE COMET-
MEDAL.
The Comet- Medal of the Astronomical Society of the Pacific
has been awarded to E. F. Coddington. Fellow in Astronomy
at the Lick Observatory, for his discovery of an unexpected
comet on June 11, 1898.
The Committee on the Comet- Medal,
James E. Keeler,
Wm. M. Pierson,
August II, 1898. Chas. Burckhalter.
(THIRTY-FIRST) AWARD OF THE DONOHOE
COMET-MEDAL.
The Comet- Medal of the Astronomical Society of the Pacific
has been awarded to C. D. Perrine, Assistant Astronomer in
the Lick Observatory, for his discovery of an unexpected comet
on June 14, 1898.
The Committee on the Comet- Medal,
James E. Keeler,
Wm. M. Pierson,
August 14, 1898. Chas. Burckhalter.
(THIRTY-SECOND) AWARD OF THE DONOHOE
COMET-MEDAL.
The Comet- Medal of the Astronomical Society of the Pacific
has been awarded to E. Giacobini, of the Observatory, Nice,
France, for his discovery of an unexpected comet on June 18, 1898.
The Committee on the Comet-Medal,
James E. Keeler,
Wm. M. Pierson,
August 18, 1898. Chas. Burckhalter.
1 86 Publications of the
PLANETARY PHENOMENA FOR NOVEMBER AND
DECEMBER, 1898.
By Professor Malcolm McNeill.
Mercury is an evening star, and toward the end of the month
it remains above the horizon an hour or more after sunset, and
may be seen under favorable weather conditions. On November
19th it is in conjunction with Venus, passing 1° 18' north of the
latter. As the planets then set less than an hour after the Sun, it
will be difficult to see them, unless the horizon is very free from
cloud and haze.
Venus is still an evening star, but is rapidly approaching
inferior conjunction with the Sun, and after the middle of the
month it will not be easy to see it. At the beginning of the
month it has just passed its period of greatest brilliancy.
Mars rises earlier, before 9 o'clock, at the end of the
month. It moves about 8° eastward during the month through
the constellation Cancer, On November nth it passes less than
half of the Moon's diameter south of the fifth-magnitude star
t\ Cancri, Its distance from the Earth decreases more than
20,000,000 miles during the month, and at the close is about
77,000,000. Its brightness increases about sixty per cent.
Jupiter is a morning star, and rises from one to three hours
before sunrise according to the time of the month. It is in the
eastern part of the constellation Virgo, and moves about 6**
eastward and 2° southward during the month.
Saturn is still an evening star, and is not far enough away
from the Sun toward the end of the month to be seen. It is in
conjunction with Venus on November 23d, passing 4° to the
north of the latter; but both planets are too near the Sun to be
easily seen.
Uranus is in conjunction with the Sun and changes from an
evening to a morning star on November 25th, but remains too
near the Sun to be seen.
Neptune is above the horizon nearly the entire night, and is
on the border line between Taurus and Gemini,
December.
The winter solstice comes and winter begins December 21st.
II A.M. P. S. T.
Astronomical Society of the Pacific. 187
Eclipses. There will be two eclipses during the month. The
first is a partial eclipse of the Sun on December 13th. It is
visible only in the South Pacific Ocean, and its greatest magni-
tude is only a little more than one-fortieth of the Sun*s diameter.
The second is a total eclipse of the Moon on December 27th,
and will, in part at least, be visible throughout the entire country.
Total eclipse will end at 4^ 27"" p.m. Pacific time, just about the
time the Moon rises in the extreme western part of the United
States.
Mercury is an evening star at the beginning of the month,
and comes to greatest eastern elongation on December 3d. For
the first ten days of the month it sets an hour or more later than
the Sun, and may be seen in the evening twilight on a clear
evening. After that, it rapidly approaches the Sun, and passes
inferior conjunction on December 21st, becoming a morning star.
At the end of the month it rises an hour and a half before sunrise.
Venus passes inferior conjunction with the Sun on December
ist, and becomes a morning star. By December loth it rises
more than hour before sunrise, and after that it may be seen in
the morning twilight.
Mars is getting into better position for evening observation,
rising before 9 o'clock on December ist, and more than two
hours earlier on December 31st. It moves eastward about 1°
until December loth, and then moves westward 3° and north-
ward 2° before December 31st. Its line of backward motion is
about 2° north of the line it traced moving eastward in November.
On December 29th, it passes about the Moon's diameter north
of the fifth magnitude star y Cancri. During the month its
distance from the Earth diminishes about 14,000,000 miles, and
is about 63,000,000 at the close. Its brightness increases about
fifty per cent, during the month.
Jupiter rises about two hours earlier than during the corre-
sponding period of November, at 2:20 a.m. on December 31st.
It moves about 3° east and south in the constellation Virgo,
Saturn is in conjunction with the Sun on December 6th, and
becomes a morning star. It remains near the Sun, but may
possibly be seen toward the close of the month in the morning
twilight.
Uranus is a morning star also, but its faintnes^ precludes its
being seen until its distance from the Sun is greater.
Neptune comes to opposition with the Sun on the evening of
December 14th.
1 88
Publications of the
Phases of the Moon. P. S. T.
Last Quarter,
H. M.
^ov. 6, 6 28 A. M.
Dec. 6,
H. M.
2 6 A. M.
New Moon,
Mov. 13, 4 20 p. M.
Dec. 13,
3 43 A. M.
First Quarter,
JJOV. 20, 9 5 A. M.
Dec 19,
7 22 p. M.
Full Moon, ]
Nov. 27, 8 39 P. M.
Dec. 27,
3 39 P. M.
The Sun.
R. A.
Declination.
Rises.
Transits.
Sets.
189S.
H. M.
/
H. M.
H. M.
H. M.
Nov. I.
14 27
- 14 32
6 34 A.M.
II 44 A.M.
4 54PM.
II.
15 7
- 17 31
6 45
II 44
4 43
21.
15 48
— 20
657
II 46
4 35
Dec. I.
16 31
— 21 52
7 8
II 49
4 30
II.
17 14
- 23 2
7 17
II 54
4 31
21.
17 59
- 23 27
7 23
II 58
4 33
31.
»8 43
- 23 5
7 26
12 3 P.M.
4 40
Mercury,
Nov. I.
14 58
- 17 35
7 15A.M.
12 14 P.M.
5 13 PM.
II.
16
-22 17
7 57
12 37
5 17
21.
17 3
- 25 9
8 34
I I
5 28
Dec. I.
18 I
-25 48
8 56
I 20
5 44
II.
18 34
— 24 12
8 42
I 13
5 44
21.
18 3
— 21 23
7 20
12 3
4 46
31-
17 25
- 20 8
5 56
Venus.
10 45 A.M.
3 34
Nov. I.
16 54
- 27 57
9 57 A.M.
2 II P.M.
6 25 P.M.
II.
17 2
— 27 36
9 24
I 40
5 56
21.
16 54
-25 58
8 28
12 51
5 14
Dec. I.
16 32
— 22 58
7 13
II 50 A.M.
4 27
II.
16 10
- 19 34
5 59
10 50
3 41
21.
16 2
- 17 17
5 2
10 2
3 2
31.
16 10
- 16 35
4 28
JhARS.
9 30
2 32
Nov. I.
8 13
+ 21 28
10 13 P.M.
5 30 A.M.
12 47 P.M.
II.
8 27
+ 21 I
9 50
5 5
12 20
21.
8 38
+ 20 44
9 23
4 37
II 51A.M.
Dec. I.
8 45
+ 20 43
8 51
4 5
II 19
II.
8 48
+ 21 2
8 13
3 28
10 43
21.
8 44
-h2i 42
7 29
2 46
10 3
31.
8 35
+ 22 41
6 36
I 58
9 20
Jupiter.
Nov. I.
13 33
- 832
5 19 A.M.
10 50 A.M.
4 21 P.M.
Dec. I.
13 56
— 10 42
3 52
9 15
2 38
31-
14 6
— 12 24
2 20
7 37
12 54
Astronomical Society of the Pctcific. 189
Sa turn.
Nov. I.
16 37
— 20 38 9 7A.M,
I 54 P.M.
6
41 P.M.
Dec. I.
16 52
— 21 7 7 25
12 10
4 55
31-
17 7
- 21 30 5 44
Uranus.
10 27 A.M.
3
10
Nov. I.
16 I
— 20 31 8 30A.M.
I 17 P.M.
6
4 P.M.
Dec. I.
16 9
— 20 52 6 42
II 27 A.M.
4
12
31-
16 i6
-21 II 4 53
Neptune
9 37
2
21
Nov. I.
5 36
+ 22 7 35P.M.
2 54 A.M.
10
I3A.M.
Dec. I.
5 33
+ 21 57 5 34
12 53
8
12
31-
5 30
+ 21 55 3 29
10 48 P.M.
6
7
Eclipses
OF Jupiter's Satellites, P. S.
T.
(Off left-band limb as seen in an invertinK telescope.)
H. M.
H.
M.
I. D.
Nov. 14.
5 55 A.M. I, D,
Dec. 7.
6
5 A.M.
II. D,
15-
5 40 A. M. II, D,
10.
2
36 A.M.
III, R.
19.
3 21 A.M. I, D,
15.
2
27 A.M.
I. D.
23-
2 17 A.M. II. D,
17.
5
9 A.M.
III. D,
26.
5 23 A.M. I. D,
23.
4
21 A.M.
III, R.
26.
7 18 A.M. I, D,
30.
6
14 A.M.
I. D.
29.
4 II A.M. I, D,
Jan. I.
12
42 A.M.
in, D,
I.
I
9 A.M.
HI, R,
I.
3
3 A.M.
NOTICES FROM THE LICK OBSERVATORY.*
Prepared by Members of the Staff.
New Gases in the Earth's Atmosphere.
Our readers will remember notices in Vol. VII (pp. 6i and
88) of these Publications^ calling attention to the discovery by
Lord Rayleigh and Professor Ramsay of a new atmospheric
gas called by them argon. These investigators and others have
continued their researches along the same lines, being aided by
the recent improvements made in the process of liquefying air
by means of which extremely low temperatures may be produced.
The result is the discovery of at least two new gases in the
Earth's atmosphere, and of a third which may prove to be new.
Messrs. Ramsay and Travers communicated to the Royal
Society on June 3d of this year a preliminary note on krypton^
the first of these new gases. From 750 '^ *'™ of liquid air, they
obtained 27 '^ *"" of a gas whose spectrum differs from that of any
other known element. Besides many feeble lines, the spectrum
exhibits two brilliant lines, one at X 5869 (very near the D3 line)
and the other at A 5570.
The properties of the new gas are not yet fully determined,
but the discoverers venture the conjecture that its density will
turn out to be 40, with an atomic weight of 80. By comparison
of the length of a sound-wave in it and in air, krypton is shown
to be monatomic and an element.
The coincidence of the line A 5570 with the principal line of
the Aurora has been noted by several observers, and it is sug-
gested that we have **at last the true origin of that hitherto
perplexing line.** In this connection, it is of interest to recall
the experiments by Liveing and Dewar in passing sparks
* Lick Astronomical Department of the University of California.
192 Publications of the
through small layers of liquefied oxygen, air, and nitrogen. (See
brief review in Astrophysical Joumaly Vol. I, p. 88.) Under
certain conditions of temperature, pressure, etc., the spectrum of
liquid oxygen showed a line at X 5572. ** The wave-length of the
auroral line is A 557 1.6; and the conditions of temperature and
pressure in these experiments must have been somewhat similar
to those under which the Aurora appears. This points, of
course, to the probability of the auroral line being due to the
oxygen of our atmosphere.*'
Still more recently, Professor Ramsay and Dr. Norman
Collie succeeded in liquefying a quantity of argon. It formed
a colorless fluid, but two other products also resulted. These
were a lighter gas which failed to liquefy, and a solid deposit
which gathered on the sides of the tube.
The lighter gas was drawn off and its spectrum examined.
In Professor Ramsay's announcement to the Royal Academy,
on June i6th, the spectrum of this gas, called by him iieon^ is
described as containing a large number of strong lines in the red,
orange, and yellow, and in the deep violet. Experiments to
determine its density seemed to indicate that the gas had not
been obtained in its pure form.
These two gases are undoubtedly new elements; but the third,
obtained from the solid frozen out of the argon, may yet prove to
be a new compound of known elements, rather than a new
element. This substance, called meiargon by its discoverers, has
a density of 19.87, the density of argon being 19.94. ^^
spectrum showed many bands whose wave-lengths are closely
coincident with those in the band spectrum of carbon and with
three cyanogen bands, as was pointed out by Professor Schuster
{Nature, Vol. LVIII, p. 199).
The spectroscopic evidence is therefore strong that it is
some carbon compound rather than a new element. Subsequently
{Nature^ Vol. LVIII, p. 245), Messrs. Ramsay, Travers, and
Baly describe precautions taken, and chemical tests applied, to
exclude the possibility of any carbon existing in this gas, and ask
for a suspension of judgment pending further investigation.
R. G. AlTKEN.
The Minor Planet (334) Chicago,
This small planet was discovered, photographically, by Pro-
fessor Max Wolf, at Heidelberg, August 23. 1892. While
Astronomical Society of the Pacific. i93
^"^ attending the astronomical conferences held in connection with
■ the World's Fair, August. 1893, he gave it the name Chicago,
r^- The planet Chicago is of more interest than many of the
T- asteroids, by reason of the nearness of its orbit to that oi Jupiter,
^— and of the large perturbations which it experiences when it is in
-'- the vicinity of the latter planet. In 1894, the two planets were
' " near together, their distance being only 1.25 astronomical units.
At that time Jupiter's perturbing force amounted to ihth of
the attractive force of the Sun.
^ The periodic times of the two planets are very nearly in the
commensurable ratio of 2 to 3, the mean daily motion of Jupiter
' being 299". 12836, and that of Chicago, 455". 998. VJhW^ Jupiter
makes two revolutions about the Sun, Chicago makes slightly
more than three. As a result, the consecutive returns of the two
planets to those points in their orbits where they are nearest
together fall at nearly the same places, allowing the perturba-
tions to have an accumulative effect. These points, however, do
not exactly coincide, but move slowly around the orbits, com-
pleting a revolution only after a long interval of time. This
insures the exbtence of very sensible inequalities of long period
and of considerable changes in the values of some of the elements
of the orbit of Chicago, The perturbing action of Jupiter
will cause the eccentricity of the orbit of Chicago to decrease
until it becomes zero (^Astrophysicat Joumai, December, 1897);
this orbit will then be truly circular, and as the eccentricity
passes on to negative values, the longitude of perihelion will
change 180°.
These considerations make it desirable to obtain at each
opposition a sufficient number of observations of the planet
Chicago to form a secure normal place, thus affording the data
necessary for the basis and control of the theoretical investiga-
tions relating to its orbit. With this object in view, I obtained
observations of it on six nights in May and June of the present
year with the 36-inch refractor, and on five of these nights
observations were also made by Mr. Coddington.
This planet is faint (i 2.1 magnitude), and at the time our
observations were made it was passing through a region of the
sky where faint stars of about its brightness are especially
numerous. On this account, it would have been a matter of con-
siderable difficulty to find the planet by examining the stars
visually for motion, and the more so since it was nearly three-
194 Publications of the
quarters of a degree from its predicted place. This difficulty was
removed by Mr. Coddington, who first photographed the
region with the Crocker telescope, giving an exposure of three
hours. He identified the planet by means of its trail, and derived
an approximate correction to the ephemeris. He next prepared
charts of the faint stars shown on his photographic plates, and
inserted on them the predicted places of the asteroid for the
times at which we intended to observe it. This proved very
successful. At thfe time of the first observation, I selected the
planet at the first trial, and within five minutes from the time
when the telescope was pointed to the proper field had it identi-
fied, by means of its motion. At the times of the other observa-
tions we found it with almost equal ease. W. J. Hussev.
Lick Observatory, September 13, 1898.
The New Minor Planet, 1898 DQ,
The minor planet, 1898 DQ^ discovered photographically by
Witt at the Urania Observatory, Berlin, August 13th, promises
to be of unusual interest. According to the preliminary elements
of its orbit, computed by Berberich, its perihelion lies far within
the orbit of Mars; and indeed so close does its path come to that
of the Earth, that at the place of nearest approach they are
separated by less than 15,000,000 miles. When nearest the
Earth, the planet's equatorial horizontal parallax is about a
minute of arc, exceeding that of any other known body whose
position can be measured with the same degree of accuracy.
On this account, it will be an excellent object by means of which
to determine the solar parallax, and thence the mean distance of
the Elarth from the Sun. W. J. Hussev.
Lick Observatory, September 27, 1898.
Discovery and Orbit of Comet h 1898 (Perrine).
This comet was discovered in the morning of September 13th.
This is the eighth comet to be discovered this year, five being unex-
pected. The comet's position on the morning of discovery at o^
58" 8' G. M. T. of Sept. 13th, was a 9*^ 35"» 49'.27, 8 + 31^4' 3i".o.
The comet was then between the two constellations Leo^ Major
and Mifior, and was moving east 6" per day and south 30'. Its
daily motion is rapidly increasing in both co-ordinates, and thus
gaining on the Sun at such a rate that it will probably be lost in
the dawn early in October. At the time of discovery, it had a
Astronomical Society of the Pacific. 195
round head 4' or 5' in diameter with a well-marked central
condensation, the entire head being about as bright as an eighth-
magnitude star. As it is approaching both the Sun and Earth, it
is becoming brighter. It has had a narrow tail about %^ long,
pointing away from the Sun. This tail has never been con-
spicuous, even with the 12-inch refractor. Within the last few
days a sharp nucleus has developed. This nucleus was noted
as stellar on September 20th, when the seeing was best, and of
about the tenth magnitude. From observations secured here on
September 12th, 13th, and 14th, the following preliminary orbit
was computed by R. G. Aitken and the writer: —
T = 1898, October 20.0168 G. M. T.
<a = 165° 16' 48" ^
0= 36 5 29 I Ecliptic and
/ = 29 12 14 ( Mean Equmox of 1898.0
log q = 9.58456
Residuals for the middle place were:
(O— C): AX' COSTS' + 3"
A)8' - I
From these elements it will be seen that the comet makes its
nearest approach to the Sun on October 20th, at a distance of
36,000,000 miles. An ephemeris from these elements shows
that the comet is becoming rapidly brighter, being three times
as bright as at discovery, on September 30th, the last date of the
ephemeris.
These elements bear no special resemblance to any known
comet. C. D. Perrine.
September 22, 1898.
New Elements of Comet h 1898.
From the Mount Hamilton observations of this comet at
discovery, September 12th, and on September 17th and 22d, I
have derived the following parabolic elements: —
T = 1898, October 20.53478 G. M. T.
0,= 162^ 26' 8^3^ ^ ,. . ,
r Ecliptic and
" = 34 55 37 -5 > Mean Equinox of 1898.0
/ = 28 51 27 .2 ;
log q = 9.622688
Residuals for the middle observation:
(O-C): AX' cos r +o".4
A/3" - I .0
196 Publications of the
On October 22d, the comet is in conjunction with the Sun in
R. A. and becomes an evening object. It should be again visible
from southern stations (only) about November ist and for a
month after. Its greatest theoretical brightness will be on October
20th, at the time of its passing perihelion, when it will be seven
times as bright as at discovery. On September 23d, it was just
visible to the naked eye against a dark sky. Some of the abso-
lute dimensions may be of interest. The head is 4' in diameter^
as seen with the 12-inch telescope, which corresponds to an
actual diameter of 150,000 miles. With the same telescope, the
tail can be traced for )^°(the tail is in all probability several
times this length), or a length of about 600,000 miles. After
passing perihelion, the comet will be close to the planet Mercury
for a week or more, the distance ranging from 6,000,000 to
8,000,000 miles. The longitudes and distances from the Sun of
both Mercury and the comet are very nearly the same, but
owing to their different nodes, inclinations, and motions in their
orbits, they do not make as close an approach as otherwise they
would. At this distance of 6,000,000 miles, the comet would be
a striking object as seen from Mercury, the head i^° in diameter,
the tail 5° or 6° in length. The brightness would be over 150
times that on September 27th as seen from the Earth, when it was
visible to the unaided eye. This would make it more conspicuous
than a first-magnitude star. C. D. Perrine.
September 28, 1898.
Elements of the Minor Planet, 1898 DQ,
From the mean of the two Kiel observations of August 15th
by Dr. Ristenpart, and my own observations of September 6th
and 27th, I have computed the following elements of this inter-
esting planet: —
Epoch 1898, August 31.5 G. M. T.
M = 222^ 51' 53".3
c.= 176 52 17 .6 1 Ecliptic and
"^^'Jo 4J J5 -.3 j Mean Equinox of 1898.0
</> ^ 12 49 40 .7
logfl = 0.164038
/* = 20T3".49i
Period = 643.66 days =^1.76 years.
Astronomical Society of the Pacific. 197
In obtaining these elements, the observations were fully cor-
rected for parallax and aberration. The interval embraced by
the observations is 43 days; during this time the planet described
a heliocentric arc of about 17^.
According to these elements, the perihelion distance of this
planet is only 105,440,000 miles, or nearly 23,000,000 miles less
than that of Mars, and only 11,000,000 greater than the aphelion
distance of the Earth. Its periodic time is nearly a year less
than that of any other asteroid. W. J. Hussey.
Astronomical Telegrams.
( Translations, )
Boston, Mass., September 5, 1898.
To Lick Observatory: (Received 9:50 P. m.)
Kreutz announces planet DQ remarkable orbit. Perihelion
within Mars' orbit. Element f*. [= daily motion] 2,000".
(Signed) John Ritchie, Jr.
[A further note on this asteroid will be found on another page
of this number. The telegram included an ephemeris, which is
here omitted.]
Lick Observatory, September 13, 1898.
To Harvard College Observatory: I ^o
To Students' Observatory, Berkeley:) ' '^
A bright comet was discovered by C. D. Perrine, September
13.040 G. M. T., inR. A 9*' 33'- 53'; Decl. + 31° 4'. The
daily motion in R. A. is +6°; in Decl. — 30'.
Lick Observatory, September 14, 1898.
To Harvard College Observatory: i /o .
To Students' Observatory, Berkeley:) ' -J
Comet Perrine was observed by C. D. Perrine on September
13.0404 G. M. T. ; in R. A. 9" 35- 49'.3; Decl. + 31^4' 3i"; and
on September 14.0145 G. M. T. ; in R. A. 9** 41" 43*.8; Decl.
+ 30° 35' 19".
Boston, Mass., September 14, 1898.
To Lick Observatory: (Received 2:10 p.m.)
A faint comet was discovered by Pechule, at Copenhagen,
on September 13.6230 G. M. T. ; in R. A. 6** 38™ 3*.5; Decl.
+ 8° 55' 40". Its daily motion in R. A. is +30'; in Decl.
— 20'. It is probably Comet Tempel, 1866 I.
(Signed) John Ritchie, Jr.
198 Publications of the
Boston, Mass., September 14, 1898.
To Lick Observatory: (Received 9:22 p. m.)
Comet Pechijle is Wolf's comet, not Tempel's.
(Signed) J. Ritchie, Jr.
Boston, Mass., September 15, 1898.
To Lick Observatory: (Received 10 a. m.)
There is some uncertainty in your telegram. First position
does not check. Repeat it. Is comet new ?
(Signed) John Ritchie, Jr.
[In answer to this telegram, part of the telegram of September
14, 2:51 P.M., given above, was repeated with the addition of
the word *'new'* before comet. The telegram on file in the
W. U. office in San Jose was read by the operator and found
to be correct.]
Lick Observatory, Sept 15, 1898.
To Harvard College Observatory:
To Students* Observatory, Berkeley:
Comet Perrine was observed by C. D. Perrine on September
14.9768 G. M. T., in R. A. 9** 47- 36-.8; Decl. 30° 4' 57".
, * >• (Sent 10 A. M.)
ley: )
Lick Observatory, September 15, 1898.
To Harvard College Observatory: (Sent 1:10 P. M.)
Elements and ephemeris of Comet Perrine were computed
by C. D. Perrine and R. G. Aitken as follows: —
T = 1898, October 20.02 G. M. T.
0,= 165'' 17' ^
0= 36 5 V Ecliptic and
( Mean Equinox of 1898.0
^ = 29 1 2 ; ^
natural q = 0.3842
[The ephemeris is here omitted.]
The Perseid Shower of 1898.
Meteors from this radiant became noticeable on the night ol
August 8th. The night of August 9th was partly cloudy, but a
number of meteors were seen in the early part of the evening.
Thin clouds still interfered on the night of the loth, but a larger
number of meteors than usual from this radiant was observed.
After the Moon rose it became clear overhead, and from 14** 25"
Astronomicai Society of the Pacific, ^99
to 14'' 55" fifty-one meteors were counted, of which all but four
were Perseids. This frequency was estimated to be about an
average for the latter portion of the night. C. D. Perrine.
Lick Observatory,
Univbrsity op California, August 16, 1898.
Elements of Comet e 1898 (^errine).
The following system of parabolic elements of this comet has
been derived fi-om normal places for the dates June 16.0, July
12.0, and August 7.0. The observations used in forming the
normal places were: Mount Hamilton, June 14, 15, 16, 17; Paris,
June 16; Strassburg, June 17; Mount Hamilton, July 9, 11, 12,
13, 14; Mount Hamilton, August 2, 4, 5, 6, 7, 8.
elements.
T = 1898, August 16.19978 G. M. T.
n=.259^ 6' i2".2| Eelipticand
« = 205 36 24 .0 \ Mean Equinox 1898.0
/ = 70 I 36 .7 ;
log q = 9.796950
The residuals for the middle place are: —
Observed — Computed,
AX'cosi3' +o".i
A^' —0.9
The comet was last observed at Mount Hamilton on the
morning of August i ith, when it was well into the dawn. It
would not have been visible except for its increased brightness
and sharp nucleus. On August 7th, the nucleus of the comet
was estimated to be nearly as bright as the 9. i -magnitude com-
parison star. The light of the entire comet probably equaled a
seventh- magnitude star. The comet has now passed out of
range of northern observatories, but should be visible in the
Southern Hemisphere for two months yet. The orbit of this
comet bears a resemblance to that of the Pons-Brooks comet
of 181 2-1884. There is also considerable resemblance to the
orbit of the comet 1785 I, especially in w and i. Comet e is so
plainly parabolic, that the resemblance must be considered as
merely placing them in a group, probably with no physical
connection. C. D. Perrine.
Lick Observatory,
University of California, August 25, 1898.
200 Publications of the
Obituary Notice.
Dr. Hermann Romberg died in Berlin on July 6, 1898.
From Professor Backlund's note in Asironomische Nachrichien,
3512, we condense the following brief account of his life and work.
Born in 1835 at Bromberg, he received his university training
at Berlin, coming under Encke's guidance in astronomy. After
a number of years' experience as assistant in several observa-
tories, particularly at Berlin, where he took part in the
observations for the Astronomische Gesellschaft Zone Catalogue,
he was called to Pulkowa in 1873. He here found, in the use of
the large Repsold meridian -circle, which was intrusted to him,
his true field of labor, and for twenty-one years he worked with
the utmost assiduity. The amount of work he accomplished
— 9,000 complete meridian observations a year, in some years —
seems marvelous, especially when the climatic disadvantages of
Pulkowa are considered, and the further fact that these were not
zone observations, but included selected stars ranging in Declina-
tion from — 25° to the North Pole.
His zeal and success in the work of reducing his observations
were equally great, and the fruits of his labors will be found in
three splendid star catalogues. The first of these, based on
32,000 observations made in 1874-1880, is his well-known
catalogue of 5,634 stars. Two further volumes will contain the
observations made in the years 1881-1894. One of these,
including about 20,000 observations, is now in press; the other,
containing 15,000 observations, is ready for the press. These
volumes will form Romberg's most enduring monument.
The key-note of his personal character was a fearless rectitude
that knew no compromise with any form of deception. Convinced
of the truth and righteousness of a given course of action, he
followed it unswervingly, despite occasional unpleasant con-
sequences to himself. With this he combined great gentleness
and friendliness of disposition, and a stanch loyalty to his
friends that endeared him to many.
Astronomical Society of the Pacific. 201
Minutes of the Meeting of the Board of Directors,
held at the lick observatory, september 3, 1 898.
President Aitken presided. A quorum was present. The minutes
of the last meeting were approved. The following members were duly
elected:—
List of Members Elected September 3, 1898.
Mr. W. A. Dawson Horatio, Arkansas.
Prof I A ToLivKT M D \ Director Little Seminary, Mt.
Prof. L. A. JOLIVET, M.U ^ Loretto, S. L, New York.
Mr. Henry B. Loomis, of Seattle, Washington, was elected to
life-membership.
Adjourned.
Minutes of the Meeting of the Astronomical Society
OF THE Pacific, held at the Lick Observato