Google
This is a digital copy of a book that was preserved for generations on hbrary shelves before it was carefully scanned by Google as part of a project
to make the world's books discoverable online.
It has survived long enough for the copyright to expire and the book to enter the public domain. A public domain book is one that was never subject
to copyright or whose legal copyright term has expired. Whether a book is in the public domain may vary country to country. Public domain books
are our gateways to the past, representing a wealth of history, culture and knowledge that's often difficult to discover.
Marks, notations and other marginalia present in the original volume will appear in this file - a reminder of this book's long journey from the
publisher to a library and finally to you.
Usage guidelines
Google is proud to partner with libraries to digitize public domain materials and make them widely accessible. Public domain books belong to the
public and we are merely their custodians. Nevertheless, this work is expensive, so in order to keep providing this resource, we have taken steps to
prevent abuse by commercial parties, including placing technical restrictions on automated querying.
We also ask that you:
+ Make non- commercial use of the files We designed Google Book Search for use by individuals, and we request that you use these files for
personal, non-commercial puiposes.
+ Refrain from automated querying Do not send automated queries of any sort to Google's system: If you are conducting research on machine
translation, optical character recognition or other areas where access to a large amount of text is helpful, please contact us. We encourage the
use of public domain materials for these purposes and may be able to help.
+ Maintain attribution The Google "watermark" you see on each file is essential for informing people about this project and helping them find
additional materials through Google Book Search. Please do not remove it.
+ Keep it legal Whatever your use, remember that you are responsible for ensuring that what you are doing is legal. Do not assume that just
because we believe a book is in the public domain for users in the United States, that the work is also in the public domain for users in other
countries. Whether a book is still in copyright varies from country to country, and we can't offer guidance on whether any specific use of
any specific book is allowed. Please do not assume that a book's appearance in Google Book Search means it can be used in any manner
anywhere in the world. Copyright infringement liability can be quite severe.
About Google Book Search
Google's mission is to organize the world's information and to make it universally accessible and useful. Google Book Search helps readers
discover the world's books while helping authors and publishers reach new audiences. You can search through the full text of this book on the web
at http: //books .google . com/
I
THE SYSTEM OF THE STARS
rr — — *" ~^~T'l ^
11- ^ '
n
/I
— .- •--=- -- -:- '-
u
Plelone.
AtlM.
Sff
+
• «
• .
i^it CWn ol xVft ^
THE SYSTEM
OF
IHE STARS
BT
AGNES M. CLERKE
HOV. mxaBft or thx botal AaTB(utoiucu.i. aocinrr
unam or ' histobt or utrmowmT dokdco tbv minnvxirrH cbvttkt ' Aim
'noasjou or AtmopBTsica'
SECOND EDITION
LONDON
ADAM & CHARLES BLACK
SG-.
'^
»5
*Oj^
TO THK MSHOBT 07
HT r ATHSB
JOHN WILLIAM GLEBKE
WHO DIED IN LONDON
FlBBUABT 24, 1690
FiPTMN years have elapsed since the original publication of
the present work ; and ^teeii years count aa a long spell of
time where sidereal research ia in queatioo* In preparing
the Second Edition, accordingly. I have introduced extensive
modifications. Considerable sectione of the book have been
recaat, and all have been thoroughly revised. New chapters
haye been inserted, old ones have been in large part suppressed.
I^raetic meaBuree of reform have, in shorty been adopted, with
reeolts that certainly Import progress and (it is hoped) con-
stitate improvements. Most of the Illustrations are entirely
new ; and I am under great obLigattonB for the use of valuable
photographs and drawings, among others, to Sir David Gill,
F-RS., to Professor Hale and the University Press of Chicago,
[to the Rev. W. Sidgreavea, S.J., to Professors E. C. Pickering,
Campbell, Barnard, and Frost, &nd to Br. Max Wolf of
PREFACE TO THE FIRST EDITION
SiDBREH. science has a great future before it. The proepects
of its advance are inoalculable ; the poBaibilities of its develop-
ment virtually mfinite. No other branch of knowledge
attracts efforts for its promotion^ at once so wide-spreai3, so
Tariedj and so enthusiastic j and in no other is anticipation
BO continoallf outrun by the brilliant significance of the
reaolts achieved.
For the due appreciation, however, of these results, some
preliminary knowledge is required, and 1^ pofiaessed by few.
To bring it within the reach of ma&y is the object aimed at
the publication of the present volume. Astronomy is
tially a popular Bcicuce. The general public has an
indefeasible right of access to its lofty halla^ which it is all
the more important to keep cleared of unneceaaary technical
impedimenta, that the natural teudency of all sciences is to
become specialised as they advance. But literary treatment
is the foe of speciaiiaationj and helps to secure, accordingly,
the topics it is applied to, against being secluded from the
interest and understanding of ordinarily educated men and
women. Now, in the whole astonishing history of the human
inteilectj there is no more astonishing chapter than that con-
cerned with the sidereal researches of the last half century.
Nor con the resources of thought be more eSectuaUy widened,
or its principles be more surely ennobled through the vision
of a Higher Wisdom, than by rendering it, so far as possible,
iateUigible to all
preiu
■ Tob:
^L^n t]
X THE SYSTEM OF THE STAKS
The following pages then embody an attempt to combine,
in a geneml eurvej, some definite particulars of knowledge
regarding our aidepeal surroundings. The plan pursued has
been to instruct hy illustrative examples, to select typieal
instancea from each claas of phenomena, dwelling upon them
with Bufficient detail to awaken interest and aasist realisation,
while avoiding the tediousness inseparable from exhaustive
treatment. In developing the subject, it seemed best to
proceed from the particular to the general ; to start with
describing the physical constitution of individual bodies, and
ascending by degrees through continually added complexities
of mutual relationships, reaoh at last the crowning problem of
the Construction of the Heavens.
The writer gratefully acknowledges the assistance derived,
in the preparation of the present work, from the kindness of
Sir David Gill, H.M. Astronomer at the Cape, first and chiefly
in affording her an opportunity of observing in southern skies ;
secondly, in reading over several of its chapters in manuscript.
Her thanks are also due to Professor E. S. Holden, to Messrs.
Buniham, Keeler, and Barnard ; to Professor R C, Pickering,
director of Harvard College Observatory ; to Sir William and
lady Huggins, Sir Norman Lockyer, Drs, Vogel, Scbonfeld,
and others for communications of great interest and value.
LoKSOif, Sqitember 2g, 1A0O.
^^^^^H^ ^
1
r cm*r.
PAQK ^1
^^ 1. TuK Tas£ of Sideileal Astho^omt
1
^H S. Ths Methods or Sidzrigat. Rebeahch
12
^H 3. Tb£ StAftR AS Sgkb ....
34
^H 4, ThS CSEMtBTllT OF ReD StARS
49
^H & Gaseous Stars akv KebitIl^
58
f ft. The Teufkhaturbs of tse Stabs
71
^K 7. Teufoiurv Stahs
81
^H 8. Stabs Va^abls in Lokq Periods and Irreoularlt
97
^H 9. Variablk Staha op Shobt E*eriod
ue
F 10, The Coloctm of the RTAitfl . . . .
13&
1 11. DotTBLE Stabs .....
160
1 IS. SraiJiAR Obbits ....
162
^H 13i. Yariable Doube^ Stars ....
176
14. Sfbcteoscofio Binabies
165
lb. Multiple Stara .....
194
16. The Etolotiojt of Mititiple Stars
SOS
17. The Pliiadbb .....
Sifi
^^18. Star Cldstkkb .....
SS7
^^■10. The FoRM.q or NxboLuS ....
£42
F 30, Tke Qseat Nebula ....
267
^^■21. Thk Nature and Chaxueh or Nebula .
872
^HiS. The Distances of the Stars
SB2
^^■£3. Tbanbi#atiok of the Solar Sybteu
303
^HS4. Tbb Pbdfbr Motioks op the Stars
316
^Bs5. T9B MruET Wat ....
333
^V £3. Status of trb Nrbui^ , . . .
349
^B SI. The Conbtructioh of the Heavens
360
^^^^^^H.
1
1.
i "^
TIL
1IV.
VI.
VIL
H.
X-
XL
XII.
xux.
XIV.
H XV.
XVL
XX.
Chart of th« Pleiadei
Photograplied Stellar Spectra .
Types of Stellar Spectra
St«llar Spectra of Three Types
Btell&r Spectm of the Second, Tbird, and Fourth
Tjp^ in the Blue Kegioti .
SputTograiu Qf Nova Aurtgi^ .
Spectrum of Nova Aurigs
Spectm of Temporary StarB ,
The Nehuloaitj round Nova Perael
Spectrum of Alpha Phaeiiicia .
IrreguLar Star CluEtera
Fbotographe of Southern Sidereal Objecta
PhDtogmpha of Spiral NehuliB
Ad Irregular Kebula in Cygnue
Photograph of the Looped, or " Spider "
Nebula . . . ,
Photograph of M«siei 1 1 and adjacent Galactic
CiDnd-formB
photograph of the Key-Hole Nebula .
Tba America Nebula
Perforated Oalacltc Group iu SagittahuB
The Cocoon. Nebula in Cyguus
Franlupisee
To/aae
pa^t 36
44
46
06
00
»l
&4
99
136
fisa
238
S60
n
S64
ses
sso
S70
33a
30E
ZIU
^H^ LIST OF ILLUSTEATIONS
1
^^^P FAINTED EN XH£ TEXT
H
»ir
Tua ^^H
1, Bpectrom of Hydrogen in Wliite Stars (Huggina)
3d I
2. DistritmtioQ of 334 Pi^riods of VarUble Stan
0d
3. Two Consecutive Maxima of Mira Ceti
100
4. BiinimiUD of Miia Ceti, 1902-3 , . . .
101
^^m 5. Light-Curve of R Narmm . . . . .
103
^^B 6. Areas of FACola on the Stm, 1B78-99
104
^H 7. Light-Curve of XS Lupi (limea)
10&
^P 8. Light-Carve of Eta C«liiL», iaiO-1903
loe
i S. Oorve of Sun-spot Frequency, 1867-77 (EKiH)
113
^^-10. Distribution of 80 Variable Star Periods under 20''.
117
^^■11. Lighi-Ciirve of Bdta Cephei . . . .
118
^^■IS. Typical LtghtrCnrvee of Cluster VariAblea
119
^^ns. Light-Curve of No. 45 Omega Centauri
120
^^|l4. Light'CoTTe of 8 Ane , . . .
ISO
^^bs. LitjhvCarre of U Vulpecuhe
12*2
^^^ 16. Ligbl-Cur\ie of Beta Lyrae (Argelander)
122
^^17. Ligbt-Curv« of V Pttppie
123
^Kl8. TAgh|>CarTefi of Five Algol Stars
1B4
^V Id. Syttem of R^ Centauri (Roberta]
125
^^K to. Algol duricg an Eclipee
1£9
^^ftsi. MmiiQum of S Cancri ....
131
^^HS2. Apparent and Real Orbits of Alpha Centauri
164
23. Four Double Btara photographed at Patifi (llottche^, Phota
graphii Aetrvnomiqw) . . , ■
166
24. Orbite of the Component Stars of Gkunma Virginia .
173
26. Orbits of tbe Compotieut Stars of Alpha Ceutann
174
_ 28. Orbits of Siri ue and its compMiion .
174
^^■27. Stars of the Trapezium ....
206
^^H
1
CHAPTER I
THE TASK OF SIDEEEAL ASTRONOMY
When all the stars blaze out on a clear, raoonleBs night, it
seams as if it would be imposBible to count them ; and yet it
is seldoEQ that more than 2000 are visible together to the
unaided eye. The nuiober, however, dependH very much
upon climate and Bharpneas of sight. Argelauder enumerated
at Bonn, where rather more than eight-teuths of the sphere
come successively into view, 3256 stara." But of these no
more than 2000 could be, at any one time, above the horizon,
and BO many would not be perceptibly above it, owing to the
quenching power of the air in its neighbourhood, Heis, with
exceptionally keen sight, distinguished at Miinster 1445
more stars than Argelander had seen at Bonn-, ^ Houzeaa
recorded 5719 at Jamaica;* Gould 7756 within lOO*" of
the south pole at Cordoba in South America.* The die-
crepancies of these figures are due to the multitude of email
stars always, it might be said, hovering on the verge of
ibility. If, indeed, the atmosphere could l)e wholly with-
iwn, fully 25,000 stars would, according to a trustworthy
stimate, become apparent to moderately good eyes,^
Our system of designating the stars has come down to us
Trom a hoar antiquity. It is a very emljarra&sing one. " The
jostellations," Sir John Her&chel remarks," *' seem to have
^ Dtanomttria AVma, 1649.
* Hiiu, De MhffHiiitdim NuJtierofjue Stellarwn, p. 16, 1^52.
» Uranuivtitrit OSrUrate, Anoalea de I'DUwrvatoire de BraselUB, t. i, 1678.
* VratitowLctria Argentina^ 1879,
* BtckhouAe* Jottr/iat Livtrpool Aair. SoeiA^, tqI. rii. ii. 33ti.
* TrtiUUe on Jsironfrnj/, p* 168. ni4e.
I
THE SYSTEM OF THE STAES
been almost purposely named aiid delineated to cause aa
much confusion and inconvenience a» possible. Innumerable
snakea twine through long and contorted iirEyis of the heavens
where no memory can follow them ; bears, lions, and fishes,
large and small, northern and southern, confuse all nomen-
clature." And yet we could ill afford to dispense with the
picturesque associatioue of a menagerie, largely stocked from
the banks of the Euphrates. The signs of the Zodiac, which
are undoubtedly of Chaldean origin, embody legendary cycles
of thought already, some four thousand yeara ago, the worse
for the wear and dilapidated by time. Homer and Hesiod
were familiar with the Bear, Arcturue, and the Bog-star, with
" the Hyades, and the Pleiades, aud the strength of Orion."
The Little Bear was introduced from Phcenicia, when the
Pole-star became the mariner's " cynosure." Finally, a number
of individual stars have Arabic appellatiouB, dating from the
epoch of Saracen supremacy over science. Thus " Vega " the
current name of the brightest star in the Greek coasteUation
of the Lyre, is the remnant of an Arabic phruse signifying
the " Falling Eagle," while " Altair " stands for the " Flying
Eagle ; " " Deneb " means the Tail of the Swan ; " Fomalhaut "
the "Mouth of the Fish;" "Eigel" in Orion is the Leg,
■' Betelgeux," the " Shoulder of the Giant " and so on.
The constellations * now generally recognised are eighty-
six in number, of which forty-eight are found in Ptolemy's
" Almagest," From Ptolemy, too, is derived the method of
classifying the stars by " magnitudes " This ia a most in-
appropriate term, since none of the stars have any perceptible
dimensions, Tht-y are literally what Shelley calls them,
" atoms of intenaest light "- — ^globes shrunken by distance to
the semblance of mere shining needle-points. Our own sun,
removed to the place of the nearest fixed star, would be in
the same condition ; contracted to xt^"^ ^^^ diameter would
be utterly inappreciable with the largest telescope. It is
true that the telescopic images of the stars appear to
be of meaaiirable size ; but this is a purely optical effect,
and the " spurious discs " shown by them actually grow
' For an eaaj method of identifying the cti&f northern atars, aee Sir Robert
Bill's Story of the HoavftiSt p, 37 'J ; »1bo the ' * Urauograpljy " itx Vouug't
£iementt 0/ Astnmomi/, 1890.
THE TASK OF SIDEREAL ASTRO>'OMV
em^er instead of larger aa the power of the instrument 18
increaeed,
'• Magnitude " has, then, nothing to ili> with apparent ai^e,
but refers entirely to apparent lustre, ^^bich depends upon
distance and intensity of shining^ as well as upon actual
{l]aien0xon£L The fainteet Btara have the highest numerical
magniCudes; and it has been found that the gap between each
mujoefiBive order^ as represented by the atars traditionnlly
belonging to it, corresponds to a falling-off of light in the
proportion of about 2^ to 1 . The arrangement by magnitudes
js> of couTBe, entirely arbitrary ; natural gradations are not
by a flight of steps, but along an inclined plane. Stars classed
48 of the first magnitude (of which there are ten in each
bezzkiephere) ^ differ accordingly very mudi among themBelvea.
Sinus exceeds Eegulus no less than fourteen and a half times ;
Vega is more than twice as brilliant as Aldebaran, Vega,
CupelJa^ and Arcturus bold a co-ordinate primacy in the
Borthem hemispheiv^but are outshone in the southern by Sirius,
CanopU£, and a Centauri. Of second magnitude are the seven
stars grouped to form " Charles's Wain," the Pole-star, and some
of the ujOHt vivid gems ia Perseus, Cassiopeia, and .the Swan.
Stars of the sixth magnitude are the faintest ordinarily visible
to the naked eye; but those of the seventh can be seen under
advantageous circumstances. The plan, introduced by Bayer
in 1603, of naming the stare of the several constellations
roughly in order of brightness by the letters of the Greek
alphabet, established for each a kind of liglit-sefiuenoe, useful,
though far from exact. The Buialler stars are usually dis-
tisguished by the numbers attached to them in various
GAbilogues.
One of the most notorious circimi&tanceB about the stars
is their "twinkling/' They undergo, especially when near the
bomoQ, extremely rapid changes of lustre^ attended sometimes
by the glinting of prismatic colours. Nor do all stand, in this
reepect, on the same level White stars twinkle more than
rud onea. Even early and untutored observers noticed how
Tbe fieiy Sirius altera liue,
And bickers uitc> red and emerald.
*■ S«e Airpendis, T&ble I.
4 THE SYSTEM OF THE STAES
whence it was called by Aratus itokiXot-, the "many-coloured";
and chromatic unsteadiness was a marked peculiarity of the
" new stars " of 1572 and 1604.
It is easy to see that tbifi effect ia in Bome way due to the
atmoaphere. Like Tefraction, it vanish^ at the zenith ; it
varies in intensity with weather and climate. The first
i&tional conjecture as to its cause was made in 1667 by
Robert Hooke, who attributed it to iixegular refraction in the
various air-strata. More exact Lnquiriea on the subject have,
in recent times, led to some curious results.
The impressions of light on the retina last, according to
Plateau's c&ieful determinationj 0*34 — say one-third — of a
second. This is the limit of their individual perceptibility.
With more fi^uent recurrence, they become mei^d indis-
tinguishably together. But the changes producing scintillation
succeed each other much more rapidly than three times in a
second Hence the need of some means of separating and
(laalyeing them.
These were provided by M, Montigny's " scintillometer," ^
in which the sensibility of different parts of the retina was
skilfully turned to account for the registration of a swift
aoocdasion of impr^sions. By the rotation of a glass-plate
obliquely inserted in front of the eye-piece of a relracting
tele*;ope, the image of a star viewed with it is made to
describe an exact circle in the geld. The line of light traced
out is, in perfectly steady air, continuous and of a uniform hue,
but breaks up, under the influence of scintillation, into vividly
tinted arcs, at times into prismatic " pearls." The addition of
a pair of crossed wires facilitates the reckoning of the colour-
fluctuations thus rendered separately visible; and they are
found to occur, on an average, in white stars standing thirty
degrees above the horizon, seventy-eight times in a second, in
yellow and red stars similarly placed, sisty-eight and fifty-six
times respectively.^
The explanation of these appearances is evidently to be
sought in the refractive power, combined with the turbulence
1 Described in £wU<iin de I'Aead. dt* Sciirux4, Brusefks, t. xvii. p. 261,
2tid actha ; MoniAty Nttiiiet, to], xxxirii, p. 203 ; Ci<i ft Ttrrt (FievflE), t. i.
p. 30&.
^ BiiU. d* VAead. firuxellca, t Jtijcvii. p. 185. 2iid Khes.
THE TASK OF SIDEREAL ASTRONOMY
of our aedftl envelope. For a different path through its strata
ia neoeasarily pursued by each of the differently refrangible
beams united to form the itnage of a atar. The violet ent«ra
them higher up, eiuce it is more bent in transit tlian the red ;
and &o proportionately of the rest. Each then ia liable to
^^mcouBter different vicissitudes on the way, betrayed to our
^Bght by rapid flashes of colour. Each is affected by innumer^
^Blle small deviations and momentary capncea of refraction ;
PHb that the bundle of rays picturing a star at a given instant
jjt, as it were, a fortuitous and eminently unstable combination.
It id dissolved, and a new one constituted, sixty or seventy
titD€s in a second ; and the elements temporarily missing
determine the reeultiug tint. The fundamental fact of the
matter, in short, i8 that the light of every star near the
horizon is drawn out into a tiny spectrum by the chromatic
dispersion of the atmosphere ; and Respighi's study of the
^actuations in these prismatic images ^ provided, accordingly,
^^le ifirsct secure basis for a scientific theory of scintillation.
^B That white twinkle more than red stats becomes intelligible
^^■ben we consider that the sheaf of their beams being fuller,
^^Kteroeptiona of them are more frequent But planets which
are radiating discs, and not merely points, rarely show the
effect, because the absence of rays from one part is compeasated
by the arrival of rays from other parts of their surfaces.
Similarly, the steady radiance of stars in large telescopes ia
k^ie to the neutralisation of each casual stoppage by the
P^^eat number of the beams collected together. Instead of a
twinkling image, however, a blurred and distended one is
formed under perturbed conditions, and observation gains
nothing by the exchange. And since the degree to which this
phenomenon is present varies very much with locality, regard
should be had to its prevalence in choosing ^ sites for power-
jil instruments. It diminishes, on the whole, with altitude.
it the configuration of adjacent mountain-ranges is strongly
uential, and Dr. Pemter found Sirius actually to scintillate
^ Le* Monda, t lix. p. 6S8 {isa&) \ Lard Rayleigh, Phil M'ag. toL xxxvj.
> 129, 1»03.
' ExDCTf Attr, Xtteh, Tjlo. 37$! ; A. E. DouglaflB, Fopttlnr Aatronontt/, Jwae
' ; I«oweU, Monthly Koti«s, Tol< Ixiii. p> 4D ; Eincr abd Villiger, Mtroph.
Jowm. vqL xxL p. 36S.
THE SYSTEM OF THE STABS
more at the summit than at the foot of the Sounblick (10,C
feet high).^
Scintiltatioti, like astronoooical refmction, augments as the
thermometer falls and as the barometer rises. Thia is inevit-
able, since the first requisite for its occurrence is differential
refractiTe action on the various Ught-rays,* But it haa other
leas obviously accountable meteorological relations. M.
Montigny ascertained, by the experience of nearly forty years,
that with the quantity of moisture in the air the twinkling
of the stars increases so markedly as to serve for a useful
pTOgnostic of rain. Cyclonic conditions promote it;^ and it
is extremely sensitive to magnetic disturbances.* Useher was
struck, in the eighteenth century, with the surprising vividness
of scintillation during aurorse ; Montigny extended the coincid-
ence to magnetic commotions perceptible only iuatrumen tally.
Moreover, Weber remarked at Peckeloh in 1880, that stars
aitoated near the magnetic meridian twinkled more than
elsewhere in the sky;^ and although little attention has of
late been paid to the possible dependence of the effect upon
the points of the compass, yet the theoretic-al interest of
scintillation would be much enhanced should it turn out to
be one of the many terrestrial phenomena associated with
vicisaitudes in the physical condition of the sun.
The world of stars thrown open by the teleaoope may
fairly be called boundless. Using a glass only two and a half
inches across. Argelander registered 324,189 down to 9i
magnitude, aU in the northern hemisphere, with the addition
of a southern zone one degree wide. The work was extended
to the southern tropic by Schonfeld, and completed to the
southern pole under Sir David Gill's direction. At the Cape,
the photographic method was employed, and the resulting
enrolment, published 1896-1900, comprises 454,875 stars
nearly to the tenth magnitude; while the Cordoba visual
Dnrchmuaterung, executed by Thome and Tucker, 1835-1904,
is a still more comprehensive register of southern objects. Yet
* Obttrmtory, rol, lii, p. 1&4.
* Montigny, Bull, de I'Acad, BrunBUeft, t. xlri. p. 813, 2t]d senea.
' Roaentlial. Meicor. 2iitschr\/t, Bd. xi. p. 145.
* CQmpltf R*nd%tMt t. icvi* p. 673-
' lyoehtntchr^t/tlr Astrtmmut, 1360, p. 2&4.
THE TASK OF SIDEREAL ASTKONOMY
greftt works are merely preliminary to the International
'chartJBg opCTationa in progress. Their accomplishment will
yi«ld a " Catalogue of precision " including at least three
million stars; aad somewhere about thirty millioas, taken
from the submerged population of space^ will, by their record on
the chart-plates, be admitted to the citizenship of astronomy.
They can never thenceforward be excluded from the scope
of research* Their light - changes, their movementB, their
distribution, will present an inexhaustible, and probably a
moot fruitM field of inquiry.
Mr. Plommer showed in 1877^ that the lucid atare (those
visible to the naked eye) in the Bonn Durchmusterung give
as mach light as 7349, the telescopic stars as 23,337 sixth
magnitude atara Those singly imperceptible thus really
illuminate the sky just three lirues more than those in-
dividually seen. Stamaing up, with the aid of the beet
photometric data, the entire light of Argelander's 324,000
atara, we get for its equivalent j^ full moonlight ; and we
y roughly estimate the total light of all those similarly
inumerated in both hemispheres, to the number of about
900,000^ at -pj^ the lunar brightness. The amount of
scattered effulgence dispensed by still fainter stars is exceed-
ingly difficult to evaluate. Sir William Abney, using a
photographic method, rated in 1896 the sum of starlight in
both hemispheres at ^iv ^^ moonlight. Professor Newcomb,
in 1901,^ from visual observations of diffused sky-radiance,
condaded the light-power of all the stars to be just 723 timea
that of CapeUa;* and 728 stars like Capella give ^ the
light of the full moon.* But it is far from certain that the
I T anlt of heaven would seem absolutely black if the stars were
^^lotted out.^ Our tipper air is the seat of processes by which
^^■iniinosity is at times strongly developed ; and we cannot be
^^pore that they are ever entii'ely suspended. Hence, Frofe&aor
[ Kewcomb's experiments ajford no assurance regarding the
^^H 1 Monthly J^fotias, vol, xxxvii. p, 43(3.
^V ^ Astrophytioil Jtmrnal, vol, xiv. p. 310; see iho OaTla J. Buras, ibid^
ToL iri. p. 169.
' Newomab'B 600 stars a{ O'O fflftgnttude are «qatl to 723 of th« pbQtoniBtriQ
bright&6» (0^1] 4f CApeUft.
* VmtT, flictomarit dtr Qt^TM, p. 340.
■ Cf. Bttrn», Jov.rn. BrU. Aatr, Au. toI. iv. p. 91.
8
THE 8TSTEM OF THE STABS
iiudividi^B
eqoiTaleat, to mf *****^f d Urn mitml BiuiLct of itaa
oomuig dinctfy, or iadtnetly wHfata o«r fcea. Thaae last caa-
QOt well &U ifaat of ntj ™ittwT«_ aad tbej m«« profaablj
mun 1^ to OBie hazidred aillioBo; bat tbe aet* of iDqaiij can
at prueeDi scmroefy be djswn ckser Yet tbe foot io Doto-
worth^ that each clan of stsn sendi itt ^ppncnl^ more
light tban tbe dam next sbofv iL Tbe I^it-Aggx«g«ta of
BBOond magmtode ttaxs exeeeds that 'of ink, of third that of
aeooud, and so oil Tbe ftinter tbe aUzs, in sbortj tbe gieatcr
is their total luminooe power/ >iw»iiiift their
uumbers more than «yMin t .f*' t;Miti^"fg tb^r diniiiiiabed i
lufiti^ But this pfogreanao, it is eridetit^ caanoi go on
iodefiuitelj, EJoce otbenrise an indtifinitelj inteoae radiaaca
would fill tbe sky. Daricnen wonld be abolished through tbe
fihiaing of invisible stara. It £ollo«a other Uiat tbe obeerred
order of the etellar vorid baa aaagnabk limits — that the alar-
depths, however proloand, are not abaolotelj tm&tbomable ;
or that space, for whaterer reasoo, is not abeolately tiaaspareat
The Laak of exploration, at anj rate, does not aeem to be
altogether hopeless. It can neTer indeed be exhausted; bat
it can fairly be grappled with by finite minds. It does aofc
evade their efibrte with the paasve ecom of material infini-
tude. Geauine. if partial, saooeases have otiwned them in the
pastf and will, it may be hoped, continne to ciowu ihem in the
future.
We must not. however, in seeking enconittgement from
the thought that it does not utterly defy oor powera^ under-
rate the difficulty of the enterprise we have taken in hand.
Tbe nature of our own sun oflers a vast and intricate problem,
still very far from being solved ; but stellar epoce contains
many millions of suns, variously couEtituted, varioualy circum-
atanced, frequently snrpaesing our magmficent orb in size and
splendour. Now each of these millions of suns challenges
the closest pergonal attention ; no single one of them is
exactly like any other, and their diffcrenoee and resemblances
open endleaa vistas of instruction and interest. Their incon-
ceivable remoteDese in no way derogates from their real
dignity. An all but evaaescent speck of light in the field of
the great Lick refractor may bo the life-giving centre of a
* L*AttTonoini*t t. v, p. 400*
THE TASK OF SIDEREAL ASTROXOMY
of worldB, each aboanding as manrelloudj vitb proofs
of creaiiwe wisdom and goodness aa tbe little planet in which
our tempoml deetuues &re imprisoned. Such ligbtr-specks are
Aea equally deeerring of stody with tbe moet effulgent orb«
in the ekj, although it may never be practicable to bestow it
apoD them. We can indeed hardly imagine the amount of
teleBOppic improrement which would be needed in order to
hnng them within the range of critical examination. For
the preeent, accordingly, physical research must be confined
to eome thonstuids of the brighter etare which may serve as
Bpecuneiu of the rest. Nor need we lament the restriction.
GenerAtioiiS of workers migbt expend their energies in
^tbering facta from the field actually open to them, and
yet leave a fiill harvest for their successors. In all ei-
perimentAl inquiiies, it may with truth be said that the
reaper, aa be gamers one crop of knowledge, sows another :
Bo endless are the secrets of nature, ao untiring the inqniai-
ivenese of man.
The »tars in their combinations demand inquiry no less
■n the stare in themselves. Stellar systems are to be met
with in indescribable profusion and variety^ from mutually
drcUng pairs, through groupa including thousands of phyei-
caUy related objects, to tbe stupendous integrated collection
which we call the Milky Way. But as yet investigation has
barely aldrted the edge of this well-nigh infinite region. Before
■^ can be penetrated by so much as a plausible conjecturej
BMtati»tics are wanted of the distances and movements of
r thousands, nay millions of stars.
I Nor is the amassing of them any longer the Sisyphean
I labour it seemed a short time ainca By the unhoped-for
development of novel methods, the pace of inquiry has been
qoickened all along the line. Particulars are accumulated
faster than they can be assorted and arranged. Time has
virtually expanded, as if for the purpose of gratifying curiosity
^^phich becomes keener a3 its sublime objects loom more
^Histtnctly above the horizon of thought Ten years now
connt for a century of the old plodding advance. Express
trains carry passengers on erraada of research, aa well as of
btmnesa or pleasure. Problems ripen as if in a forcing- bousej
and 80 numerously as almost to bewilder tbe attention.
THE SYSTEM OF THE STAPS
The whole sabjecc af ddereal natural historx ia
and intricat« beyond wbAt il is eAsy to coarej to the
approaching it for the fitBt time. TheT« ia ac»rcely a topic iti
physical aHtronomy with which it is unconcected. The pro-
gress of discovery has giadtially drawn ctoaer the geuenc
relationships of the hearenly bodies The mm has oome to be
recognised ns the grand exemplar of the Atars ; meteoritea
show themseWes to be intimately associated with comets ;
comets are perhaps the shreds of uaed-np nebnlfe ', while the
stellar and nebular realms blend one with the other aa indift'
tinguishably as the animal and vegetable kingdomB of organic
nature.
The strange cloud-like objects called "^ nebulie " may be
considered as wholly of telescopic revelation. Only one of
them — tlie famous object in the girdle of Andromeda — can
be at all easily seen with the naked eye ; and even that
escaped the notice of aU the Greek, and most of the
mediseval astronomers. The " nebuloase " of the ancients
were many of them small groups of stars accidentally set
close together ; but among the seven enumerated by Ttoiemj
were two real clusters like the Pleiades, only (presumably)
much farther away, one in Perseus, and the other in Cancer.
Indeed, to extremely ehort-aighted persons, the Pleiades them-
selves put on a nebulous appearance, the individual ertars
nmning together into one wide blot of light
Halley was the first to form anything like an adequate
conception of the importance of nebular observations. He
was acquainted in 1716 with six -'luminous spots or patches,
which discover themselves only by the telescope, and appear
to the naked eye like small fixed stars ; but in reality are
nothing else but the light coming from an extraordinary great
space in the ether, through which a lucid medium is diffused,
that shines with its own proper lustre." ^ Only two of Halley's
half-dozen objects, however — those in Orion and Andromeda —
were genuine nebnke ; the rest when viewed with better instru-
ments than hia " six-foot tube," proved to be magnificent star
clusters.
This small beginning of knowledge was followed up by
Lacaille in the southern, by Messier in the northern hemi-
^ Phil. Trafit, vol, izLi. p. 3»0.
THE TASK OF SIDEBEAL ASTRONOMY
11
ilibere. Then Hencbers great tdescopes opened the modem
epoch in the sciesce of nebole. A» the result of his labours
thef came to be reckoned by the tbooeaud instead of by the
Kore. Portioofi of the Eky were foand to be crowded with
them. Yet the vaat tnajoritj must always, owing to their
^ctzeme faintness, remain imperceptible without powerful
opCiical Aid, only sixty-four coming into view with the same
tfllaoeope which showed Ar^lander 324,000 atara. Thua
Aeoees to the nebular heavens can be gained only by making
the yerj most of the little light they send iia> I^u-ge
teleeoopes and prolonged photographic exposures are indeed
pie-eminently uBeful in this department of celestial phyBic8»
which, mainly through the application of the camera, has of
late incalculably widened A pioneering survey with the
Crosaley reflector led Profeseor Keeler to estimate at 120,000
the number of nebulae which might be chemically recorded by
it8 meftns ; and the specimen sheaves garnered by Dr. Max
Wolf at Eomg;3tuhl in 1901 are no lees promising for a rich
future harvest. But discoveries are of email account if
Bucceeded by neglect. Assiduous and prolonged observation is
indispensable for the detection of the cyclical or progressive
changes doubtleas proceeding in these inchoate systems.
This then is the task of sidereal astronomy — to investigate
the nature^ origin, and relationships of 30,000,000 stars and
of 120,000 nebalse — to inquire into their movements among
themselves, and that of our sun among them — to assign to
each ita place and rank in the universal order, and, gathering
hinU) of what ■ has been and what will be from what is,
distinguish hierarchies of cele.^^tial systems, aud thus at last
rise to the higher eynth^is embracing the grand mechaniBm
of the entire — the sublime idea of Omnipoteuce, to which the
stars conform their courses, while " they shine forth with joy
Him that made them."
CHAPTER II
TEDS HXTHODS OF SIDEREAL BXSEAItCH
Sidereal science is, on its geometirical side, of modem dfiTekip-
ment ; on its physical side, of modem origin. The places of
the stars, as referred to certain lines and points on the sar&ce
of an imaginary hollow sphere, are obtained now on eaaentiiiUy
the same principles as by Hipparchus, only with incompazaUy
greater refinement And refinement is everything where the
stars are concerned. Significant changes among them can
only be brought out by minute accuracy. To a rough dis-
cemment their relative situations are immutable; and
systematic inquiries into their movements hence became
possible only when the grosser errors were banished &om
observation. Bessel's discovery of Bradley's exactitode gave
the signal for such inquiries. It seemed worth while to re-
observe stars already so well determined that discrepancies
might safely be interpreted to mean real change.
Thus it is only within the last hundred years that the
stars have been extensively catalogued for their own sakes
and no longer in subordination to the interests of planetary or
cometary astronomy. The scope of such labours now widens
continually. For the objects of them are all but innomerable,
and the inception of ambitious schemes is encouraged by
modem facilities for executing them by combination. The
project set on foot by the German Astronomical Society in
1S65 of fixing the precise places of stars to the ninth
m^nitude. found co-operators in all parts of the world ; and
it« virtual completion in 1903 to the verge of the southern
zones obseiTod by Qould and Gilliss* raised the number of
stars not mer>L^ly rooordoil. but known in the strict astro-
metrical sense, to not far from 400,000.
19
THE METHODI
IDEREAl RESEARt
A star is located in the LeaTens, just as a city or a
oimtain ie located on the earth, by meaaurements along
two imaginary circlea. Its " declination," or diBtance from
the celestial equator, corraaponds to terreatrial latitude ; its
'■ right ascension " to terreBtrial longitude. The astronomical
prime meridian passes through the first point of Aries» that
is, the sun's position at the vernal equinox ; intervab from it
reckoned eastward &om 0"^ to 360"*, or in time from 0*^ to
And since the zero-point retreats slowly westward by
the effect of precession, it follows that the right ascensions
of moat stars increase steadily year by year, apart from any
moTementd " proper " to themselves.
The diurnal revolution of the sphere furnishes the sole
standard of time in sidereal astronomy. Sidereal noon at a
given locality is the moment when the first point of Aries
crosses the meridian of that spot; the right ascensions of
the heavenly bodies indicating the order of their successive
culminations. Thus, if the right ascension of a star be two
hours and twelve minutes, it ^ill cross the meridian of any
place on the earth two hours and twelve minutes after the
first point of Aries has crossed it, coming up behind it, to that
extent, in the grand diurnal procession. Differences in right
aaoeuBion signify differences in times of culmination ; and
tbeii measures in hours, minutes, and seconds need only multi-
plication by fifteen (the number of times that 24 is contained
in 360), to appear as measures of arc in degrees, minutes,
and ^seconds.
A transit-ciixle and a clock are the two essential inatru-
tnenta for ascertaining the places of the stars. The instant,
to the tenth of a second, at which a star stands in the
meridian, is noted ; the vertical circle is read, showing its
"aenith -distance" (giving at once its dechnatiou when the
latitude of the observatory is known)> and the observational
part of the work is done. The data thus obtained, after
idergoing numerous corrections, aufi&ce to determine the
ition of the star with reference to some other " funda-
mental " star, the ahsobde place of which has been separately
and laboriously ascertained.
This business of star-location forma the substraturo of the
older astronomy. But the precision given to it ia altogether
THE SYSTEM OF THE STABS
new, Bod alone has fitted it to be the meana of eliciting facts
80 coy aa those that relate to stellar niovementa. For their
diacloaure devices of accuracy are needed which our astro-
nomical progenitors never caat a thought upon. Optical and
mechanical skill has, in our days, reached a point of almost
ideal perfection ; yet when the artist has done his utmost, the
instrument is» in a sense, still in the rough. The astronomer
then takes it in hand, and his part is often the more arduous
aad anxious. The investigation of small surviving errors, the
contrivance of methods for neutralising their effects, the carry-
ing out of delicate operations of adjustment* the detection of
microscopic detbrmatioD3, tremors of the soil, inequalities of
expansion hy heat, fall to his share. Even his own rate
of senBe-transmiseion has to be measured ^ and figures, under
the title of " personal equation," as a correction in the final
result. For, between the actual occurrence and the perception
of a phenomenon, there is always a gap, more or less wide,
according to individual idiosjoicrasy, and it is only after this
gap — tiny though it be — has been crossed, that electricity can
he called upon to play its prompt part as amanuensis to the
observer.
This detailed and painful struggle against eiTor has
made sidereal aatronomy possible, by pr€cipitatinff from the
mixed solution that held them the minute quantities it deals
with. Just because the universe is almost infinitely large,
these quantities are almost infinitely small They are small,
not in themselves, but through the incomprehensible remote-
ness of the bodies tliey affect.
Sidereal astx-onomy is deeply concerned with the motions
of the stars. These are of different kinds. " Proper " motions
— so-called to distinguish them from " common " apparent
displacements due to the slow shifting of the points of refer-
ence on the sphere — advance uniformly along a great cirele ;
orbital revolutions of one star round another are periodical in
small ellipses; besides which annual oscillations, varying in
extent with the distances from ourselves of the objects per-
forming them, are barely measurable in a few of the nearest
stars. The perception and characterisation of these orbital
and " parallactic *' movements have become possible only
through the attainment of exquisite observational accuracy.
J
THE METHODS OF SIDEKEAL RESKAECH 15
rbe JDstrunients employed are the equatoieal with micrometor
Attached^ and tbe heliometer.
An equdtoreal la a telescope so mounted as to follow the
diurnal Eevoltktion of the heavens. It i^ coimected with an
ftXJB directed towards the pole, and revolving by clockwork
oooe ID twenty-four hours. An object accordingly once brought
into its field of view remains there immovably for any desired
time, provided the tube be clamped in position^ and the clock
3et going. The inconvenience of the earth's rotation in pro-
ducing a continual ** march-past " of the heavenly bodies id
thus neutraliged.
To the eye-end of an eqnatoreal is uenally attached mi
arrangement of spider lines constituting a " filar micrometer."
Two sets of Buoh threads (which in subtlety and evennesa of
texture far surpass any artificial product), crossing at right
angles and some of them movable by fine screws, while the
whole can be made to revolve together^ afford a most delicate
means of ascertaining the distance and direction from each
other of any two objects close enough for simulumeous
obeervation. Mea-stixes of double stars are executed^ and some
stellar parallaxes have been determined in this way. But for
the latter purpose, the " beliometer " is the more appropriate
instrument-
Its designation is a misnomer, or rather represents the
tradition of an original purpose to which it was never effec-
tively applied. The true function of a hebometer is tbe
critical measurement of two adjacent stars, or of a star and
planet. Primarily, it is an equatoreal telescope ; its micro-
gtrical powers are conferred by the division of the objetjt-glass
Btu two halves sliding along their common diameter, and
duplicating by their separation the combined image formed by
them when together. The amount of movement igiven to the
segments in bringing about alternate coincidences between
opposite members of the pair of atars shown by each, suffices
to determine with the utmost nicety the interval between them.
That is to say, after endless precautions for accuracy have
been taken, and endless care bestowed upon detecting and
obviating occasions of infinitesimal error.
The Badeliffe Observatory at Oxford possesses the largest
heliometer in existence* Tbe diameter of its object-glass ia
16
THE SYSTEM OF THE STAES
Beren and a half inches. A siiuilar idstrument, however,
erected at the Eojal Obaervatory, Cape of Good Hope, nearly
fortj years later, ia but slightly inferior in size, and is in other
respects considerably its superior, Dr, Elkin, at Yale College,
haa charge of the only hetiometer in the Kew World, while a
good many are to he found in Germany and Huseia. The
Kepsolds of Hamburg may he eaid to bold a monopoly in the
mechanical part of their production ; and Merz of Munich
stands almoet alone among opticians in bi3 readiness to take
the responsibility of sawing a fine object-glass in two. Nor
is the aptitude for the use of these instruxnenta by any
ni^ns uniyersal among observers ; hence theii' comparative
scarcity
The science of the motions of the stars is only a part of
modem sidereal astronomy. Within the last forty years a
science of their nature has in defiance of forecast sprung up, and
assumed surprising proportions. Sidereal physics has a great
future in store fot it. Its e^cpausiveneas in all directions ie
positively bewildering. The " What next ? " is hardly asked,
when it is answered, and often in the least looked-for manner.
In following its progress, the mind l>ecome5 so inured to
novelties^ that antecedent improbability ceases to suggest
dissent. Some details of what we have thus so far learnt
will be contained in the ensuing chapters ; the means employed
must be briefly indicated in this.
They are of three principal kinds — spectroscopic, photo-
metric, and photograpliic. The general theory of spectrum
analysis has been explained elsewhere ; ^ here we need only
repeat that it rests upon the constancy of the positions in the
spectrum belonging to the taya of light given out by ignited
vapours. These invariable lines serve as an index to the
presence iu the sun or in a star, no less than in the laboratory,
of the substance they are associated with. Whether they be
bright or dark, the principle remains the same. They are
bright when the vapour originating them is the chief source of
illumination ■, dark, when a stronger light coming (rom behind
ia absorbed by its interposition. Their appearance as " lines "
is merely due to the transmission through a narrow slit of the
light afterwards priamatically dispersed.
^ 8«e tlie AQthor's Hittory t>/ AxlrOTiomy. 4th edit. p. 189.
^k
THE METHODS OF SIDEREAL RESEARCH 17
Ifow a main difficulty in getting starlight to disclose ita
secreta^, is that there is so little of it. It will not bear the
Dficessarj amount of spreading -out, but evades analysis by
&dinig into impei-ceptibility, like a runnel of water that widens
only to disappear* Hence the absolute neoesaity in stellar
spectroscopy for large telescopes. The collecting aeta have to
be widely extended to gather in a commodity so scarce. Could
we at all reaUse, indeed, the portentous expanse of the evet-
broade&ing sphere filled by the stellar beams as they travel
_towardB vm, we should be inclined to wonder, not at their
itneaa, hat at their intensity. Bat the weakening effect of
^diatattce is in some degree counteracted by powerful concentra-
tion ; and this is one of the chief uses of the large telescopic
apertureB bo much in vogue at the present time.
Viewed with the lick refractor of 36 inches, any given
Btar 18 32,400 times brighter than it appears to the naked
eye, or 324 times brighter than when shown by a 2-inch
telescope.* The large inBtrumentj that is to say, provide*
324 times more material for experimenting upon, or raages
further by 6^ stellar magnitudes than the small refractor.
The interpretation of spectral hieroglyphics, by which we
Jearn the chemical coostitution of a star, is a very delicate and
iborious operatioa What is called a " comparison-specDrum "
usually employed a*? an adjunct to it. Rays from some
terreetrial source are reflected into one half of the sUt, through
tht! other half of which the stellar rays are admitted. Both sets
then traverse the same prisms, and form strictly comparable
Spectra side by aide in the same field of view. Lines common
to both can thus easily be identified ; and their genuine occiir-
recce leaves no doubt that the element compared^hydrogeu,
sodium, iron, magneaium, or any other^ — enters into the com-
position of the star. But this process of matching can st^Mom
or never be completely carried out. A dozen known lines
may be attended by a hundred unknown onee, either too faint
to be distinctly seen^ or in positions unfamiliar to terrestri»l
light -chemistry. Nor is it safe to infer the absence of an
ingredient from the absence of its representative rays. Many
caufies contribute to render the display of lines in sbolkr
ctra selective.
18
THE SYSTEM OF THE STARS
Where direct comparisons can he dispensed with, & slit is
not easential to stellar light -analysis. For a star, having no
Benfiible dimensions, gives riee to none of the confused over-
laying of images produced by gioasor light-sources imJess super-
fiuoua rays be excluded by the iise of a fine linear aperture*
Hence the poasibility of applying a " slitleaa spectroscope " to
the stars. Their light is then simply passed through a prism,
either before it enters, or as it leaves the telescope. The
resulting variegated stripe, looked at through a cylindrical
leas to give it some tangible breadth, shows the dark gaps or
lines significant of the " type " of the atar,
But prismatic analysis is not merely communicative as to
the physical and chemical nature of the stars. It can tell
something of their movements as well. And, what is especially
fortunate, the informRtion that it gives is of a kind otherwise
inacce^ible. ''End •on" motions, as every one knowa^ axe
visually imperceptible ; the discovery that the spectroscope
has the power to make them sensible ie of such far-reaching
importance that Sir William Huggins, by bringing the method
into effective operation, performed perhaps the greatest of his
many services to science. Through the link thus established^
geometrical and physical astronomy have been placed in
closer mutual relations than cotxld have been thought possible
beforehand.
The observiitions concerned are of great delicacy^ and can
only he made with a powerful telescope* collecting light
sufficient to bear a considerable amount of dispersion. Their
object is to measure the minute displacements of known lines
due to " radial " or end - on motion, and proportional in
amount to its velocity. These displacements are towards the
blue end of the spectmm when the star is approaching, towards
the red when it is receding from the earth. The refrangibility
of the luminous beams is changed, in the one case, by the
crowding together of the ethereal vibrations, rendering them
more numerous in a given time, in the other, by their being
(as it were) drawn apart, and so rendered less numerous.
The juxtaposition of a standard terrestrial spectrum, such as
that of iron, gives the means of measuring deviations thus
produced, and so of determining the rate of approach or reces-
sion of the star examined. But the process is impeded to a
THE METHODS OF SIDEKEAL RESEAECH 19
degree hardly imaginable without personal experience by
tioahles in the ocean of our air. The twinkling of the stara
i& represented in their spectra by tremors and undulations
oitan permitting only instantaneouB eatimates of line-pogitious.
This inconvenience has been largely remedied by the use of
^e camera.
Stellar photometry has a twofold object It gives the
means of investigating, first, the individual nature ; secondly,
the collective relations of the stars. Stellar lustre is affected
by endless gradations of change. It ia rarely, perhaps never,
really constont. Periodical fluctuations are in many cases
obvioua ; secular variations are suspected. The suspicion can
be verified only by precise light-measurementa repeated at
Jong interv'als.
Their apphcation to the problems of stellar distribution
becomes feasible through the dependence of brightness upon
distance. The law of the decrease of light with the iwretue
of the square of the distance is universally familiar. If all
the stars were equal in themselves, their appai-ent differences
would thus at once disclose their relative remoteness. We
could locate them in spa^e just as accurately as we could
determine their lustre. But in point of fact the stars are
vastly diversified in siae and luminosity, and we can hence
reason from distance to brightness only by wide averages.
A statistical method alone is available, and its employment
evolves the establishment of strict principles of light-measure^
lent.
The firet requisite for this purpose was an unvarying and
consistent scale, which was provided with the least possible
diatorbance to existing habite of thought by regularising the
antique mode of estimation by " ms^nitudee," Intervals
loosely defined and unequal were made precise. A " light
ratio *' was agreed upon. To this proportion of change from
one magnitude to the next, the numerical value 2*512^ hwa
been assigned. That is to say, an average first magnitude
star sends ue 2-512 times as much light as an average star of
tho second magnitude, which, in its turn, ia 2'512 times
brighter than one of the third, and so on. From the first to
ie third magnitude, the step is evidently measured by the
' fiekotMl oM tbe uiuuber of which 0*4 ia the loguithm.
20
THE SYSTEM OF THE STAES
square <if th« " liffht raiio " (2-5l2x 2-512"6-310); and in
general the relative briiliaucy of any two stars may be found
by raising 2'512 to a powyr represented by the numerit^'al
diffei^nce of their magnitudes. One first magnitude star, for
instance, is equivalent to one hundred of the sixth tank
((2"512)^— 100) ; and to no less than a million atara of the
sixteenth magnitude.
All this IB a matter of pure definition, and definition is a
useful leading-string to experiment. It is something to have
a clear conception in the abstract of what a tenth, eleventh,
twentieth magnitude star is, even though the conception be
not altogether easy to realise. The problem of applying the
aumerical standard set up waa practically solved ahnoat at
the mme time by Professor Pritchard at Oxford, and by
Professor Pickering at Cambridge in the United States. They
first systematically and extensively employed instnunental
means in stellar photometry, with the result of satisfactorily
ascertaining the comparative lustre of till stars visible to the
naked eye in these latitudes.
Professor Pritchard adopted for his researches the ^' method
of extinctions." The image of each star wag made to vanish
by sliding between it and the eye a wedge of neutral-tinted
glass, of which the thickness just needed to produce invisibility,
waa found to give a very eiact measure of intensity. In this
way tlie brightueasof 2784 stars from the pole to teu degrees
south of the equator was determined and registered in the
" Uranometria Nova OionieuBis."
The Harvard " meridian-photometer " waa constructed on
the principle of " equalisation/' The images of the pole-star
(adopted as a standard of comparison) and of each star succes-
sively experimented upon were reflected into a fixed telescope,
and brought to an exact equality by means of a polarising
apparatus. From the amount of rotation given, for this pur-
pose^ to the double refracting prism, the actual difference of
brightness was easily deduced. The method is of wider appU-
cability than that by extinctions ; none the less, the '' wedge
photometer," in the form given to it by Pritchard, has taken
its place aa an indispensable adjunct to such inquiries. With
either instrument the limit of clearly distinguishable diflerence
is about one'tentb of a magnitude^
THE METHODS OF SIDEREAL RESEAl^CH 21
The original Harvard photometry' included all atanf to
the sixth maguitude as far as 30" of south latitude, to the
number of 4260. But it was only the first in a series of
similar and larger works. Its extension over the entire
heavens was aceompliahed by the publication in 1895 of the
San^ieTn Harvard Photometry of 792U stars ;^ and the
Revised Harvard Photometry, embracing about 9000 stars in
both hemifipheres, wae approaching completion in 1903>' A
Photometric Durchmaatemng of stars to 7'5 magnitude within
130"* of the North Pole was besides constructed with a larger
iustmment,* while the measurement of thousands of stars in
zones has established standards of exact comparison down to
the ninth stellar magnitude.
Potsdam is also the scene of extensive photometric opera-
kions, which have now virtually reached their immediate term.
Lbout 16,000 stars have there been very precisely observed
by MM. Miiller and Kempf, with a polarising photometer
employed on 26llner's plan of comparison with an " artificial
Vtar." The results thus by various observers variously obtained
1 in general satisfactorily accordant ; although the insecurity
Itiending processes of correction makes some degree of diverg-
ence inevitable. A Photometric Catalogue gives the bright-
ness of stars in all parts of the aky " reduced to the zenith."
But the reduction is not by a simple or Certain procedui'e. A
law of light-absorption in the terrestrial atmosphere has first
to be arrived at experimentally, and the esperimente are
difficult and delicate. Even at the zenith a heavy duty has
to be paid, estimated by the Potsdam obsei-vers at 16 or 17, by
Frofeaeor Pickering at 20 per cent ; and the rate of increase
towards the horizon differs at different allitudea, and probably
in diSereut climates as well. Hence the adoption of a uniform
plan of reduction for photometric observations seems to be
^recladed ; yet its absence must involve more or leas serious
ancies. They are, however, possible only when the
ige of conditions is wide ; where they are fairly constant,
treme accuracy is attainable.
1 Harvard Annals, toI. xiv. pt. i. (IS&l). For i coupariBon with the
)zfcrnl rrffuUs we ibid, voh xlii. |k ICi
* Harvard ^ntuila, vol. rxiiv.
« Jhul. vol L
* Jbiii. ^-ol. x!v. 1901.
22
THE SYSTEM OF THE STABS
In the Keviaed Harvarti Photometrjir two stars, Aldebaran
and. a Crucia, are rated as almoflt exactly of standard first
magnitude brightness, each being 2 '6 times more lumiiioua
than the pole-star. They have in the northern hemisphere
six superiors — Arcturus, Capella, Vega, Procyonj Altair, and
Betelgeux, the standing of which has accordingly to be
expressed by fractional numbers. Capella and Arctnras are
' of magnitude 0'2, aignifying that each is eight-tenths of a
magnitude brighter than Aldebaran, while the figure 0"06
attached to a Centauri conveys the fact of its superiority to
ft Crucis by just one magnitude. Carrying out the same
system of notation, we get negative numbers for the designa-
tion of still higher grades of lustre. Sirius, for instance,
sends ug eleven times more light than Aldebaran ; it excels
the standard by two magnitudes and six - tenths, a pre-
eminence compactly expressed by calling its magnitude - 1'6.
To find a star uutshining Sirius we must go to otir own
fliun, to which a rank can be assigned on the same flcale. Its
light, as measured by Alvan Clark in 1863, exceeds that of
the dog-star 3600 million times. Bond made the dispropor-
tion 5970, Steinheil 3B40 millions to one. From a mean of
these insecure determinations, Professor Pickering fixed the
sun's stellar magnitude at - 25'4 ; ^ but various lines of
inquiry^ separately traced by Mr. Gore ^ and Sir David Gill»
converge upon a much higher value lying between -26'5
and - 26'8- It seems fairly certain^ accordingly, that the
splendour of Siriua is some 10,000 million times fainter than
the blaze of sunshine in which we live.
The invention of the telescope itself does not mark an
epoch more distinctly than the admission of the camera into
the celestial armoury. All the conditions of sidereal research,
in especial, have already been transformed by its co-operation.
The versatility of its powers is extraordinary ; no task has
yet found it unready or incapable. It is the very Ariel of the
astponomical Prospero.
This untiring serviceable ness was made possible by the
sulistitution in 18*71 of gelatine for collodion as the vehicle
for the Siilts of silver, the decomposition of which under the
' Proeetdingi Ainerisan Aca(Lmy, toI. svi. p, 2.
> Monthly Notiw^ vol Ixiii. p. 184.
IHE METHODS OF STBEREAL RESEARCH 23
infiueace of light forms the easeutial part of the photographic
process. The new plates were, however^ first used for " astro-
graphical" purposes by Sir William HugginB in 1876. Since
they are five times more sensitive dty than wet, expoeurea
with ihem can be indefiiiitely prolonged. They may, besides,
be prepared any desirable time before, and developed any
d^irable time after exposure^ thus accommodating themselvea
in a really wonderful way to the needs of a&tronomers.
The unique power of the pbotogniphie plate as an engine
discovery is derived from its unlimited faculty for amassing
liat impressions of light. By looking lontj enough it can see
anything thtre is to be seen. Sir William Abney'a expet-i-
ments convinced him that no rays are too feeble to overthrow
the delicate molecular balance of silver bromide if only their
separately evanescent effects get sufficiently piled up through
repetition.^ By thia capability of taking time for its ally, the
camaru leaves the eye far behind. Witli any given telescope
much more can be photographed than can be seen, and the
threshold has been crossed of a region of research, visually
inaccesaible, but open to exploration by the far-reaching
chemical method.
The penetration of space has, nevertbelessj limits. A
pixis -ultra is imposed, if not otherwise, by the restricted
possibilities of continuous exposure to the skj'. Darkness
does not last indefinitely, nor is it absolute while it pievalb.
There is always enough light scattered abroad to " fog "
sensitive plates left long under its influence j and when
fogging begins, portrayal compulsorily terminates. Thus, the
plan first adopted by Dr. Roberts of obtaining a single pict^ire
by means of exposures renewed night after night can be
availed of only with restrictions.
The telescope forming the image which imprints itself upon
prepared plate is always equatorially motmted, and has
a motion given to it exactly concurrent with the revolution of
^le sphere. Yet the utmost mechanical ingenuity cannot
Bake the concurrence absolutely perfect. Minute inequalities
survive and need intelligent correction. Even more sensible
are disturbancea caused by the changes of atmospheric re-
&ttCtiou with the ascent towards or decline from the meridiau
* ObiertyitOTy, ffol. stu. p. Ift5.
24
THE SYSTEM OF THE STAES
of the objects in course of delineation. For these reasons a
photographic telescope has, aa a nde» a guiding telescope
attached to its axis, through which an observer watches to
counteract, almost to anticipate, nascent tendencies to die-
jplacement- The strain upon the attention la severe ; ita
endurance, upon nccaeions, for three, even four hours at a
stretch, is no small proof of resolution,
Expoaurea can^ however, be curtailed by shortening the focus
of the photographic telescope, the image being thus rendered
smaller, and — through the closer concentration of" the ^ame
amount of light — more intense. For simply exploring the
skies, sounding their depths, and dredging-up their contents,
nothing can be better than the form of an ordinary portrait lens.
With such a one^ only two inches in diameter, the picture of
the comet of 18 82 was taken at the Royal Observatory^ Cape
of Good Hope, the " thick-inlaid " background of which
afforded the first palpable revelation of the star- charting
powers of the camera ; and much of Professor Pickering's
admiKible work in sidereal photography has been done with a
Voigtlander's " doublet " [two achromatic lenses in com-
bination) of eight inches aperture and about forty-five focus.
Objects imperceptible through the Harvard fifteen-inch refractor
can be photographed with this instnunent ; and it has proved
extraordinarily efficient for the rapid charting of stars and
their spectra. The " Draper Catalogue " was indeed com-
piled wholly from materials collected by its means. In the
*' Bruce telescope," completed by Alvan Clark under Professor
Pickering** direction in 1S93, and mounted at Arequipa in
1896, after transmission through the Straits of Magellan, the
same plan of construction was carried out on a larger scale.
The object-glass has a diameter of twenty-four inches, the focal
length is eleven feet Stars down to the seventeenth magnitude
are probably recorded on plates ex].H:>5ed to the strong con-
centration of light thus effected. The portrait-fonn of lens
has the additional merit of giving a large field of view. Each
photograph taken with the Bruce telescope covers, with very
slight distortion, five degrees square (25 square degrees) on
a scale of one minute of arc to a millimetre. The whole
heavens could be charted on about two thousand such
plates.
THE METHODS OF SIDEREAL EESEAUCH 25
Where acciirate measurements are aimed at, however, the
type of inaCrumeut represented bj the MM. Henry's photo-
graphic telescope ia preferable. The object-glass in thk is of
the ordinary achromatic kind, but corrected with reference to
chemical, instead of to viBuiil jicti<jn. The rays selected to be
brought to a foctis are those to which, not the human, but
the "photographic retitia" is aeositiTe. The aperture is Id
ioches, the focal length eleven feet ; a plate-holder is substituted
for an eye-piece^ while a guiding- telescope of slightly inferior
ilimensioaa ia enclosed within the eame rectangular tube.
The field of view with the Paris photographic telencupe, within
which definition may be considered as virtually perfect, is a
le three degrees in diameter,' covering an area of not quite
"five square degrees. Fully ten thousand of these plates
(allowing for overlaps) will be needed to picture the sphere;
and they ate being taken in duplicate for the purposes of the
International Celestial Survey. Eighteen instnxments, modelled
on that of the MM. Henry, are employed upon it ; and the
high quality of the data they will provide is assured. Yet
thought quails before the quantity of materials presently to
be dealt with. Eventually, we may fairly hope, they will
be brought within the unifying grasp of statistical research ;
at only at a heavy cost of wearisome toil.
Studies of the distribution of the stars," Professor Picker-
ing remarked, " can now scarcely be undertfiken in any way
except by photography." But photography, to be really in-
structive on thia point, must be combined with photometry,
The portrayal of millions of stars projected side by side oa a
spherical surface tells us little or nothing of their relations to
lie immensity of space. Thia can only be found out, for the
St majority of them, by collecting atatiatic-a of the amount
~f light they send us. Hence the importance of the photo-
metry of small stars. Yet no visual means have hitherto
proved competent to deal with it. Eye-estimates, however
aided and succoured by instruments, break down when
shed too far down the scale. The problem is evidently one
of those reserved for successful treatment with the camera.
What is called " photographic iiTadiatiou " affords one
zaeans of attack upon it. This arises from the diffusion of
' £ullttin Attrtmomiqut, t vi. p. 308.
26
THE SYSTEM OF THE STABS
light within the eubatance of the gelatine film. The particles
directly meeting the atellar rays reflect tbem irregularly all
round to other particles, thus widening the area of oheruical
decomposition, and creating circular imagea which, with the
same exposure and on the same plate, are found to vaiy in
size with the magnitude of the stars they represent.^ Thua,
from a few stars of ascertained brightnesa, that of the neet
imprinted with them may, dowa to a pretty low grade, readily
be inferred. The faintest stars, however, give rise to dots so
small that differential measures of them are scarcely practicable.
The method is further ci:)mpromised by the uncertainty of the
law connecting the size of chemical star-discs with brightness.
It is indeed a mere empirical formula varying with the con-
ditions of obaorvatioiL It ia not the same for rapid aa
for slow plates ; it is not the same for twinkling as for
steady images,^ There is no help but to treat each plate
aa a document apart, and to assign its constants inde-
pendently ; and this is to adopt an expedient, not to employ
a system.
Nor does the scale of photographic effectiveness agree at
all closely with that of visual sensibility. Colour has in this
respect a strongly disturbing influence. The quick vtbratioua
at the blue end of the spectrum are those most active in
releasing silver from chemical bonds. Blue stars are con'
sequently far more, and red stars far less conspicuous self-
printed than to the eye. Photographs of chromatic double
stars thus show curious reversatsr a small blue companion
often coming out superior to its yellow or reddish primary,*
And tinted stai-s too ftiint for eolour-diaerimination with the
telescope can sometimea be picked out on a negative, simply
through anomalies of relative magnitude. Now differences
of this sort occur not only in isolated cases but methodically.
Their frequency, aa Professor Kapteyn discovered in measuring
the Cape Dui-chmuaterung plates, depends upon celestial
situation. It varies with galactic latitude. And the in-
evitable inference was drawn that "the stars of the Milky
Way are in general bluer than the stars in other regions of
1 Asir. NacJi. No. 2SS4.
• Gill, Inteoducti^n to Ca.p': Phatograj}hie DureJtirwstervng, p. 24-
' Eipin.tJfewwitffJ/, Tol. vii, p, 247.
THE METHODS OF SIDEREAL RESEAJICH
^i
the sky." ^ Thoflj photographic photometry has a very im-
portaat beazing upoa studies of sideieal cotiHtructioti. Bat a
settled baais of principle is needed to give its ne^oJta the full
authority that should belong to them. At preseut. actioio
magiutiid&s are derived very much at the discretion of individual
obeervere. Perhaps the beat way of treating them would be
to take them for what they are worth, abandouing attempts
toveduce them to scales of visual magnitude. They are worth
a great deaL^ In some respects, perhaps e^Tea more than
magnitndea estimated by the eye. For their enumeration
and classification may supply both geometrical and physical
data regarding the stars ; indications^ that is to eay, as to
iheir arrangement in space, and indications besides of their
aaaortmenb by affinity of constitution into indefinitely vaat
aggregations.
The photometry of nebulfB haa, so far, obtained less than
ite due meed of attention. Sir William Hu^ina ascertained,
in 1866, the extreme intrinsic faintness of such objecta,* and
there the matter rested until the universal agency of the
camera was made available. Then, in 1884, Mr. "W". H,
Pickering described a mode of constructing a scale of photo-
graphic intensity by expoeing a number ot" email squares at
one aide of a sensitive plate to a known light-source during
different inten-'als of time.* These, developed with a nebula-
pictore subsequently imprinted, afford so many terms of
compansoa for the relative brightness of its parts. He drew
in this way a set of " isophotal contours " in the Orion nebula,
and the map representing them constitutes a record of present
intereatj and of poesible future importance. The absolute
brightness of the formation, in the central " Huygenian "
region, was found to range between VO and 140 units, the
adopted unit being one-millionth of the light given by a
standard pentaue lamp. No further equally systematic
attempts have been made to determine the luminosity of
iiebulffi ; although its variabihty, assured in some cases,
' Introduotiaa to Ca^i Fhotetfraphic DuTehmuattruntf, p. 22.
* Oill, il^. p. xii. Tiote.
' PKU. 3>tJM. vol clvL p, 302. CC J. E. Oew, Ohasrmiory, Mny 1£»05.
* /Vm. Anutr. Aaad. ToL 3cx» p. 613; HarvoTd AnnaJs, va\. xxiii. p. 16.
Sir W. Abney iDdepeudeitCly t^a ytat« l*ter inreDted tk simikt derice, iVWurv,
Tol. i3. p. 472.
THE SYSTEM OF THE STAES
suspected in manj more^ strongly suggests the desirability of
establishing a fixed plan of measurement.
There is scaxcely one of tlie numerous taflka of nebular
oatronomy that cannot be better performed photographically
than visually. lu the simple perception of faintly illuminated
surfaces, the tjuickly fatigued living retina is left far
behind by the imperturbable gaze of a seneitised plate ; in
their delineation, the subtlest human hand is at a similar
disadvantage. Professor Holden gave his testimony to the
effect that " every important result reached by his four years'
study of the Orion nebula with the 26-inch Washington
equatoreal/' and very many not comprised in it, were attained
by Dr. Common*B subsequently taken photograph, which
required an exposure of only forty minutes,^ Spectroscopie
inquiries, both stellar *uid nebular, are enormously facilitated
by the substitution of permanent autographic records for seta
of quivering lineSj caught in their mean positions only by a
keen glance at critical raomente, and constantly liable to
effacement by atmospheric waves. It is true that the range
of observation ia not the same in both cases. The plates
in ordinary use ignore the lower end of the spectrum, but are
affected by the higlier vibrations which, by their quickness
and shortness, evade the eye. " Orthochromatie " plates,
sensitive to yeDow and red rays, can, however, be produced
by staining with eosin and other coabtar dyes; but their
use is attended by some inconvenience. Uniformity of light-
action can scarcely be secured with them ; they respond bo
it with a certain caprice ; and are henoe apt to yield spectra
of a somewhat patchy brightness.
The wonderful comprehensiveness and adaptability of this
method are strikingly apparent in the results obtained since
1886 at Harvard College. By no other means could the
spectroscopic stellar survey executed there and at Arequipa,
its southern dependency, have been carried out on so great a
scale. The results constitute a veritable spectroscopic Durch-
musteruug, complete to about the ninth niagnitude ; and the
work is now being extended to fainter stars. The manner in
which it was conducted, although described by Frauuhofer and
Secchi, was virtually novel. A prism large enough to cover
' Owrlaiid Ifonthly^ NovembeT ISSfl.
THE METHODS OF SIDEREAL EESEAKCH 29
the entire object-gloas is placed in front of it. The stellar
beams are thiia analysed before they we concentrated ; every
stellar image is trunaforraed into a prismatic rii>aud ; and stara
by the dozen or by the score print their eeparute sjjectra on a
single plate with a single expoaure. SUt and cylindrical lens
are alike rejected ; the diurual motion is employed to widen
the sEpectral bands sufficiently to bring out their distinctive
features. That ia to say, the stars are allowed to " trail "
slightly across the direction in which their light is dispersed.
The results are admirable ; innumerable lines are cleai-ly
recorded ; but the highest degree of accuracy cannot, in the
abeence of any system of reference-liues, be given to deter-
minatioDB of their positions. Mrs. Flemiug's scrutitiy, mean-
time, of the i*ecords thus profusely accumulated, has led to the
discovery of hundreds of objects remarkable for the unusual
quality of their light; and the spectra of about 1800 bright
ebars, photographed on a larger scale with more powerful
inBtrnmenta in the northern and Bouthern hemispheres, have
been discussed and catalogued respectively by Mlbs Maury and
Miss Cannon.
For detailed identifications, the more laborious plan
adopted by Sir William Huggins in 1879 is still pursued.
The stars are taken one by one ; their rays are admitted
through the postern-gate of a slit, and record their peculiarities
aide by side with a comparison-spectrum providing starting-
points for measurement The "Atlae of Stellar Spectra"
published by Sir William and Lady Huggius in 1899,
exemplifies the perfection with which details, otherwise
iuaccassible, can thus be brought into view. Glass, which ia
strongly abeorptive of the shorter wave-lengths, is excluded
from their apparatus. The stellar raye admitted to it are
concentrated by an 18-inch speculum, and dispersed by quartz
prisma. Introduced by Sir William Huggine in 1868, the
spectroscopic method of determining stellar motions in the line
of sight was perfected, ten years later, by the change of venue
effected on the initiative of Dr. Vogel, from the eye to the
plate. Its superiority has, in this difficult branch, trium-
phantly asserted itself. The precision photographically
attainable in measuring spectral shifts is chiefly due to the
virtual elimination of the effects of air-troubles. The lines
THE SYSTEM OF THE STARS
from which information &r to movement has to be gathered
depict themaelvea in their normal places. Their waverings,
so bafQiug visually, are chemically ineHective.
Nor is it only here that the autographic mode of pro-
cedure attains a refinement on a par with its power. The
subtlest problem of atellar astronomy is that of aiminil
parallax. It leaves room for no compromise in the matter of
lu^cTU'acy, yet it has been solved with the aid of the camera.
Professor Pritcbard's careful and persevering experiments
established the validity of photographic determinations of
parallax, and so furnished to the sidereal armoury a new
weapon of pi-ecisiou and loug range. It happens, moreover,
that the objects most inviting to the one mode of treatment
are precisely those reached with difficulty by the other.
StarB too faint for the eye to deal with satisfactorily come out
on negatives in neatly measurable form ; while the brighter
stars suitable for observation with tlie telescope and micro-
meter give distended photographic images uupromiaiug for
exactitude.
There are intlicationa that reflecting telescopes will before
long regain the position of preference which Fraimhofer's
skill in grinding lenses forced them to abdicate. They have
over their rivals the special advantage of being perfectly
achromatic ; they collect at one focus all the ray^, visible and
invisible, striking them. This the very best refractors fail
to effect However skilful the combination of different kinds
of glass, a largo amouat of ligbt is necessarily "thrown
away" ^ Opticiana have to choose what sections of the
spectrum they will turn to account, and neglect the rest
Photographic re^jctors are for this reason useless in ordinary
observation. The images they give are wholly built up out
of blue light, while the light proper for seeing by wanders
unserviceably astray. The plates exposed with them must
accordingly be sensitised in correspondence with the mode of
their correction. No tolerable results could be got with
orthochromatic plates in the Henry telescope.
These drawbacks are, nevertheleas, to a great extent out-
weighed by tyauntervailing prerogatives, Refractors are moi^
manageable than retiectors. They are less sensitive to slight
1 SiF H. Clrabb, Monihl^ AViw. yol xlvii. p. 30*.
THE METHODS OF SIDEREAL EESEAECH 31
less intolemnt of unequal pressures ; they Bcconuno-
date tbemeelves better to mechanical exigencies, can be more
rigidly mounted, hence made to follow more strictly the
circling of the sphere, and so to ]seep & steadier hold of the
Ejects in the 0el4 of view. Where measui-ee of precision are
liefly aimed at, choice is thus naturally directed to them,
and they have been stamped as the official inatrumenta of
celestial photography by their adoption for the vast
Btar-eharting operations decided upon at the Paris Con-
gress of 1887. The splendid nebular pictures, on the other
hand^ obtained with reflectors by Common and Roberts,
and more recently in America by Keeler and Eitchey, prove
their superlative fitness for tasks of delineation. More-
over, their future extensive employment in spectrographic
work eeema inevitable. With refractors, the range of
good spectral definition is narrowed by their inequalities
of focal concentration, while reflectors display in uniform
distinctness the whole light-gamut from end to end. This
point of superiority is very important, since a partial view
of stellar spectra is, in many cases, not only unsatisfac-
tory bat misleading. All telescopic varieties, in fact, find
their place in the boundless fields of photographic research.
Mirrors do not exclude lenses; instruments of short focus
have A special function, while for other purposes those of
long focus are preferable. The needs of sidereal investigation
are manifold; they claim subventions from every quarter;
they invoke the most diversified forms of assistance. And
their demands have been met by a geueruus largesse of
inventions and contrivances.
The foundation of stellar astronomy is, as we have said, in
infinitesimal accuracy. It could not otherwise exist, since the
quantities concerned are so small as to disappear amid the
errors of rough obaervatione. But for its progress, something
more is required. A few scattered items of knowledge do not
constitute a science. The word implies the suflusion of a
subject with intellectual light derived from large inferences.
Large inferences, however, must be based on a plentiful store
of facta ; and the facta collected by sidereal study are, even yet,
few compared with its innumerable objects. They are, indeed,
being continually multiplied. The alliance with photography
Jl THE SYSTEM OF THE STABS
iifcs »:o=cr=»i tJi-r tiisi* .:: reaa>:ing without impairing il
asccmj. Ft •:■ r-ibsr '" V Ar? co-idd the desired informatiB
x 5:^rofc. -M .dj iz. « ': :ukdizice, but with the
■^'dTcn-ir. F:c. :•: a ci=r:Aia exient, the work has to
i-"of iij-i:za5 t^'t. r-zi- i* rsi'ii intuitions are necessary ]
rcu."*:.::^ * '-^ irizz -:■: zi^iLrsiatical reasoning, beoiQ
"wc.'K*: :!■:? «Ccrt> att li'tc-^r^c. the w^e^ed faculties at
r^rL* :c :vc.r^ze tc toie them, so some degree of
:3T«r^ is iTsi^^iSirZ-r r'.'-r sristdining the tmiversal int
w^-* r>r* 1 ?z:iec: ::* TiiAlirr. but declines to foUow too]
tATir ic jx:''.Ti~^ :;■ ;-•* bilrinr-plaoe for another.
T-z*^ z*:c zLi-rrvZy wLa: i: c-^ji do. but the rate at which it]
v%kr i: ::. his :c ':«r ;»:n5iirr*i*i in estimating the value dl
yi?:c-vVt*rCT i^ m ai^i :c iSTr^zLomx. And there is little fear
:c 'J^ ^^z:z.z*'jz^ Useznir thzv^c^h sluggishness of pace. It
i»tfc«? -r i VST ■" S:;:r=i ;:2d Drang " of progress. The
.•jivuTj: ^x-w«r* :■:' er-.:=i-=rii:c»=. dvsiied br Homer for cataloga-
;z^ ;is ,r:vi :c* Gr«ek siije aie £ir outdone by it Its
i:iS3r;:rie-i:TAl::T. riKWTer. came to hand just when the
rs:*I::::3-ii:iv"^ :iir*::«rr c: the problem set by the heayeiia
S.y*z :c ':« *T*srei in ill ::s f:rnudable reality.
Tbtf $Tar'.:"^r^B*5 :z :hr r>i>:-:'^phic method is due, not
il'.'Oii* :o :rj=' iT«i: =.;u:::tr o: vcoects it can register t(^ther.
:;;: ;o ;>.-? ,l:<r%rr5;:- Ari division of labour it makes possible.
K^vr.*.? -*cCA:~-vi *;y ;: hi^^ ih* enormous advantage of being
•.vrrjiATs^r.^ Tb^y di :bc i:::in^ incidents of the heavens as
:h<f v^'.*iv,vr*vi: lies :he iransien; accents of the human
\ ,':^v. All ihr; sotriy hc'-irs of unclouded darkness can thus
Ix- ,li-^c«v; :o AV-r^c n^icriils for subsequent investigation
i:; ,l4xlxj:^.: .XT >i*d w-tither. Innumerable experts may be
^xv.yls'w. :u ;>.:s wriy *: re::;o;c plaoes and with different ends
'.*.'. \ vw A s;v«;li* :uy&::ve :::iT be communicative regarding
*;>-lU? vhcCv ".•;:'; ry. d:s:r.ru:i^^n. ^xirftUax, proper motion; its
,vr,;'Av.'.s.-r. w::h s-rher? ^rves ;o t-est variability, or even to
r"\ ;S4' *"AV> .■:" s.'v.5e ::;ys;crl:uf sidereal cataclysm. Yet the
».\vft*•««.^r, ,-: y:x;-rf# o: <vlest:al objects does not in itself
xV-v.*; ;:;;•«' sr. uvrtvist ot kr.owle«,:ce. They contain latent
*,;-»o^".;a:u".;. ;;:*: as :he siit^s ibeniselT«3 do, but the educing
^\:\\\'«v Vv «hK'h i: is nude stf^sihif is as n etcom y in the one
v'^k*^ *» u'» :>-^ v^:^.ef. Zeal in securing them !• ao
THE METHODS OF SIDEREAL KESEARCH 33
;ht avail without induatry ixi discusslDg them, whether
inally or by deputy; for astrographical tasks are easily
le of delegation. Star-prLnts are indeed usually dealt
ith by specialUta in measurement, whose Bkill has been
by many noteworthy diacoveriea. Those, too,
the ftttuie has in i^^rre will doubtleaa fall macb more
ty to the share of investigators armed with microscopea for
bisection of star-dol^ on glasa plates thau of tekacopic
lera of the heavens.
Kot that the telescope is, or ever can be superseded. On
'tiie oontraty, the enlargement of its capacity becomes more
desirable with every fresh addition to the apparatus used in
lOonjuDction with it. Modern sidereal astronomy may be said
%o live an light. Large telescopic apertures are a sitw qud
nan for its growth and activity, A considerable proportion
Inf the objects it has to do with are, in fact, beyond the range
4f AdaU instruments. It is. however, &a important to
economise as to collect the far-travelled rays from the stars ;
pUd m this direction little has been accomplished. Under
l^lfae beet conditions, no more than 5 per cent of the light
' Itriking the 40 -inch object-glass of the Yerkea refractor
ictaiUly reaches the sensitive £lm after trausmiasion through
t^ great Bruce epectiograph \ and although the waste in
other forms of apparatus is less formidable in amount, they
cannot yield results of equal precision. For obtaiiiing legible
Rcords of the faintest spectra, none can compete with the
slitless spectrograph employed in connection with the Crossley
veflector at the Lick Observatory, How much of the incident
Bgfat it tarns to account has not been ascertained ; but stars
of the fifteenth magnitude have none to spare, and their rays
ba Buccesafolly anadysed on Mount Hamilton.
CHAPTER HI
THE STAKS A& SUNS
The Btara, speaking broadly, are buus. But what is a eun?
We can only reply by taking function into consideration. A
sun ia a great radiating machine, and the obvioufi chterion
for admission to the order is fitiieaa for this office. Qualifi-
cation to be a centre of light and heat is the dominant
characteristic of each of its true members. Now the solar
emiseive activity ia concentrated in a shining shell of clouds
known as the "photosphere," which the entire energies of the
organism (ao to speak) seem directed to maintain and renew.
And with reason, since its efficiency as a radiator depends
upon the perpetuation of the condensing process by which
this brilliant surface is produced.
The poaseasiou of a photosphere muat then be regarded &s
an essential feature of the suns of space. But such a struc-
ture can only he formed in an incandescent atmosphere, the
action of which modifies^ more or less powerfully, the light
traversing it. The spectroscope can, in fact, alone decide
whether a given sidereal object be, in the proper sense, a sun.
For it is not so much the quantity as the quality of its radia-
tions that determines the point. They must be such as can
be supposed to emanate from condensed and vividly glowing
matter bathed in cooler, though still ignited vapours. That
ia to say, they must, when dispersed by refraction or diffrac-
tion, constitute a fundamentally unbroken prismatic band,
marked iyicid^Titall^ by effects of absorption, A continuous
ftinge of vivid light, crossed by dusky lines, is hence the dis-
tinctive spectrum of a sun.
The enormous light-power, and, 60 far, the solar nature of
THE STABS AS SUNS
35
the stare, followed as a corollary from the Copernican theory^
since at the unimaginable distances implied by their apparent
immobility while the earth performed its vast circuit, they
should otherwise have been totally inviflible. But the analogy
could be strictly tested only by spectrum analyaifi, and it
proved virtually complete. Complete, that is, for the great
majority of the etellar populace. There is a residuum in
which it is impaired ; there are a few scattered inatancea in
which it is actually overthrown.
•■: This degradation of type shows itself in different ways.
Absorption in some cases becomes so immoderate as well-nigh
to smother the original light of the star ; the atmosphere in
others outshines the photosphere^ giving rise to bright instead
of dark lines in the spectrum ; while in certain objects a
similar efi^ect appears to be produced rather by a paucity of
photoepheriCj than by the intensity of atmospheric radiation.
When the failure boa gone so far that the light of a seeming
ite, analysed with the spectroscope, ia found to consist chiefly
of isolated rays of various colours, then the object approximates
more to a nebula than to a star. It certainly cannot lay claim
to the designation of a sun.
But as in the other kingdoms of nature, ao here ; there are
no abrupt tranaitiona Continuity is everywhere maintained.
The descent from a perfect sun to an imdoubted nebula
ia effected without interruption. Hence, inevitably, some
uncertainty in classification. Broad divisions are easily
established, but hard and fast outlines to thoee divisions
cannot be drawn. " Frontier-instances " abound, and compel
recourse to somewhat arbitraty distinctions. We propose,
in the present chapter, to consider only bodies of assured
status, with radiative machinery in fuU working order —
bodies, as to the essentially sun-like nature of which there
c&n be no difference of opinion.
The four spectral types discriminated by Father Secchi
atill form the basis of arrangement. They may conveniently be
designated as Sirian and solar, Antarian aud carbon stars* all
showing continuous spectra crossed by dark lines of abaorp-
tion, to which, in the two last varieties, dusky bands and
flutings aj^ superadded. The Sirian order, however, as
originally describedj included certain bright atars with seem-
36
THE SYSTEM OF THE STAES
ingly blank spectra, prominent chiefly in the ooosteUation
Orion ; and these have gained auch importance through the
discovery of terrestrial helium as to compel their relegation to
a class apart. Thus^ Secchi's ^hite stars have, as it were,
epontaneously ranked themselves into two great battalions,
and we shall consider firat those that came last to full recog-
nition.
Stars of the " Otloq " quality are purely white ; their light
approximates to being io the native state ; that is to say^ it is
Bcarcely modified by the arresting action of their atmospheres.
Yet it 19 not wliolly characterless. Hydrc^en and helium,
especiallyj have left their Btamp upon it. Fig. 1 of Plate 11.
reproduoes, by the kind permission of Professor Pickering, a
spectrograph of e Orioms, the middle star in the Belt, taken
at Arequipa, November 10, 1896, with the 13-inch Boyden
refractor. The dispersion was produced by means of a train
of prisma in front of the object - glass ; no slit was used,
consequeDtly uo comparison could be made available ; and the
exposure allowed was of 106 minutes. The darkening at
either end is due to the limited range in sensitiveness of the
plate employed. Helium-lines are nearly as strong as those of
hydrogen in the spectrum of e Orionis ; and their association by
Sir Noiman Lockyer and others with the newly unearthed gas
encouraged Dr. Vogel, late in 1895/ to search for further
flignfl of their presence in a large collection of stellar spectro-
grams, prepared at Potsdam by Dr. Wilsing, To his siirprise,
he foimd Orion-stars to be fairly numerous all over Che sky .
and the late Mr. McClean's researches proved them to be still
more prevalent in the southern than in the northern hemi-
sphere.
They are, for several reasons, of particular interest.
Sidereal genealogists assign to them a very early standing.
They seem, indeed, to occupy a position intermediate between
true nebulas and Siriau stars. This conclusion is enforced,
first, by the visibility of nebulous appendages attached to
many helium-stara ; next, by the low density which is one of
their least doubtful characteristics. And it obviously implies
that they have made less progress in contraction through
cooling than globes of more substautiat build. But even
^ SitxtngtinridUc, Berlin, October 24,, IStffi.
THE STARS AS SUNS
87
among helium-BtarB themselves gradations of age are per-
ceptible, Mias Mflury arranged theiu into six groups/ corre-
flpondiug, it was plausibly supposed, to so many stages of
sdy&nce in condeusatioa. One of the earli^t of her etars,
$ Orionia, ia aigaiiicantly placed at the core of the great Fish-
mouth nebula ; and la the species to which it belongs^ metallic
abeorptioa is barely discernible, while some peculiar lines,
identified with hydrogen by Pickering and Rydberg, come into
view, together with a few delicate triplets ehowa by McClean
to originate from oxygen. Helium and hydrogen are beaidea
represented by their usnal acts of rays. Although some
advance from the immature state of ^ is marked by the spectrum
of c Ononis, it etiU bears the impre-ss of oxygen and "cosmic"
hydrogen. Silicon-absorption is unmistakable in Bellatrix ;
^ Crucis, one of the gems of the Southern Cross, is an
exemplary oxygen-star; and, at the stage reached by Algol
and Rigel, primitive symptoma have been superseded by the
clear emergence of magnesium and calcium-absorption.
To resume. Helium-stars have the&e special features. They
pOBsess envelopes of helium capable of selective action upon
li^t. Some among them^ and notably those with nebular
affinities, show dark rays of oxygen and cosmic hydrogen. In
aU, metallic absorption is feeble. The photospheric radiance
o>f all spreads abroad into space sensibly unmodified by atmo-
spheric stoppage. Finally, they tend to congregate in the
Milky Way, particularly in the eouthem hemisphere.
Sirian stars resemble their predecessors in their brilliant
whiteness and comparative freedom from atmospheric encroach-
loeDtB. There is little or no trace in them of the general veil-
ing efiect by which our own sun is shorn of a large proportion of
his more refrangible beams. The Sirian spectra, although not
intact» are entire, and are hence especially strong in their
ultra-violet sections. To this immunity from absorptive
attacks there is one remarkable exception. The eign-
manual of hydrogen is stamped upon them with extraordinary
intensity, A number of metals are also present, but they
show lines too faint and fine for easy recognition. Fraun*
hofer*s " T)/' the ubiquitous double-line of sodium, is neverthe-
obviotiB, as well as the " K " of calcium and the " blue "
^ Harvard Awutls^ toI. xxviji, p, IS,
38
THE SYSTEM OF THE STARS
line of magQeeium. With the best definition, too> mtilti-
tudinoua fine striations, a large proportion of them due to iron,
can be photographed. Thua, in the spectrum of Sirius (see
Plate II. Fig. 2), Mr. S. A. Mitchell counted on his plates 75
Hues in the restricted section compriaed between two consecu-
tive hydrogen-lines {H^ and Hy).^
, Photography has indeed played an essential part in the
investigation of Siriau spectra. The strength of their ultra-
violet radiations lends to the method peculiar efficacy in
dealing ^vith them ; and the advantage was turned to the
fullest account by Sir William Huggtna in 1879.' The
impressions secured by him with an apparatus from which
glass was wholly excluded, afforded a discovery memorable,
not in the history of astronomy alone^ but in that of mole-
cular physics as welL
Tia. 1.— 8|»rtnim of HjdnjeMi ^ Wliifca BUn (Hagglnm).
A photograph of the spectmm of Vega obtained with one
hour*8 expoaure contained twelve strong lines (shown in Fig. 1)
forming a group in obvious rhythmical connection. They
crowd together more and more as their wave-lengths shorten.
A common ongin for the entire at once auggeata itself: and,
on the ground that its two moat refrangible members were
already known as hydrogea-lines. Sir William Huggiua did
not hesitate to pronounce hydrogen reaponsible for all His
inference has been amply justified. Seven of them proved to
have been, a short time previously, photographed directly from
glowing hydrogen, by Professor H. W. Vogel ; * and the com-
plete set was similarly procured later by M. Coriiu»* but with
^ AitTOpK Jaum. vol. r. p. 32.
> Pkit, Trans, vol. clixi. p. 669.
' MtT. NfKh, No. 2301.
* JmrMtl dt Physique, E, v, p, 841 (1886).
THE STAES AS SUNS
S9
extreme difficulty. Although the purified gas filling the
capillary tube placed in front of the slit was excited by
powerful electrical discbai^a, its highest radiations took no
less than three hours and a half to get satisfactorily printed.
Some idea may thug be gained of the intense incandescence
leigDing in the remote stellar atmospbereB from which they
wete fii^t derived.
The law regulating the sequence of hydrogen -lines was
aaBigned by Balmer in 1335.* It is a purely empirical
formula that may be modi^ed at will ; yet since it has
availedt not only to connect together numerically lines already
obeerred, but also to locate additional ones, it must corre-
ipond to something esacDtial in nature. The membem of the
" Huggina-eeries " are really indefinitely numerous. They
crowd up towards a limit in the ultra-violet, which, like the
aaymptote of a curve, is continuously approached, yet never
ftctnally attained. Subjoined are the wave-lengths, in ten-
miUionths of a millimetre, of the first twenty, as given by
Dr. Kayser.^ Their designation by the letters of the Greek
alphabet is now all but univerBal
Waw
tODj^th.
nsifgiLEtlan.
Wavfl-tone^h.
6583-07 (Frannhofer'e
C)
H A.
3734-51
4861-52 <
I*
F)
H/£
3722-08
4340-63 (near „
G)
H V
3712-11
4IOl-90(
n
h)
Hf
3704-00
3970-Sa (
n
H)
Ho
3697-29
3881) -30
Hit
3691-70
3935-53
Hp,
3686-97
379S-04
Ho-
36S2-9&
3770-77
Ht
3679-4d
3760-30
H V
3676-40
^K Theoretical limit A 364613.
^^ This series was believed to be solitarj' until Professor
Pickering announced, in 189V* bis identification of a com-
panion-set of line.^ in the peculiarly constituted southern star,
^ Pnppifl. Much knowledge had by that time been gained
regarding spectral aeries. The pattern set by hydrogen had
been foxmd to be conformed to, with variations^ by the
^ WiedemMHi'fl AnnaUn, Bd, xxv. p. 80.
* Han/dbueh d<r Spietros'wpie, Bd. ii. p. &06.
• AstTOph, Ji»tmal, toL t, p. $2,
40
THE SYSTEM OF THE STARS
eimssions of a number of other subetanced ; and what might
be called a typical arraagemeiiC of three series linked together
by a slightly modified common formula^ had come to be recog-
niaed as prevalent. This triple set consists of two " subordinate *'
series^ conveiging towards the same Lmiting wave-number^^ and
a " principal " Beries, composed of much more widely separated
lines. Now Pickering's series is constructed accordantly with
Huggins'g seriea ; it runs up to an identical " head " in the
ultra-violet; and was hence at once» and beyond the possi-
bility of mistake, associated with hydrogen. Yet it cannot
be procured artificially. We are entirely ignorant of the
conditions under which it is displayed. It is only certain
that they prevail in early helium stars^ and have become
abolished by the time the Sirian stage is reached.
The fact is a memorable one that the true character and
full extent of the hydrogen -spectrum became known through
astro-physical inquiries. It shows with what curious un-
expectedness the obligations of one science to another may
be repaid, and exemplifies the advantages to be reaped by
terrestrial chemistry from extending its experimental range
to the heavenly bodies. The " white star " set of rays has
fumiahed a clue to many a spectral labyrinth, and its under-
lying principle of order has been proved, by extended
laboratory -research, to be of vital importance in molecular
physics. The modulated behaviour of different rhythmical
series under varied treatment is profoundly significant, and
indicates one of the most promising methods for probing the
secrets of material structure and ethereal relationships.
DisproportioE in etrength between hydrogen and metallic
lines reaches a maximum in the spectrum of Sirius, a section
of which, from a superb Harvard photograph, is shown in
Plate II., Fig. 2. Helium makes no effect in it; and the
change of type from e Orionig could be discerned — even if
every other symptom of it were absent — from the substitution
for the " blue " hehum-line (at X 44Y2) of a dark magnesium-
ray slightly less refrangible. This trait of magnesium -absorption
is relatively much stronger in Sirian stars than in the eun and
his analogues; and a particular meaning is lent to the dia-
* W»Te-numherB, or fi-aquenoiee of Tibrition, »» the reciprocala of waTB*
]eugthE>, and are klwajA substitatod for them in nimierical calcDlationa.
THE STABS AS STJNS
41
crepancy by the circumstance that the line in question iB (in
Sir Norman Lockyer's phrase) " enhanced " in paaaing from the
electric are to the spark Silicon is the only non-metallic
element besides hydrogen identified La Siiius \ and here again,
t^e identification i^ by means of lines intensified in the electric
epork.
An erpoeura of eighty-two minutes^ with the 13-inch Boydeu
la&actor, was given at Areqtiipa to the negative from which
Plate 11., Fig. 3, is copied The spectnim represented is that of
the niagDi6cent Canopua {a CariniE), The diminished width of
the hydrogen 'lines, and the augmented conspicnousness of the
calcium K> signify a decline from the condition of Siriua
towards that of our aun. Many distinctively solar lines have
aaeerted themselvea \ yet no less than twenty members of the
hydrogen -series may still be eeen or photographed, while only
four can be clearly made out in the sun. There is reason
to believe that the measure of their affluence givea a searching
L -test of stellar constitution.
IH Although the hydrogen spectrum is dominant throughout
the first order of stars, it is not in all represented with equal
empham The diifuee lines constituting it in Sirius and
Vega show, in descending gradations of fineness, in Castor,
IFomalhaat, and Altair. They appear, moreover, less solitary
in proportion as they become less intense. Their all but
eiclueive posfiession of the ultra-violet field is progressively
encroached upon by the development of other spectral lines.
The co-ordination of the two kinds of change may be expressed
by the general statement that the prmninenci of Tays dut to
ahtorption hy metal& in the speeira of whiU Btars varies in-
veruly toiih Chat of ike hydrogen, series. When the hydrogen-
niys become eflaoed from the invisible, and cease to dominate
the Tiaible part of the spectrimi, the second, or solar type of
stars is reached
These are about one-sixth less numerous than the fiist
kind. We may tafce aa examplea : Capellaj a Ursfe Majoris,
a Casaiopeiae, a Arietis, c Carimje, a Serpeutis, Aldeharan, and
Arcturua. The pole-atar, Procyon, a Leporis, and a Persei,
stand nearly midway between the two groups.
A golden tinge like that of sunlight betokens, in stai^ of
tfafl second order, a spectrum more or less perfectly similar to
THE SYSTEM OF THE STAHS
that of the sun, delicately ruled from end to end through the
absorptive effects of a great variety of metallic vapours ; non-
metallic Bubstaacea are lepreseuted only by hydrogen, itasociated
in the sun with ailicoa, oxygen (a trace), and carbon. Th«
extent to which the Unea are crowded together may be judged
of from the photographed spectrum of Capella depicted in Plate
IL, Fig. 4. Dark hydrogen-rays are present, but with no pre-
eminence, and No. 5 of the aeries (He) probably lurks concealed
within the shadow of an obscure dififuse band which covers its
place. This hand was named by Praunhofer H, and its com-
panion, a little higher up, is designated K. The pair form the
moat strongly^marked feature of the spectrum of calcium when
raised to the highest pitch of incandescence ; the ordinary
tiame of the substance shows them but dimly.
They are peculiarly characteristic of the spectrum of solar
prominences. Daylight observafcions at the edge of the aan
disclose them as invariably brilliant in the chromosphere, and
shining up to the very summit of each one of its flame'like
extensions. Moreover, during the total eclipse of May 17,
1882, the violet radiance of H and K Eooded the shadowed
part of our atmosphere, and dimly UluuiinatLng the purple
diBC of the moon, was scattered far out among the " aig;rettes "
of the corona.
Corresponding symptoms of the phenomenal importance of
calcium-vapour in the aun'a economy had been already de-
tected by Professor Young in the course of his daylight
epectroecopic obaervatioas. But they were not fully appreciable
until photography was made available for their continuous
investigation. H and K lie at the verge of the visible
spectrum ; the eye perceives tham with some difficulty ;
while the chemical retina is extremely sensitive to their
vibrations. Further, the black bands due to their absorption
have, in the Frannhofer-spectrnm, dark shadings symmetri-
cally attached to them, by which the bright rays of the
same refrangibility used in prominence -photography are
eflectively sheltered againflt atmospheric glara This con-
venience was amply turned to account when Professor Hale
and M. Dealandres independently adapted to the purposes of
daylight solar photography Janssen's invention of a double
slit for isolating individual qualities of light. In particular.
d
THE STARS AS SUNS
43
it led them both to the discovery that the sun's diac is over-
spread with wreathed ghapea of glowing calcium, designated
by Profeesor Hale " flocculi," and regarded aa expansions
of vaporoufl niaaaea^ lying at the base of the chromosphere,
uid fed hy mounting torreute &om the Bun'e interior.^ The
intensity of their radiation appears anomalous, and may, he
thinks, need to be explained otherwise than by mere elevation
of temperature.
Presumably, all solar etara poaaees calcium -appendages
eqnally well-developed with those of the sun. Their epectra
are impressed with the same powerful H and K abaorpfcion ;
and it is hardly conceivable that a stamp so peculiar^ and
to emphatically impressed, should have a different meaaiug
in them from that deciphered in the one star accessible to
interpretative research. The calcium H falls, neverthelese,
very near indeed to the hydrogen He (see Plate II., !Fig, 3),
the difference of their wave-lengths amounting to no more
than one ten-miUionth of a millimetre, and it lb only on the
best negatives that they can be separately distinguished.
Usually^ either the hydrogen-line is so widened as to mask
the calcium-line, or the calcium-line as to enwrap the
hydrogen-line. Professor Young, however, saw them side by
gide, bright, during his observations of prominences in 1879-
1380 ; and they appeared dark in a photograph of the spectrum
of a Cygni taken at Harvard College, November 26, 18&6.
In this star, a spectrogram of which, taken under Professor
Pickering's direction in 1893, ia reproduced in Plate IIL. Fig.
1, the hydrogen rays have thinned down almost to their eolar
condition, while other metallic lines are tine yet pronounced.
Such a critical balance of conditions alone made possible the
individnalisation of the two lineB on the earlier Harvard plate.
Thus, while the double origin of H opens the way to
mifiunderstandings, the state of the calcium-line at K is a
most usefol index to the physieal condition of a star," Next
to the mode of appearance of the hydrogen series, it is
perhaps the feature most deserving of study in analysed star-
light. The substance emitting both K and K is evidently
of first'rate importance among the vapours surrounding the
^ FuiAi<aiwtu of Vu Ytrkes OhKTvntoryi yo\. iil. parti, p. 16.
=* A3 Sir William Huggitts pointed out in 137&.
44
THE SYSTEM OF THE STARS
sun. And th^Lt it is, In fact^ the metal calcium in a highly
rarefied state, was proved by the expeiimentB of Sir William
aud Lady Huggine in 1897.' The hypothcBia of its dis-
Bociation in the 8iiu thus remains unverified. It is true
that the twin-lines H and K difler in their relationships from
most of the other ccmponent-rays of the calcium spectrum.
They stand aloof from any arrangement into seriea ; they
exhibit special effects under pressure^ and — ^we may add with
approximate certainty — in a magnetic field. Such personalities
of behaviour in Bpectral lines are familiar in the laboratory
as well as in the heavenly bodies They do not e^m to
iudicate a compound nature (as ordinarily understood) in
the emitting element; yet they undoubtedly suggest a lesa
rigid uniformity of structure among its minute vibrating
particles* than had, until reeentlyt been held compatible with
the accepted principles of physical cbemietiy.
Some alight diversity of detail is to be found among
Bpectra of the second type. In the main, however, they are
cloeely alike ; and the chemistry of the sun may be called
normal for all his congeners. The model solar star waa
long supposed to be Capella ; aud it is true that in the
invisible, as well as the visible part of its prismatic light, all
the characteristic solar groups exist iu about their solar
strength. Dr. Scheiner identified with extreme precision
255 lines photographed from Capella (between wave-lengths
4124 and 4638)* with lines derived from the sun;' and it
appeai-ed reasonable to infer an almost perfect constitutional
simihirity between the two bodies. Capella has since, never-
theless, provetl to be a double star with a compound spectrum ;
and the secondary component gives light resembling that of
Procyon or Canopus more than that of the sun. Thus, the
ultra-violet hydrogen-lines distinguishable in the joint spectrum
belong to this star, and not to the primary body, which is
genuinely solar. In the sun itself^ the hydrogen-series has
no more than four representatives. Professor Ames was able
to ascertain, through the cloak of calcium -absorption, the absence
of Hf, its fifth member ; * and some vague shadings, noticed
^ Astroph. Joumaii vol. vi, p. 77.
=* Rftyser, BandbueK der SptctroKopte, Bd, i, p. fi7fi.
^ JwtT. Naeh,, No. 2»23, * F%il. Ma§. ToL xa. p. 54, cerioB t.
THE STARS AS SUNS
45
hj KowUnd oear the poeitionfi of ^me of ita more refrangible
associates, are of imcertuiii meaaing. Solar stars of pure
type should, thea. display four, and only four, ilark r&ys of
liydiogBn ; the presence of additional onea givea nee to a
suspicion of duplicity. The chief member of the aouthern
slar-pair, a, Centauri^ again oETers a perfect example of a sun-
like spectrum ; and this stai^ being the sun's equal in mass,
may be concluded to be similar to it also in temperature,
dftnfiity, and light-power. The usea, for purposes of com-
paiifloUf of an authentic model-eun have been expressly
idierted to by Sir David GiLL
In Aldebaran tbia standard is pretty widely departed
from. The pale rose tint of its light is accounted for by the
sUghtnesa of abeorptive e£fectB in the red end of ita spectrum,
while numerous lines modify the yellow and green, and the
violet rays are so feeble that, with an exposure yryily times that
required for Siriu^, Sir William Hugginsj ita original spectro-
grapher, obtained only an impression virtually conterminouB
with the perceptive range of the eye. This feebleness of
chemical action is perhaps due, not to intrinsic deficiency of blue
light, but to its stoppage in the vaporous envelope of the star
The spectrum of Arcturus (a Bootis) varies from the solar
pattern in the flame direction, though not to the same extent,
wi that of Aldebaran. A section of its blue part is copied in
Plate rV,, Fig, 1, fi^m a photograph taken by Profesaora Frost
and Adams in 1903 with the great Bruce spectrograph of
the Yerkes Observatory. Spaik-lines of titanium fuinished
a comparison-spectrum ; and the emphatic nature of the coin-
cidences gives an idea of the strength of absorption by that
metal in the star's atmosphere. In the sun also, titanium
plays a remarkable part. The lines due to it, although
mostly faint in the Frauuhofer spectrum, come out with
augmented intensity in the spectra of agitated spots ; and
the copious photographic record of its emissions, especially aa
obtained by Mr. Everahed during the Indian eclipse of 1898,
assign tt a place among the permanent constituents of the
solar chromosphere and prominences.' In the spots and
eruptive appendages of Areturus, we may be reaaonably sure
that it is still more plentiful and active.
i ICftimder, The Indian ^i^pse, p, 70.
46
THE SYSTEM OF THE STABS
No line of demarcation can be drawn between helium
and Sirian stairfc on Ibe ont^ band, or between Suian and
6oLar stars ou the other. And the presumption is strong that
the tiHDBition from each class to the next is ejected bj actual
deyelopment ; that the same object passes successively throngb
the indicated changea The chief reason for hesitation in
adopting this view is that the various stellar oiders are not
indifferently scattered over the heavens ; but we understand
very little of what such distinctiouB really imply. There ia,
besides, some direct evidence that heiium stars are those moat
recently condensed from nebulje. Some of them appear to be
as yet not wholly detached from their cloudy matrices ; while
Sirian and solar stars, although they may be projected casually
upon a nebulous background, are probably never, in point of
actual fact, nebuloua. Kor ig the eupposition admissible — aa
the case stands at present — that helium stars can progress
to the solar condition otherwise than by the prescribed route.
The intermediate Sirian type must apparently be conformed
to before the third station on the long journey comes within
reach. Some authorities, it is true» believe that it may be
dispensed with, and that a Cygni is an example of stars
traversing this evolutionary short-cut ; ' but the better
opinion is adverse to such a possibility.
We may now briefly reconsider the course and kind of
modification undergone by the stars^ so far as we have yet
taken them into account In the first place, there is a steady
increase of general absorption. The light of Bellatrix (7 On-
onis), for instauce, attains outer space substantially aa it
left the star's photosphere. Its native bluish tinge subeista;
the proportionate intensities of its variously refrangible
sections remain unaltered. But our sun's proper atmosphere,
or *' emoke-veil," arrests a large percentage of his violet radia-
tions. The solar disc is, indeed, quite brownish near the
edges, because near the edges the light cuts obliquely through
the reddening strata, and suffers in consequence heavier
encroachments. Could they be stripped off. the sun would
blaze with at least once and a half times its present bright-
ness, and would show a steely lustre very different from the
golden radiance we are accustomed to. There is hence no
' Scb«<iD«r, P^tdam PuHieationent Bd. tII. TI1. ii. p. 331.
SteJlur Sjiectrn nf three Tyi"'*.
Vx, Siwi'trmu uf ArcturuH wiih TiUmiim Com]Mui»on-Si*ctt-Hin (Frost).
S]i«tTiiTii urn? Ct'ti (rifkeriwg).
THE STABS AS SUNS
47
warrant for aeaerting that the emissive outpourings of solar
ort» differ intrinaicaU)- from those of Sirian or of helium
fitaiB. It is certaiB ooly that they are strongly inodilied by
elective abaorption which has no appreciable effect upon
spectra of the earlier types.
The signs of speciSc abfiorption» as helium grow into solar
stars, alter by insensible gradations, but according to a
viaiblj conaistent method. From beginning to end qf the
series there 19 a steady increase in the number and intensity
of metallic lines, very notably in those of iron, whichj next to
the giant-bands of caJcimn^ constitute the dominating feature of
the solar spectrum, yet are imperceptible in the prismatic light
of Bigel and BeUatrbc. Absorption by helium and oxygen ^
comes in at the start, but has a strictly limited time-range.
It scarcely brooks competition, sharing the field only with
hydrogen in its terrestrial and cosmic forms ; metals, in the
earliest stars, showing only by a faint streak of ma^eaium.
As they begin more numerously to assert their presence,
helium lines become effaced, and those of hydrogen attain
their mwdmiun development. But the Huggine-series is now
alone repreaented, for the Pickering set is even shorter-lived
than the helium rays, and it appears exclusively in what are
supposed to be the earliest stars. This is an extraordinary
circumatance, most battling to comprehension. There is no
other known instance of such independent behaviour on the
part of a spectral aeries. Nor can its meanings in the total
I absence of terrestrial experience, be interpreted by so much
j^ a plausible conjecture. If the Pickering lines could be
feduced to show in vacuum-tubes some basis would he supplied
pbr reasonings on the subject ; but attempts to elicit them
have, so far, proved altogether fruitless. It is also important
' to remember that, in the stellar succeasion, the character of
I metallic absorption changes as well as its strength. The few
traits of it which appear compatible with the display of
I helium are — in Sir Norman Lockyer'e phrase^'* enhanced '^
lines ; lines which vivify notably when for the illuminative
agency of the electric arc a disruptive spark -discharge ifl
' FroHt ojid Adaina siupecl that ozygen-Btart may be trrayernDg a road
pamUel to the maia tr&ck of evolution. FabL l/niversity of Chicago, vol. riiL
^1(I7.
CHAPTER IV
THE CHEMISTRY OF EED 8TAKS
Kbarlt aU Stars of a pronounced red colour show Bpectra
crossed by dusky banda of absorptioii. Two varieties can be
at once dificriiainated. They respectively form Secchi's third
aad foarfch types. Kow epecti-a consisting of bands or flut-
inga are given out in the laboratoiy by coinpoimd eubatances,
tsach as oxides and chlorides, as well as by the chemical
elemente glowing at a low pitch of excitement. They were
formerly thought to originate from molecular, line-spectra from
Atomic vibrations. But this opinion has been much shaken
by recent experience/ Trowbridge and Eiehardg concluded
in 1897* that, where electricity is the illuminating ^nt,
an oecillatory discharge gives rise to iaolated rays, a " dead-
bd&t'' discharge to flutings. And it is easily understood that
Buccesffive shocks of transmitted energy should evoke more
intimate thrillings than an even flow. Electrical stimulation
of any kind is not, however, necessary for the production of
banded spectra ; the cool oxygen of our own atmosphere
stamps the red section of dispersed sunlight with three
conspicuously dark flutings. Moreover, a profound difference
in the relationships of the two kinds of spectra is signihed by
the insensibility of fluted emissions to magnetic influence.
They evince no trace of a " Zeeman effect " ; they remain
unaltered and imperturbable in the field of the most power-
ful magnet Pressure is similarly impotent to modify their
wave-lengths or structure. Tliey are, however, displaced by
1 B«8lukdroa, CvmpUt Jiendus, t. crxxrii. it. 1013, Deo. 14. 1903.
* Anuriean Journal of Seimet, vot. iii. p. 117.
4ft 4
50
THE SYSTEM OF THE STARS
radial motiou in the same maiiDer, Aod to the same extent, as
linear emiaaiouB.
FititiDgs are made up of uumerous iodividual lin^ set
more and raore cloeely together towards the " head," and at
continually widening iutervaU towards the '* taiL" They in
fact constitute series, on the model of tlioee of hydrogen and
helium, but: condensed into a much smaller space. The
numerical formuljs repreaentiug the principle of their con-
BtruL-tion have, since 1885, been investigated with a fair
promise of success, first by M, Deslandrea/ later by M. Thiele.'
Enough has been done to show that the arrangement both of
bands in the same spectrum, and of lines in the same band,
is methodical, and may eventually be rendered intelligible ;
but the underlying lawa are too intricate for immediate and
full recognition.
In the stars, fluting-absorption is 3uj>eradded to absorption
by lines. Metallic groovinga, agreeing in position with those
of the solar spectrum, but somewhat reinforced, aa a rule, in
strength, aid the interception of photospheric radiationa
dimmed further by a " smoky " envelope chiefly arrestiTe of
the shorter wave-lengths. Thus, three distinct forms of
jibaorption mark their effects in banded spectra, and seem to
betray the action of deep and dense vaporous strata. Hence
the redness of the stars. And, because their photographic
rays are largely cut off, they come out on sensitive plates five
or six times fainter than they appear to the eya Their
spectra, too, ate recorded with much difficulty. In some
nearly all the violet^ and all the ultra-violet, light is extiu-
guiflhed ; while their blue beams are enfeebled by crossing a
triple barrier of absorption. For purposes of effectual investi-
gation, accordingly, orthochromatio plates have to be em-
ployed ; and these are not free from inconveniences and
drawbacks.
From Autares {a Scorpii), a remarkably fine specimen of
the third stellar type, Sir Norman Lockyer has conveniently
designated its members " Antarian stare," The fiutings in.
their spectra terminate abruptly towards the violet, but shade
1 Compfes J^cridu$, tc. p. 1256; ibid. Oct 17> IWl ; Eaywr, Bandbueh
dir Spectroscopie, Bd. ii. p. 175.
^ Aitrc^h. Jounu^t toI. tl p. 65, vliL p. 1.
TJtE CHEMISTEY OF BED STAHS
51
if pida&Hy towards the red, pnxluciag to the eje something
^1 colonnaded effect. This, however^ is loat in photographs ;
puti/ becaxise the flutiugs are discontinued in the higher
^eccnil ranges, partly hecause the general impression is over-
le by the wealth of self-recorded details. All spectra of
th^ kind are constructed on the game fundamental design.
princip^ bands, of which ten are counted, reappear with
tial invariability in every Antarian star.' A homogeneous
is thti9 suggested for them. It is unlikely thut many
each acting independently of the others, are con-
in the weaving of a pattern widely diffused, and
pxaclically unchanging. Yet their chemical interpretation
long remained a source of perplexity. Thii-d-type absorption
^ no known analogue until Mr. Fowler, in 1904,^ thought
^ comparing it with the Sutinga emitted by titanium oxide,
tntdeied luminous by low-tension electricity. They were found
to coincide very approximately with eight out of the ten star-
baods; and particular resemblances in the arriiogeraent of
kaea within the tlutinga emphaaiaed the general agreement
Stellar spectrsi of the third type thus promise iinally to yield
Dp their setsrot ; for it must be, at least provisionally, admitted
ihdt titenium playe a leading part in giving them their
channelled a8j)ect. Cyanogen flutinga, too, have been photo-
graphed in these stars by Prafe-'ssor Hale and Mr. EUerman ; ^
1 they are of shorter wave-lengths than any of the bands
ily measured They constitute a novel featui'e of
.on interest, as the only symptom so far recognised of
,ce of carbon, or its compounds, in third-type stars.
Aldebaran, although a solar star, ia unmistakably of a
reddish tinge. The blue end of its spectrum is heavily
ptMCured ; and the tiutiugs chariictmstic of the type towards
which it aeems to be advancing are just indicated as embryonic
I^MMlings. The object might be called a Unking instance
between Arcturua and Betelgeux (a Orionis), in which titanium
latingB (if we may bo designate them) are fully developed,
irhilo the main features of the Franuhofer spectrum remain
and uneffaoed. The least possible departure is made
52
THE SYSTEM OF THE STARS
from the aolar model that is recoadlable with the complete
presentment of a different type. Bj'oomparing Plate II. » Fig.
4j with Plate III., Fig. 2, our readers can estimate the close-
nenB of the analogy between the linear elements in the spectn
of CapeUa and Betelgeux. The four lo^'^st lines of hydrogen
are ikirly stroag in Betelgeux ; but in specimens presumed to
be more "advanced" they thin out, and perhaps disappeftr
with the dosing in of denise banded absorption. A fine led
Btar in the Southern Cross, y Crucis, ia of nearly the same
standing as Betelgeux ; in a H^ercuUs the bands have acquired
strength through the efflux of time, it Is supposed, and the
progress of cooling.
Eight or nine metals are easity reoognidable by their
abaorption-liues in Antariau spectra. Calcium is the most
prominent. The notable pair of difluse stri^ies in the violet
due to it are fully the equals of their archetypes in the sun ;
while the llame-line iu the blue, X 4227, shown as a black
bar bisecting the spectrum in Plate IV., Fig. 2, is of greatly
augmented intensity. Iron comes next to calcium in elective-
neas for ligbt-stoppage; and with it are associated magnesium,
sodium, chromium, titanium, vanadium, aluminium, strontiiun,
and probably manganese. No lines distinctive of the electric
spark are present; but those widened in sun-spots stand out
significantly.
Red stars, as we have said^ are encompassed with power-
fully absorptive atmospheres ; and atmospheric density and
extent are, for some recondite reason, accompanied by in-
stability in shining. The radiative machinery tends to become
clogged fitfully, or at definite intervals^ and irregular or
periodical variability results. Nor do the spectra of Antarian
stars remain imafTected by these vicissitudes. Their con
tinuous radiance brighteuB and fades unequally in its differ-
ently refrangible sections, though according to no traceable
method; the bauds interrupting it alternately close in and
thin off; above all, vivid rays of hydrogen and other eub-
stances are kindled with the recurrence of the brilUant phases,
and die out as each fresh outburst of energy becomes exhausted.
This striking feature was first detected in a spectrogram of
Mira Geti taken at Harvard College in 18S6; and scores of
" long-period variables " have since, through Mrs. Fleming's
THE CHEMISTKY OF RED STAKS
53
been recognised by their exbibition of the Bame
peculiantj. Only two of them, however, have as yet been at
all ftdeqoately studied. Mira has been made the subject of
«OQie admirable mveatigations at the liek Observatory; unil
^ Cygni has been dealt with to good purpose at Potadam
dnring some of its recent ma^dma.
The character of the flpectrum of Mira is well ahawn in
Plate IV., Fig, 2, reproduced, by the kind permission of
Profe^eor Pickering, from a Harvard photograph. The two
Uae hydrogen-raya (Hy and H£) emerge resplendent ; yet the
gxeen and violet linea (H^ and Hs) are alike imperceptible ]
while four of the ultra-violet sequence shine brilliantly.
Professor Campbell ascertained by direct observations with
the great Lick refractor at the high majcinium of 1898, that
the crim;&ou hydrogen-line makes no show in this star.^
Kevertheleas, in vacuum-tubes, in the solar chromospliere, and
in bright-line helium stars, C is the most vivid lueuiber of
the series. In nebuhe, on the other hand, it is usually
invidble ; and thus the unexpected conclusion is forced upon
us that hydrc^en glows in the great irregular nebulffi under
similar conditions of excitement to those prevailing in variable
Antarian stars. The suppression of the fifth line (He) is
universal in anch objects, and was believed to be complete
until the missing radiation faintly recorded itself on some of
the spectrograms of Mira lately secured by Messrs. Wright
and Stebbins at Liek. It seemed to glimmer through a dense
Uyer of calcium, the nearly coincident absorption of which in
g^eral masks it effectually. This explanation, however, needs
to be further verified. It has much to recommend it ; yet it
inTolvee an inversion of the order of stratification, as regards
amitting and absorbing vapours, commonly observed in stars.
The tripling of the hydrogen -Hnea in Mira, noted by
ProfeaaoT Campbell in October 189S, is highly suggestive of
niftgnetic action. But the effect, though eagerly looked for,
has not since recurred, and appears to betoken exceptional
agitation. On the sain© occasion, two iron-liuea, previously
ngistered as dark, came out conspicuously bright; and they
were again brightened at the maximum of 1902, together
with a number of others, including the principal arc-line
^ Attroph, Jmtm. toL is. p. SO.
54
THE SYSTEM OF THE STABS
of silicon at X 3906. Mr Joel Stebbins^ followed the atar
spectrograph ically down to a nmuiimm at ninth magnitude
in January 1903. when a six hours' exposure barely sufficed
to procure a legible, though not a measurable impreasioa from
rays shorn of the adventitiovis glory lent to them by transitory
gaaeous incandescence. The phenomena attending the brilliaiit
phases of x Cygni, as observed by M. Eberhard,^ are essentially
aimilar to those displayed by Mira.
About 15 per cent of third-type stars are establiahed
variahlea ; and few shine with the constancy of an average
white star. Moreover, those subject to the widest vicissitudes
have, on the whole, spectra the least like that of the sun.
They seem to have descended furthest along an inclined plane
of change, for there is no evidence of abrupt departures from
what was presumably the more primitive type. The dis-
tinctions between our sun and a Mira-variahle« though
strongly pronounced, may have been brought about by in-
sensible gradations ; and the inference invites, if it do not
command our assent that no halt can be cried in the evolu-
tiouary journey from a stable condition of sun-like luminosity
to the stage of turbulent incandescence marked by the ruddy
flare of recurrent maxima.
The apeetra of fourth-type, or "carbon -stars/' resemble
those of the Antarian kind in being marked by linear, as well
as by banded absorption. Their aspect to the eye is illustrated
in Plate IV., Fig. 3, copied from M. Dun^r'a drawings by
permiaaiou of the University Press of Chicago. From the first,
Father Secchi recognised the carbonaceous origin of the three
deep shadings, distinguished in the Figure as B6, B9, and BIO.
They face redward (to the right), and match respectively the
yellow, green, and blue flutinga of the so-called "Swan"
spectirum, derived, according to some authorities, from pure
carbon — according to others, from carbon monoxide. But
these stars are, without exoeptiou, faint ; the brightest is of 5*3
magnitude ; and beyond the preseuce of some strong lines
due to iron and sodium, little further could be learned about
them until more powerful optical means became available.
The completion of the Yetkes 40 -inch refractor at last
* Aatropk. Joum. vol. Kviii. p. 341.
* IhU. vol. itvUi. p, 20a.
THE CHEMISTBY OF BED STARS
55
supplied tbe needed facilities; and in 1893 Professor Hale»
aasisted by Mr. EUerman, undertook the spectrograph ic in-
vestigation of fourth-type stars. Their overwhelming aelf-
AbeorptioD in tha blue made the task seem unpromising ; but
by the employment of isochromatic plates of different quality
for the several spectral aectious, together with exposures up
to twenty-four hours in duration, it was successfully executed.
The definite results, published in 1903, are of the utmost
Talae.^ They refer more particularly to eight stars, the
tions and places of which are as follows :- —
Nuns.
B.A. (IMUX
OaaQWO^
»«.
74 8elu«IlBnip
75 BnlueUeTap
llA Schlellenip
132SchjeUBnip(=UHrdi») .
3IS BinDJDgham
152 SclijeUenip
Id Fiscitim ....
280 Schjellerup
8b]9Bt4B*
a 29 40
8 49 4fi
10 32 36
10 38 a
12 24 2e
23 41 17
'2S ee 10
+ 14' 47'
+ 38 32
+ 17 37
-12 62
+ 67 68
+ 45 59
+ 2 &d
+SB 4S
6 -a
«-5
«-6 (vw.)
6-4
5-8 (v*r.)
7-6
Of the above, six are known by their numbers in a
CaifUogu* of lUd Stats, drawn up by the Danish astronomer
Schjellemp in 1866 ; one ia taken from a similar work by
John Birmingham of Tuom, dated ten years later; and the
eighth and brightest was enrolled by Flamsteed. On the
Yerkea plates of their spectra no leas than 307 dark lines
were measured, and in part traced to their origins. They
indicated the undoubted action of ten substances, namely,
hydrogen, calcium, titanium, vanadium, iron, aodiumj mog-
lieaiuin, chromium, nickel, and manganese, and suggested that
of others. The record of cyanogen-flutings in the bine (see
Plate V,) constituted in itself an important gain to know-
lodge; and still more the discovery that bright lines are
profusely scattered among the dark elements of such spectra.
This bad been to some extent perceived by Father Secchi ;
but his observations were only rescued from the discredit into
which they had fallen by tbe sure testimony of the camera,
Lt present some two hundred rays of emission have been
^ DecenniAl Publieaiioru of the Univernty qf Chicago, vol. riii.^ fVom which
PlfeU V. ifl Tcproduoed^ by the courtes^y of the ITuiventty Press AuthDri'CioH.
56
THE SYSTEM OF THE STARS
determined ia carbon- stars, althotigh one only h&& been
eecurely identified. This is the bydrogen-F, which at timea
(for itB condition is subject to change) shines conspieuously in
the peculiar star 280 Schjellerup (see Plate V., uppermoat
apectrum), and more diinly in a few other members of the
class; while, in 19 Pisciura, the blue and indigo hydrogen-
lines are dark, and no trace of F, bright or dark, is to be
found. Of the remaining crowd of vivified rays, some may
be due to oxygen and nitrogen, one coincides with the funda-
mental member of the Pickering-eeriea of hydrogen, and three
or four besides fall very near emiesion-rays in gaseons Btars of
the " Wolf-Rayet " variety. On the other hand, the absorption-
spectra of carbon-etara are extensively oompo^ of lines widened
in Hun-apots ; the metallic spark-lineB characteristic of early stars
have vanished from them, and been replaced by arc and flame-
lines> held to be an unfailing symptom of advanced stellar age ;
and it is associated with variability in light even more pro-
nounced than that shown by Antarian stars. Professor Hale's
general conclusion is that third- and fourth -type stars "should
be elaeaad together as co-ordinate brunches leading back to
stars like the sun," from which they probably develop through
loss of heat by radiation.^ That is to say, an outworn solar
atar may descend to extinction by either of theee alternative
downward paths. But why one is chosen rather than the
other remains obscure.
Two circumstances are, however, adverse to the view that
suna like our own are liable to degrade into carbon stars.
The 6rst is the lack of intermediate specimens. Profeesor
Hale urges the plea often put forward by embarrassed palae-
ontologists, that the record is incomplete ; and it may well
prove valid. He has already picked iip some stray connecting
links, and it would be premature indeed to despair of more
being found. But there is another very serious difficulty.
It relates to the distribution of the stars. Those of the
fourth type are strongly condensed towards the Milky Way.''
Their relations to the fundamental plane of the sidereal
system are quite different from those of solar stars. More-
' Decennial Pi^lusaticns, vol. via jx. 136.
' DuHtr, ilpteiret de la Troitiem^ CioiU, p. 126 ; Porkturet, Aatn^h. Joum,
tqL ix. p. 230 : Espm, ibid. toI. x. p. 169.
THE CHEM^STBY OF KED STAES
57
they &P6 evidently extremely remote. They eeem to
occupy a region of space apart from that tenanted by our sun
and his congeners. The incongruity is then obvious of sup-
posing that they are united with them in a single evolutionary
verier.
About 250 carbon etara have, so far, been registered.
Many were detecteil visually by Mr. Espin ; but Mrs.
Flemings photographic gleanings have contributed largely
lo swell the total Seven out of the 250 can just he seen
with the naked eye ; the rest are telescopic objects. Oue
of the finest specimens is Secchi's " La Superba " (152
Schjellerup)^ situAted in Canes Venatici. It was so entitled
for the extraordinary vivacity of its priflmatic rays, separated
into dazzling " zones," red, yellow, and green, by broad spaces
of profound obscurity. This Btar ahinea with approximate
constancy; 19 Piscium at times surpasses it in brightness,
but is subject to temporary deprivations of more than one-
half its light. These happen irregularly ; many periodical vari-
ables, however, belong to the same spectral type, among them
XJ and V Cygui, S Cephei, V Hydrje, and K Leporis, noticed
by Hind for its intense crimson colour.
The comparative dimness of all such objects, though
doubtless in part due to their great distance from the earth,
is readily explicable by the opacity of their atmospheres.
How much of their intrinsic light escapes absoiption can
only be conjectured ; if we put it at a tenth, our estimate
is likely to exceed rather than fall short of the trutli.
Only loopholes, so to speak, are left for its exit; and, as
usual, the violet and blue rays suffer most severely, being
indeed almost completely smothered. The special depth of
colour in carbon stars is thus accounted for. They are not
merely suffused with red, like Betelgeux and Antarea ; they
actually simulate the glow of carbuncles or rubies in the field
of the teleacope. Vast and magnificent orbs must be found
among themL Under circumstances less disadvantageous^
some might well take rank in the second magnitude of Siriau
»nd solar stars ; and this apart &om any allowance for their
apparently exceptional remoteness. The final darkening and
death of fourth-type stars may then be reckoned as a con-
tingency too far off for definite realisation.
CHAPTER V
GASEOUS STARS AND NEBULA
Gaseous stars form a restricted aud peculiar class. The
objects belonging tu it are characterised by the display in
their spectra of isolated bright and dark lines on a mom or
lesa perfectly continuous background. They present \m then
with a triple combination — a direct gaseous spectrum, r
reversed gaseous spectrum, and a spectrum due to glowing
solid or liquid matter, all simultaneously made manifest by
the unrolling of a single scroll, yet each originating under
very different conditions. The true discrimination of those
conditions tasks all the resources of physical eidereal
astronomy.
The state of bright emission is in 8om.& stars normal, in
others it only supervenes as part of a great general increase
of light. It ia not limited to any one period of sidereal
existence. Stars barely condenaed from nebulae sometimea
show bright lines, and the symptom is (as we have seen) apt
to recur at the advanced stage reached by red stars with
banded spectra. Only Sirian and solar stars are exempt
from the tendency ; helium stara are peculiarly liable to it.
It would thus seem that tlie stars capable of yielding mixed
spectra of absorption and emission are those either unfinished
or verging towards decay, while, during the iutermediate
epochs of vigorous maturity, absorption is alone effective.
The term " gaseous," however, should be reserved for inchoate
orbs. Those giving bright lines are probably distended
far beyond the solar proportion of size to mass ; and their
spectra bear the distinctive marks of helium, frequently of
cosmic hydrogen, and not rarely of oxygeu and aitrog:en.
fid
d
GASEOUS STABS AND NEBULA
59
They have the farther diBCinction of showing the oidinary
lirdfogen -series — the Huggins-series — in duplicate, a bright
Une being coupled with, or Buperposed upon, a dark one of
identical origin ; and the rule first adverted to by Professor
Campbell ^ is invariable that, under these circumBtances,
ibaorption becomes atraager, and emission feebler with
dimiQutiou of wave-length. The brightest lineSj^ in other
worda, are the least refrangible. Alcyone in the Pleiades is
aa example. In this Btar one solitary ray is vivid, and it ia
the fundamental (Ha), which glows cnjuBon beeide a dark
CDmpatiioo. Plelone in the same group, on the other hand,
and many stars besides, exhibit the direct radiance of several
members of the hydrogen-aeries ; but that of C always pre-
dominates. Similarly in the various helium-series, the stress
of brightness is inevitably laid upon the lowest of their
constituent lines. But to make this apparent, the fieries
most be sorted out ; for the rule applies to each individually.
An analogous order of progression was subsequently found by
Professor Hale to regulate the reversal of lines in metallic
spectra,^ As the vapours rendered incandescent by the
electric spark taken under water became more and more
self- absorptive, he perceived that the lines progressively
darkened descended the scale of refrangibility with approxi-
mate steadiness. That is to say, the rays most persistently
bright were those of greatest wave-lengths. Here, undoubtedly,
we hold a clue to the physical state of emissive stars, but
one, unfortunately, by no means easy to follow up.
The first specimen of a gaseous star was made known by
Father Secchi's discovery, August 19, 1866, of the green line
(F) of hydrogen conspicuously bright in 7 Caasiopeias," the
middle star of five of the second and third magnitudes
grouped into the shape of a W 011 the opposite aide of the
pole from the Great Bear. Soon afterwards the same peculi-
arity revealed it&elf in ff Lyrae, the emission being discerned
in it as well as in 7 Cassiopeiae of three rays of hydrogen
and one of helium. But these do not always present the
same appearance. As early aa 1872 Vogel was struck with
^ A*troph. Jowmalt toI. ii. p. ISl,
» Thid. vol rv. p. 527.
' Sugli Spettri I^ntmatici dclU UtetU Fisse^ H«m. i. p. ](], Mem. ii. p. 32.
60
THE SYSTEM OF THE STARS
tbeir apparently imaecouii table capricea of visibility ; ' and
M. von Gothttid watcheJ vainly during two years before he
caught sight iu 7 Cassiopeiie of the crimson twinkling of
C in paTdcnlariy unfuvonrabU weatkert August 13* 1883.*
His subsequent obaervatione, and those of M. von Konkoly*
fully established the occurrence, in both stars, of remarkable
spectral fluctuations, which have eince been studied, with
attentive curiosity, in widely separated parts of the world.
The result has been to establish their reality, but strongly
to disGriminate between the modes of their occurrence in the
two objects. They are periodi*ail in /3 Lyrse, and their
period is that of the star's light-changa The flickering of
bright lines in its spectrum, accordingly, depends in some way
upon the rise and decline of its visual luminosity.* But the
white radiance of y Cassiopeipe, although including variable
elements, is^ in its sum-total, perfectly steady. Since lh6
advent of spectrography, fluctuations in the hydrc^en-linea
have ceased to be apparent ; but then C, ivhich IJea below the
range of the sensitive plate, has scarcely of late been looked
for. And C was precisely the line most noted, in the days of
viaual observation, for capricious shining. This property is
unmistakable in the yellow helium-ray (B^); the sodium-
flbaoi-ption near it is ;ilso apt to become effaced ; and the
green and blue magnesium lines appear, with unaccountable
alternations, bright and obscure^ Kor is it at present known
whether these sundry changes proceed in concert, or each on
its own account.
The speetrum of fi Gentauri, which closely resembles that
of 7 CaaaiopeiBB, is represented, from a photop'aph taken at
Arequipa, February 8, 1897, in Plate III,, Fig. 3- The
brilliant line to the right is H)3 (¥) ; but the dusky edgeSj
faintly perceived to fringe it on the original negative, are
swallowed up, in the print, by the general gloom due to the
idiosyncraay of the plate. The luBtre of H7 is, however,
strongly relieved by corresponding absorption, and HS dis-
plays merely a thread of light dividing a profoundly dark
band. Two clean cut, black lines to the right of H7
' ^Qtfikamp Btobachiunoen, Heft iL p. 29. ^ Attr. Nach. Noa, 2&S1, 268fi.
' Obseroalor'^, vol, vi. p. S^2 ; O Gyalla Beobachfungtny toI, viii. p. &.
* See Chapter XXl. of FrobUma in Aflropkyria Ity the pJesBtit wTitflf.
GASKOUS STABS AND NEBULA
61
ta from helium ; and there is room for farther research
ui the ideutificiition of many additional rays, hotli bright
aad dark, in this beautiful apectrum.* ProfesBor Campbell,
in 1S94, observed in it the crlmaou shining of C. No
Bospicion of variability attaches to the star,
A etar-disc is rendered through distance immeasurably
Bmall. It has no longer diversified parta The light from
aU is blended indiscriminately into the radiance of a single
point. Hence, Dr. Scheiner argued, the mere increase of
atmospheric extent, apart from any increase of atmospheric
enuBsive intenaity, would give overweening effectiveness to the
bright-line ingredient/ an insignificant proportion of which
ifl present in the luminous aheaf sent out by ordinary stars.
Experience has, however, virtually negatived this view. The
phenomena of spectral variability are entirely irreconcilable
with it. And, in one form or another^ they prove to bo
widely diffused. But the absurdity is patent of invoking
fluctuations in atmospheric compass to account for them.
de gaaeous surroundings of stars may conceivably bo subject
to changes of luminosity ; but the hypothesis of their ex-
pansion and contraction with the rapidity, and to the vast
extent required, is plainly inadmissible. Moreover, the
diverdty of conditions under which bright Unea are perceived
to originate, their complex reversals, their peculiar individu-
alities, intimate the working of profound physical agencies,
and repudiate any single formula of explanation incapable of
t adaptation to the lavish variety of nature,
I Dr, Schuster proposed, in 1903, a theory in some respects
BPeferable to Scheiner's. Both speculators alike sought to
Irade the direct consequence of Kirchhoff' s Law, according to
which, " a layer of gas in front of a radiating surface can only
give bright lines if its temperature be higher than that of the
radiating surface " ; ^ a state of things not easily to be supposed
esdiBtent in stellar or solar atmospheres, A new expedient
was accordingly resorted to by Dr. Schuster. He showed
that bright lines might he produced by the dispersion of light
in layers of incandesoant vapours overlaying a hotter radi-
1 Cf. Loolcyar and Bkiendali, Month. Notices, April 1£K)&, App, No. 2.
^ Scbeiner, Di« Spiclralana-iyse d4r GtsHrnt, p. 270.
• OhterDtttery, vol. ixvL p. 379*
e2
THE SYSTEM OF THE STARS
ating surface, His roaBoniiig ia no doubt correct, aod we
have here a " true cause," although scarcely one that is
sufficient for the part aasigued to it. Its inadequacy becomes
patent when we consider that ita action ia at a minimum
just where the eflects attributed to it are most conspicuoas.
The scattering power of pure gaaea must be very small
compared with that of the vapours, say* of carbon, ailicon, or
titaniuoL Yet the bright lines in stellar spectra are chiefly
those of the tenuous and transtueent gases, hydro^u and
helium. The rationale is thus unconvincing.
Another, designed expreasly to meet the case of temporary
stars, has been advanced l^ M, Ebert.' It is based upon the
principle of "anomalous refraction," by which light subtracted,
through a special action of the refracting medium, from one
narrow section of the spectrum, goes to reinforce the adjacent
Strip, a show of paired bright and dark lines appearing as the
reetilt. But here, again, the actual phenomena seem recalci-
trant. Hydrogen and helium are among the least refractive of
substaQces. They are eminently unlikely to act on transmitted
radiance in the forcible manner demanded by M. Ebert's theory.
The stellar cLlss, of which 7 Caaaiopeiae is typical, haa
now upwards of fifty known representatives, most of them
having been detected by Mrs. Fleming on the Harvard
epeotiographic plates. Among them are the noted ex-
v&riahles, at present shining with an uniform, unpretentious
lustre^ 'rj Garinaa and P Cygni. The spectrum of the former
object was found by Sir David Gill to bear a strong re-
semblance to that of Nova Aurigoe ; ' and P Cygni is
similarly characterised. The pemmnence in both of spectral
relations transient in new stars has an import which can
hardly be over-emphasised.
The so-called Wolf-Rayet species of gaseous stars, although
cognate with the helium variety, stands well apart from
them. Hydrogen and helium rays are» in their spectra, of
Bubardiuate importance. They are mainly distinguished by
certain vivid bands in the yellow and blue, some of them
due to cosmic hydrogen, others of untraced origin.
> Aar. Jfach. No. 3917.
^ Monthly I^otw$, vol. Ixi. p. AL6.
Atmali, vol, xxviii. part ii. pv llb^
See alfto A. J> CumoD, Harvard
GASEOUS STAICS AND NEBUL.E
63
The finest epecunea of the class is invisible in them
Utitxbdea. Jirat detected by Kespigbi at Madras^ December
24, 1871/ the pecaliarities in the light of y VelonuD were
studied with fiome caxe and much delight at the " extmordiuary
beauty " of the spectacle they present, by Dr. Copeland at
Puno in the Andes, April 24, 1883.' "An intensely bright
line in the blue" he remarked, " and the gorgeous group of
tbT«« bright lines in the yellow and orange, render the apec-
tram " of this star " incomparably the most brilliant and
Btiiking in the whole heayens." There ia no eign that it is
in any degree variable. Its appearance to the present writer,
at the Cape, in October 18S8, tallied precisely with Dr.
CopeUnd'e description, only that the additional feature of a
deep band of absorption below the cobalt line seemed unmis-
takftble.' A vivid continuous spectrum extends into the
violet as far aa the eye has power to follow it, and accounts
for the brilliant whiteness of the star. The diffiiseneae of
radiation in this splendid object is an obstacle to its effective
spectrographic treatment. A fair idea of its character can,
however^be gathered from Plate II L, Fig. 4j which reproduces,
by the courtesy of Professor Pickering, a photograph taken
at Ajrequipa with 99 minutes' exposure, April 28, 1897.
It does not extend to the lower tract illuminated by the
golden and citron rajs. The spectrum begins on the right
with the double or triple a2ure bands distinctive of this
Bfcellar type. The less refrangible (X 4688) occupies a
remarkable position. It is that theoretically assigned by
Bydberg in 1897 to the one member accessible to view of the
" principal aeries " of hydrogen. By analogy it should 'be
there, and it ia This azure band seems to be an unfailing
adjimct to the Pickering series, which it imitates aa well by
refusing to be evoked in the laboratory. Professor Campbell
was surprised, in 1893, to find C briUiant in the spectrum
of 7 Velorum, the other hydrogen lines being dark.* They
are nevertheless perceived photographically as projected on
bright bands, an arrangement the inverse of that prevalent in
' Oe-mpbit RmdvSf t Ixxiv, p. 610.
* Vopemitnu^ vol, iii. p, 206.
' Obtervatory^ vol. n, p, 430,
' Pablieatiena Jstr. Fete. Soddy, rol. v. p. 106.
THE SYSTEM OF THE STABS
gaseouB stars of the helium kind^ Abeorptiott by o;
WBA detected by Mr. McCleau amid the emissive spleudoius
the southern luminary; metallic action is probibly a1
throughout the class which it exemplifies.
ItB original members, three small stars in Oygiius, havi
in the course of thirty-eight years, obtained about one hundiw
aaaociate-s, lurgi^ly through the extensive photographic researchfl
of Mrs. Fleming. All theee are situated in the thivii
of the Milky "Way, or of the Magellanie Clouda ; and ol
except 7 Velorum, are insignificant when casually regarda
None are known to varj' iu light; in none» so far, has any epectn
clmnge be-en recorded. Indi^'idual diversities, however, abouitf
Lines dark in one specimen may be bright in another ; band
are mote or less hary ; the blue effluences differ from atar U
stftT in relative strength ; hydrogen and helium lines are nO'
piximinent, then again of quite subordinate importance. O;
8uch star was discovered by Campbell to possess a
hydrogen-envelope, indicated as existent only by the eenaibh
length of the green ray originating from its glow. Perhapi
some of its fellows have similar, if lesa conspicuous appurten-
ancea ; though none of them are, in the proper sense, nebuloufl^
aiuue they give sharp images, teleacopically and photo
graphically.
Yet^ in the Wolf-Rayet stars, we have imdoubtedly reacheJ
the borderland between the two great sidereal kingdonug
where definitions cease to be valid, distinctions become inJ
secure, and nondescript characters perplex classificationJ
Between gaseous stars and stellar nebnlre there is but m
narrow gap. Individuals of both species present the teleacopia
Appearance of small star? ; and they discloBe, when a prisnt
is applied, analogous peculiarities — analogous, not identicaL
The light of a gaseous star so examined is ordinarily concen*
trated in two points, or where a cylindrical lens is employed
in two short lines, yellow and blue respectively; that of il
ftteUar nebula gathers into one green knot. Its rays are, in a
MOUse, incapable of analysis; they are so nearly monochromatio
Ihul tliey can be refracted without being dispersed. Objects
^'1' this nature can be picked out at a glance from ordinary
*l'iil"n by Professor Pickering's method of "sweeping" with 4
k^ A. J. C&Dnoit, Harvard Annait, voL xxviiL p. 247.
^ i
GASEOUS STARS AND NEBULA
65
tall direct-vision spectroecope used as an eje-piece.^ AI>ove
flcote of them were in this m&nner found previously bo
t90. and many more anbeeqnently by photDgraphic means;
d it is remarkable that the exclusive prel'erence for the
ilky Way of gaseous stars is shared by stellar nebulae.
The green ray of the latter is the characteristic token
gaseous nebulae. From the great Orion *' portent '* to the
inteet "planetary," all without exception ahow it; and in
any it appears at first sight ao pretlominant as virtually to
and alone. But its origin remains an enigma. In position
is almost coincident with an important line of nitrogen. A
ifling divergence, however, shows them to be certainly dia-
neL Nor can it be identideil, as Sir Iforman Lockyer
loaght it might, with the sharp edge of a fluting emitted by
agneslnm burning at about the temperature of the Bunseu
ime.* The supposed agreement was made the corner-stone
the meteoritic hypothesis of nebular constitution;* but it
iled to obtain ratiticatlon by precise inquiry.
Careful measurements by Sir William and Lady Huggins,*
d by the late Professor Keeler, showed the fundamental
steoric and nebular lines to stand very slightly apart in the
Bctrum. But epectioecopic agreements must be absolute if
ey are to be reckoned aignificanL Moreover, the nebular
le is sharp ; and even the thinnest remnant of a luting
ould have an attachment of unilateral haze.
KebuJar radiance cannot then, it seems, he imitated in the
jQiatory. PoBsibly it signalises a modification of matter
sing only under extra-terrestrial tjonditions, " Nebulium/"
the hypothetical element is called, has been vainly sought
tongst the mixed leavings infioitesimally separated from
Damon air by intense refrigeration, under favour of their
equal boiling'pointa ; no mineral, however scarce, has Iwen
eovered to occlude it ; no volcanic vent exhales it. Yet it
is whole tracts of galactic space. Must we then admit,
ier all, that there is a chemistry transcending text-booka ?
jjgmy be so ; but to abandon the grand ideal of an universal
*PioJcerifig, Obsermtoryj toIs. ir, p. 81 i t, p. 294 ; Axtr. JVacA. No. 2517 ;
pelmnd, Mort-tkly NoIums, toL xlv. p. 91.
■ Prot. R. Haciely, toI. xltU. pp. 124, 327.
* Xkid. mL xliv. p. 2. * Ibid. toL ilri, p. 18.
ee
THE SYSTEM OF THE STARS
physical acieuce because of a few outetanding incongruitiee
would be to listen balf-heartedly to counsels of impatience.
Stellar nebula, so far aa can be judged^ are exceasivelj remote,
Toluminoua, faintly glowing bodies. The condensed or nuclear
portions probably included in them give but slight eigns
of incandesceuee ; spectroscopically (whatever they may be
physically) they are mere spheres of glimmering gas. Now
planetary nebuhe (so called by Sir Wjlliam Herschel becanse
they exhibit a planet-like (Hsc) scarcely differ intrinedoally
&om the stellar sort, but they either aFSk or owing to their
greater vicluity, appear larger and brighter, and hence offer
better facilities for the aualyaiB of their light
It is found to consist mainly of three rays composing the
fundamental spectrum of all gaseous nebulEe. Of these, the
lowest, of wave-length 500 7> is invariably the strongeist* and
accordingly survives alone in such a dearth of light as that
created by the combined distance and faintness of the moncn
chromatic discs or points detected by Professor Pickertng'e
method.
The nebular trio of lines, since they lie adjacent to each
other in the middle or green part of the spectrum, inevitably
give a resultant green or bluish colour to the objects they
characterise. The intermediate ray at X 4959, as well aa
the chief ray, is plauBlbly conueeted with uebulium since it
preserves in each individuiU nebula the same relative intensity.
The third or moat refrangible line, on the contrnry, is inde-
pendently faint or bright. It is no other than the familiar
F (K0); and the undoubted and unfailing presence of
hydrogen betokened by ifc in theae fomiationa constitutes one
of the very few links as yet recognised between nebular and
terrestrial chemistry. From the former metallic elements are
excluded ; they are, in uebulic, either non-existent or non-
apparent. And we recall that stars supposed on other groimda
to be in a primitive condition are just those in which metal-
loids tend spectroscopically to suppress metals-
Modcrn appliances, spectroscopic and spectrographic* have
enriched the nebular spectrum with some three dozen extra
lines, mostly in the ultra-violet. Some of those derived from
plttnotary nebulffi agree with lines bright in Wolf-Eayet stars,
nfitably with the fundamental member of the Pidtaring series,
GASEOUS STABS AND NEBULA
67
utd with the Bjdberg blue baod^ Occasionally, a glint of
red hjdrogen is seen ; eight of its more refrangible com-
panions have been measured ; and helium is represented b^
ft domewhat axbitraiy selection irom its various seriea.
The spectrum of the great Fiah-inouth nebula in Orion
was first adequately studied by Sir William and Lady Hugging
from 1832 ouwarda. Ita hydrogen -ingredient is in the peculiar
condition denoted by itB emission of the higher members of
the Huggins series, C being imperceptible. The yellow ray
of hftliiirn was detected by Dr. Copeland, December 28, 1836 ;*
and he remaxked " some iudicatioiis of resolvability into lines
or bands " in the dim prismatic backgroiuid upon which the
central group of rays in this spectrum are relieved The
Q^iiion further expreaeetl by Sir William and Lady Huggina
that the faint continuoi^ spectrum visible in most gaseous
B6bula^ might, were more light available, " be found to consist,
in great part at least, of closely adjacent bright lines'*^ hag
been strongly confirmed by recent Lick spectrograms taken
with the Crossley reflector, exhibiting tell-tale breaks and
g^nnptoms of overlap in the hazy radiance previously assumed
to be of '■ white " or unbroken quality.* On a plate exposed
at Tulse Hill in 1882, an intense ultra-viotet ray of wave-
length 3727 waa recorded,* and it has proved to be almost as
marked a feature of the nebular spectrum as the "chief" line
itself ; QOr can it be an emission of nebulium^ since its
intensity varies disparately from that of the green lines.* It
is fiingttlariy prominent in the Ring nebula in Lynu
A gaseous nature was suggested for the four bright stars
grouped into a " traiiezium " at the core of tlie Orion nebula
by an abnormal photograph taken by Sir William and Lady
Huggins, February 5, 1888J Several years later,® they per-
ceived the hydrogen-lines to be not only arranged in bright and
* Oopel&iid, Copemicttt, vdI. i. p. 2. The original "four-liue" pl&netariea
AH Dnmbered in Dreyer'a JStw General CatAlogae, 7S^2, 7024, aod 7027. The
two ]vt b*loag to a smgnlar group of allied ijuoous objetta in Cygno*.
* Monthly N^otices, voL x^riii. p. 360.
* Fnc -B. Hoeittif, vol. ilvi» p. 60.
* Lick Sulictin, Sq. US.
* JttpvH BrU. ABSoeialum, 1S62.
* Attroph. Jaumat, vol. xxi. p, SflS (Hnftiuaiin).
' Proc. Soy. Soeifty, toI. xlri. p, 4Q,
* AHroph. Jottmat, vol. vi, p. 322.
eS THE SYSTEM OF THE STARS
dzLrk pairs, but to undergo shiftinga defined hy Frofuaflors
Frost and Adams* as periodic in the chief member of the
group, and dependent upon rapid orbital circulation. Theae
etars are of the early helium variety ; they show absorption by
oxygen * and cosmic hydrogen ; and it is an open question
whether the bright lines crossing their spectra may not be
deriveil from the folds of nebulous matter enwrapping them.
Local variations in the spectrum of the Orion nebula are
most likely to subsist. It can hardly be supposed that so vast
and 80 agitated a formation can be throughout of uniform
composition, Profeasor Campbell, accordingly, found in 1893
that the relative intensities of the three lines, " which con-
stitute nearly the whole of the viaible spectnmi, vary within
wide limits as the slit of the spectroscope L^ moved over the
different parta of the nebula." * That is to say, the two first
lines, while preserving to each other a constant ratio, fluctuate
largely by comparison with the third or hydrogen-line. In
some sections of the nebulous Btructure, in fact, the hydrogen
appears at least five times stronger than the nebulium-ray,
although near the trapezium it lb four times fainter.
Hydrogen- light, in conjunction with the unidentified ultra-
violet emanatioUj, thus tends to become predominant with the
decUne of illuminative power, whence the conclusion may
reasonably be di-awu that the nebula verges more and more,
with the increase of tenuity upward and outward, towards an
almost purely hydrogenous composition.
And this serves to remind us that the spectra of the great
nebulaj, like those of " zoned '* stars, must be considered 08
integrating the results of emissions taking their rise under
notably diverse circumatances. Inniunerable strata of nebu-
lous matter are piled one upon the other in the same line of
sight. The eye is impotent to discriminate between them ;
even the spectroscope can do so only indirectly. For, at the
centre of the nebula, the lines coming from all its depths are
seen or photographed together ; their different places of origin
* Aatroph. Journal^ voL zix^ p. 15'3<
a McCiean, Phif. Trans, vol. Cici. p. 128.
"^ PuhL Attr. Pae. Sode(^, toL t. p. 300 ; Asir. Nack. No, 3471 ; tf.
RuDgfl on the phyaiologioal variatJons of brightn«a3 dne to differeace of colour,
J$traph. Jount. vol. viii. p. 33.
GASEOUS STAKS AXD NEBULiE
69
^.
are fuinoticed. Light, on the other haDd» t&ken from near
the edges of the same object, emanates eicluaively from ita
higher regions, and its characteristic peeuliariti&a may safely
be localised. The possibiiily then seems at band of dtnding
in this way the Orion nebula and others of tbo some claiia
ioto various spectroscopic levels, distinguished by minor
radiative differences. The helium- lines, for example, may
prove separable from the hydrogen- lines ; and it would be
eqtecially interesting to ascertain -ffhetber the three hydrogen
fleriee change their relative intensities with remoteness from
trapezium. The differing conditions along the same line
sight must also hampt^r attempts to determine the internal
mavemente of the nebula by the displacements or distortions
of its spectral rays. For there must be a wide disc<»rdance in
these effects at the heights and hollows projected together by
perspective. Opposite motions might be progi*eaging in the
lundry regions conjointly inspected • and the upshot would
be an ambiguous blurring of lines. Such a possibility
most be taken into account in estimating the value of some
proiaifling experiments of this nature made by Dra. Vogel and
Sberhaid at Potsdam in 1902.^ They hinted at tumultuous
flows, or eddies, more probably than at a general potation.
But until they have been repeated and confirmed, it would
be vain to speculate upon what they seem to communicate.
Only the species designated as stellar, planetary, annular,
and irregular nebula give unmistakable signs of gaseity.
Some five or six score have^ up to the present, been recorded
to do so ; while several hundreds, and presumably the majority
of thoee unobserved, shine with continuous light. Yet the
disttuctiou is perhaps less profound than it seems. The gap
is at any rate partially bridged. One connecting link
Beeias to be supplied by the great " looped nebula ** in the
southern constellation of Dorado, observed by Mr. C, E.
Burton^ in 1874 to yield a strongly continuous spectrum
croesed by the unfailing green nebular ray at 5007. Ita
gaseous nature is thus shown to be modified by the presence
of an unusually large proportion of dense material, and wliere
this predominates, as in the Andromeda nebula, the spectrum,
1 SiizuiufshtrriehU, B«TUa, Unralt 13, 1902.
> Monihly Kotiees, vol. xxitI. p. 3S. See (7th Harvard JUporC, p. 7, 1392.
70
THE STSTKM OF THE STAES
tboBgh nanhmOj ' ttntiamfrnt" is still nx&rkedLy dUferent
from the coadnnooB wpettrrsm of a star.
The light at Uiis "queen of the ne&qle,** prismaticall^
diflpened for the fint tizBO bj Sir WiHuun Hoggins in 1364,
fltmcJE bim ae fu- &omiiufi»B; H aeemed wi^Ul^ thioughoat,
whether hj the effects of aheorptuxi or of imgnl&r emisdon,
it was impoesble to decide.^ Beee&t ofaaerratioDs at Tulse
Hill point to the exiatesioe in Uua i|iectniiii of Twrions bright
linee or wpatcea intennized with fcimilB of abeorptioiL- Dt.
ScheJner perfonned in 1899 the diffieolt feat of spectrograph-
iog the object, which he tolerred, &om the faint tndicalnons
on hia pl&te, to be a claster of solar stars.' The truth of
tile matter remaiD« still hidden ; but there are dg&s th&t it
can before long be dicited. In the iiiTestigatioa of the diis-
tinctive pecnljarities of continoous nebular light, a field
lies open which can hardlj &il to be worked with profit to
the rapidly advancing science of coemical phjsica
* i'iliL Trmu. toL dir. }>. 441.
* AUMtfSuUar Sf*eirt, p. 13S.
> AMr. Ifatk. No. 3549.
CHAPTER VI
THB TKMPKRATHREa OF THE STARS
T we mean by the temperature of a star is the degree 'of
heat corresponding, on admitted principles, to the radiations it
sends abroad into space. That ia to aay, the point at which
4ti ide^il thermometer would stand if placed within the
photoepibere, assumed for the purpose of simplification to be
«flecttvely a single emitting surface. Now, the temperature
of the sun, understood in this sense, has been fairly weU
aaoertained. It is held by the latest authoriticB not greatly
to exceed 6000* C» while that of the electric arc, determined
by similar metboda, comes up to 4000".^ Thug, the gap
dividing the heat of the solar furnace from the tu plus ultra
of the laboratory has been greatly narrowed. It no longer
seems hopeless to establish some degree of continnity between
the state of things on either side of it. Nevertheless, there
are qualifications to be taken into account. Conclusions
legarding the sun's temperature depend essentially upon two
conditions: first, that the photosphere is what is technically
known as a "black body"; next, that "Stefan's law" of
tadiation holds good over a range some thousands of degrees
beyond the limit of experimental verification. Now, a " black
body " is one that absorbs completely, and, through an inevit-
able correlation^ emits perfectly. It radiates in the strict and
due proportion of the heat communicated to it. But there is
no such substance in nature ; even lamp-black meets very
imperfectly the stipulated requirements. They have of late,
^however^ been imitated by an experimental artifice;^ and the
* D«7 ftttd OntrAnd, AatTOph, Jtmrnal, roL xix. p. 40.
* Wien and Lmumer, fFitdtmanti's Anruittn, Bd. Ivi. p. 453, 1895,
71
72
THE SYSTEM OF THE STAES
facilities for investigation thus acquired prove of high valnti
Yet the laws of radiation securely est&bliehed with their
are, in all probability, conformed to only approxiniately
the Bun. For the photosphere is certainly not, strictly
ing, a " black body."
Stefan's law defines the rate at which increase of radiative
intensity corresponds with growing temperature. It is as the
fovirth power ; a body rendered, for instance, twice as hot will j
radiate sixteen times more powerfully than before. Nor ia I
this a purely empirical rule. Boltzmann broitght thermo-
dynatnical considerations to its support in 1884, and Planck
deduced it in 1900 from the electro- magnetic theory of ligbt^
Stilli it luay break down before the soUr temperature is
r^suhed. Its validity, experimeuUlly ascertained up to near i
1200"» cannot be confidently relied upon at indefiniteljH
exalted tenn^rstures. Such laws of nature have usually a
limited fiold of iiction, and we do not know where to fix iu
boundarii^ This element of uncertainty affects many other-
wine well 'grounded conclualona. Nevertheless, high tempera-
tUTtf n^Mitoh has made substantial progress; and much has
en done in removing the difficulties which long stood in the
[way of establishing a trustworthy relation between the he
rStOilved from the aun and the sun^a proper heat.
But ft8 regards the stars the case is widely different
DirtOt mod« of procedure are here excluded. We cannot*
determine stellar heat-constants, and thence infer stellar
ttiwuMiriitures, This is rendered impossible by the funda-
mental ciruiuustanee that the heat reaching the earth from
the stars is all but insensible. The rays of the " wan. cold
moon" have a thermal power more than 150,000 times
t than that of the rays of Arcturus,* and Arcturus
■« judging by the crude standard of direct heating eOects, the
hottest star of onr acquaintance. No wonder, then, tba|^|
quantititis bo minute failed to be elicited with the thermopile.
Sir William Huggins made persiflteut experiments on the
subject nearly forty years ago,"* and Dr. Stone* a little later.
* Mandenhall uxd Saauden, Aalropk. Jounu toL xiii. p, 30.
* Hicboli, Jttr&ph. Jgufn. toI. liii, p. 103,
* JProc R(ryal Society, Toi. ivii. p. 309.
* Ibid. ToI. iTiii. p. 159.
I'ne
be«lM
THE TEMPEBATURES OF THE STARS
tried his tadimeter in 1873, Boys his radiometer in
888;^ both vainlj. At last, in 1896. Pi-ofea&or Miuchin
'ntooeeded in converting stellar energj^ into electromotiTe
Ukw ; ' jet his results, though genuine, were not wholly
legitimate, owijig to the strong Belective preferencea of the
onailive cells.* Thoee, on the other hand, ohtained by Pro-
GEOor Xichols :it the Yerkea obaervatory in 1900 were of
unequivocal signihcancd. The beams to be examined, after
being concentrated by a two-foot mirror, fell upon the vanes
of a radiometer eo delicately impressionable as to detect
tempera tore-di^erences not exceeding one ten-inillionth of a
JE^ree oetitigrade. Eesponsive detJections were, accordingly,
undoubtedly due to radiated stellar energy ; and
,ey varied from star to star, those caused by Artiturua being
than twice as large as those which the white rays of
A had power to produce.^
The outcome is in many ways hopeful. Not tliat the
prospect can he discerned of arriving, by this straight'
route, at the absolute temperatures of the Btfira ; but
that it opens a way by which, with much further care and
BOme knowledge of their relative temperatures may
led. And even in this direction progress is seriously
pered by diversities of absorption in stellar atmospheres.
'e know by eveiyday experience that a glowing object
fiwm red to white as it grows hotter. So likewise
with the stars. The larger the proportion of light to obscure
beat in their radiations, the higher their temperatures must
be; But we do not see the stars as tliey are in themselves.
Their faces are veiled by absorptive envelopes, and tar more
[j veiled in some cases than in others. Moreover, the
of absorption in the bodies strongly atfected by it is to
modify very materially tlie relation of luminosity to thermal
inleaaitj in the emissions they send out. The upper sections
of the sjjecbram are those chiefly encroached upon ; the stars
are rendered fulvous, and reduced to a lower grade of photu-
tnetric magnitude than should be assigned to them if their
* Pjroc, lioyal Societv, vol. ilvii, p. 480.
■ /bid, vol, iTiii, r- 1*2.
* HichoU, Astropk. Joum. vol. xiiL p. IfSi
• Ibid. p. 136.
n
THE SYSTEM OF THE STABS
inUiDSU^ biiUiAncj were fiillj displayed. Kov^ Arcturos is a
aoUr vbftT of a reddisb tii^ ; its blue rays paj heavy toll in
tnTEtstDg its pbotospbenc ^ivelope. Not m those of Vega,
which escape virtimllj scot-fi«e to the open. It follows that
companaoQB between them are made on unfair term& If they
were equalised, Arctums would seem much more brilliant than
it does now, and the proportion of its heat to ita light would
be redreesed. And it ia the proportion only, we repeat, which
is significant as regards temperature Professor Nichols's
resolt implies, on the taoe of it, that Arctums stands at a
tower heat-level than V^a, becanae^ althoi^h its radiationja
contain absolutely more heat, they correspond to a leas
intense degree of incandeacenceL Bat no such deduction is
admissible in view of the disparity of conditions. Nor is it
possible to define the extent of the correction required. So
far, theuj the relatire temperature of the two atars remains an
open question.
Professor Nichols himself i^e^rds his attack upon the
problem of stellar heat as httlc more th^i a reconnaissance
by which it has been learned that the position is not im-
pregnable. With more powerful means at command, he hopes
to achieve its capture. By pkcing his radiometer at the
focus of a five-foot mirror, he believes it should be possible to
arrange white stars to the second, and red stars to the third
magnitude, " in the order of the thermal intensity of their
radiations.'' That fainter red than white stars must, owing
to the quality of their self -absorption, be thus measurable has
been sufficiently illustrated by the case of Arctunia, Just for
this reason, however, no instructive comparisons can be insti-
tuted between stars with notably different atmospheric sur-
roundings. The use of an identical platform of investigation
for disparate objects can only lead to illusion. But by ranging
white and red stars in separate series, and bringing aolaa: stars
into relation with the sun, much may be accomplished. There
is no surer criterion of temperature than the distribution of
energy in the spectrmn. As it rises, the culminating point in
the representative curve shifts steadily upward to shorter
wave-lengths. Hence, by locating the maxima of emission
from glowing bodies, their temperatures can be ascertained;
and this Professor Nichols hopes to accomplish for the stars.
THE TEMPERATURES OF THE STARS
76
It will be a matter of excessive delicacy; but, apart fioni
instniinental difficxdties, the method seems promising. Not
.t the esseDtial incompatibilities of stat« between the
Brent spectral classes can be abolished by ita means; but
ties of white stars might be examined together, while
stars could advantageously be Bssimilated to the Bun.
xm, Capella gives a spectrum almost indlBtinguishable from
the Fraitnbofer spectrum eave through the slight discrepancies
occaaioned by the differing light-quality of its spectroscopic
companion. It is, however, an enormously larger and more
ImzuDous globe than om: sun ; and it would be of crucial import'
auoe to determine whether its vaster acale corresponds to a
higher degree of heat. Again, Sir Norman Lockyer finds the
oltra-violet spectrum of Kigel to be more extensive and intense
than that of Siriua, and to be in turn surpassed, allowance
being made for the lower magnitude of the atar, by that of x
Orionis.* If these diversities can be securely associated with
gradations of temperature, much would be made clear as
regards the course of stellar development. And Professor
Nichols's method of spectral energy-measurement pFomiBes,
if efifectively realised, to afiford just the needed verification.
Speculations concerning relative star-heat have heretofore
been based chiefly upon the study of specific linear absoiption.
But the observed indications refer immediately to the state of
things prevailing in the reversing layers of the stars, and only
indirectly to the condition of their photospheres. Moreover,
their iDterpretation is, unfortunately, still a subject of debate.
Indeed, it is more actively in debate than ever before ; for, ao
the importance of reading their meaning aright has come to
be more fully recogniyed, the pitfalls laid for their would-be
decipherers have also become mote evident and formidable.
^^ It has loug been known that the rays emitted by glowing
^^aseoufl substances alter with alterations in tlie mode of kind-
ling them to luminosity. Thus, metals rendered incandescent
in the electric arc give out conspicuously bright tines that
show quite dimly when the same metals are burned in a flame ;
and similarly, lines subordinate in the arc develop iuto pro-
minence through the excitement of the disruptive discharge
in the electric spark- These progressive changes were, until
» iV«. Boy*^ Soci«ij/t Feb. IS, 1904.
76
THE SYSTEM OF THE STAES
lately, ascribed by general, though not univeiBal consent, to
increasing temperature, the spark being, it "waa supposed,
hotter than the arc, and the arc hotter than the flame.
Adopting this view, Sir Norman Lockyer gave special
attention to " enhanced " lines, and pointed out the
remarkable ci^rcumstanoe of their selective display in th«
spectra of certain daseea of stars.' It ia undeniable that the
brightest Unea in the spark-apectra of the chemical elements
are also highly characteriatic of white, and more especially of
helium stars; that arc-lines to a certain extent supersede
them in solar stars ; while in red atars with banded spectra^
even fame-lines take a position of importance. And the
aaeumptioii that from these modifications trustworthy informa-
tion could be derived regarding the comparative temperatunw
of the stars in which they were observed, lay ready at hand,
yet proved misleading. So early as 1888, Professors Liveing
and Dewar were led by their experiments on the spectrum of
magnesium to throw doubt on the received opinion that the
electric spark ia, in the literal sense* hotter than the arc'
Sir William and Lady Huggins demonstrated in 1897' that
the colcimu-lines, H and K, owe their preponderance iu the
stin not to extreme heat, but mainly to the inconceivable
rarity of the emitting vapour, and they illustrated in 1903*
by photographs of the magnesium-spectrum, the sensitiveness
of radiation to changes in the mode of electrical excitation.
The spark-discharge is oscillatory ; the released energy rushee
with amazing velocity Lo and fro across the gap. But in the arc
it assumes the character of a continuous flow ; means of trans-
port are available ; it does not need to force a passage. That
the ultimate particles of matter acted upon must respond very
difiTerently in each case is then eaaily understood. A final
overthrow was given to the older opinion when MM. Eherhard
and Hartmann of Potsdam pronounced,* after laborious investi-
gations, the spark-spectrum to originate, not from thermal
radiation, but from ** electrical luminescence."
The word is of subversive import. Its introduction by
' Ptec Seyal Society^ toIs. Ixi. p. 441 ; Ixt. p. ii2.
^ Ibid. vol. iUt. p. 341.
■ Ibid. vol. Ixi. p. 433 ; Alias of JiUilar SpiCtra, p. 91.
• * Aatroph. Joum. ?ol. xtu. p. 14&.
= Sit^ngtbtriehtf, Berlin, Feb, 26, 190S.
THE TEMPERATURES OF THE STARS
77
Wiedamauu in 1894 ^ to signiiy light without heat, or light
in excess of bemper-atuie, liceaBed the adoption into orthodox
phjuical science of certain new ideas which had long been
gradually creeping to the front. They allow a wide latitude
m the explanation of radixitive and spectral phenomena.
Ltmiiaesoence may be evoked by chemical or electrical action ',
it may be superadded to ordinary light, or appear by itself;
either a continuoua or a discoutinuoua spectrum may be
derived from it ; nor is it necessarily correlated with absorp-
tion. Hence strict reasoning ia precluded where there is
maon to suspect its ]>resence ; for the laws of its production
w yet evade research. We find, accordingly, that the spectral
peculiarities detected in the various classes of atars^ and long
held to supply sure indlcationa of their thermal rank, fivow in the
laboratory highly complex relations with vapour-density, with
electrical '' damping," with chemical proceeaes, with luminescent
iction. We are then thrown back in our search for tests of
stellar heat-power upon the varied intensity of blue radiation
from stellar photospheres, allowing, as beat we can, for the
differences in absorption by which it is partiully masked.
One pair of stars — Capella and Vega^thns compared by Sir
William and Lady Huggina* yielded an mdooked-for result.
The solar orb seemed intrinsically the hluet\ and was inferred
-to he the hotter of the two.
■ The temperatures of the atare are intimately related to
their life-history. From the time when they first assume the
phdtospheric vesture until, through decrepitude, they cease to
ahine, a constant waste of energy must be going forward in
them pari passu with contraction. Yet, up to a certain
point, recuperation, ao far as eensible heat is concerned, takes
the lead of dissipation. Cooling bodies, by a seeming paradox,
rise in temperature until they cease to be wholly gasuous. The
kw of thermal ascent, enounced by Lane of Washington in 1870,
applies^ however, only to average temperature, while such indica-
tions as can be gathered by us refer to surface temperature. And
this depends not so much upon the amount of heat stored in
ch globe as upon the facility with which it can be conveyed
Kpward to the scene of action. Hence viscosity, gravity, chemical
* Annalen dtr P/'i/nk, Bd. liv. p. fl04,
■ Atlaa f)/ Stellar SjiesCrat p. 85.
78
THE SYSTEM OF THE STARS
oompositioai, enter into the account as items of uaknown value.
Nor is there any posibility of fixing & priori tho point ut
which the extenul beat-power of a atar begins to f&ll ofl
Too manj conditions are involved The main object of actual
iuquihea is to establish the thennal reUtious of the varieties
of stelUr spectra. Those of earlieet type are non-metallic ;
they are markied hy the absorption or emission of hydrogen,
heliom. 09^gen» and nitrogen. Sir Norman Lockyer alleges
abnormally high temperature as the cause of this unusual
chamcter. Metala, in his opinion, do not exi^t in 8uch stars
because intense heat keeps their primal elements aannder.
They are dissociated, or perhaps have not yet be^n to be
associated Nebuh^ are nevertheless equally uou-metallic with
incipient stars, and it is difficult, if not impossible, to ascribe
an enormou^y high temperature to volumes of matter in the
last degree of attenuation. However this may be, the fact
can scarcely be gainsaid that metals show more and more
distinctly in stars as they adranoe towards maturity, and that
the ^t signs of their presence are the lines ''enhanced"
in the laboratory when the spark -discharge replaces the electric
are. Bat, a^ time and condensation go on, the arc-lines gain
upon their nv'als, and in spectra of the solar type leave them
utterly in the lurch. Finally^ in banded spectra strong flame-
lines emerge ; while throughout the progression, as if to com-
pUcate matters still further, the great violet ray^ of calcium,
although eminently characteristic of the oscillatory spark,
reach their highest development in reddening stars. The
entire series of changes, nevertheless, is beyond question
orderly and consequential ; and the obscurity of their origin
will be in part cleared up should it be found possible to
connect them with an equally consequential series of tempera-
ture-changes. Yet it must be owned that the trend of pi-esent
inquiries is rather towards establishing for them relations
with varying modes of electrical illumination than directly
with gradations of thermal intensity in stellar photospheres or
their reversing envelopes.
The hope of estimating temperature by locating maxima
of intensity in discontinuous radiations is probably fallacious.
Sir George Stokes, already in 1876, held it possible that the
intenser blue radiation with increase of heat obvious in con-
d
THE TEMPERATUEES OF THE STAKS
79
tinuons spectra might extend to spectra composed of separate
lajB — that the intensest line might shorten in wave-length ae
Uiermal energy was gained by the emitting vapour,^ And
M. l-Angenbiich obtained, in 1903, some experimental indica-
taODft of the actual subsistence of some such relation.' He
eonsideTa, indeed, that Professor CampbeU'fl observation of
tbe greater strength in the Orion nebula than in vacuum-
tubes of the mot* refrangible hydrogen-linea affbrda proof of
ft difference of temperature which may eventually be measured
in thernaometric degrees. Professor Xeeler, too* had inferred
ixom the singular vividness of the green and blue hydrogen
emanations in all gaseous nebulae " eithex a high temperature
of the gasea emitting the light, or a state of strong electrical
excitement/' '
The conditions of electrical excitement in heavenly bodiea
caoiiot as yet be de&ned. That they are present in some casea
moie fully than in others is. however, virtually certain ; and
many anomaloufi appearances will doubtless ^nd an appropriate
explanation when they come to be interpreted as electncal mani-
feetations. Meantime, we can only reason about what cornea
more or lees within the range of tangible acquaintance ; and
experience is wholly contradictory of the notion that nebulffi are
flZoeBBively hot bodies. On the adopted principle they should
be at least 3000*^ C. hotter than the solar chromosphere,
in which red hydrogen-light ia predominant, while nebular
hydrogen shines exeluaivcly, it might he said, with green,
blue, and ultra-violet emissions. Further, in many variable
otans the leading bright hydrogen line is the dark blue
HS» C and F (Ha and Hy5) being equally invieible. This
relation, if interpreted on the basis of Wieu's law of spectral
energy, would lead to the inference of fabulous temperatures as
prevailing in such stars. It is, however, moat improbable that
Wien's law is really applicable to bright-line spectra. " The
radiation from gases," we are told on high authority, " is usually
wholly or partially luminescent." * This means that its calorific
ipendence is slight and secondary. Hence nothing can be
^ Proe, Boyal SccUtj/t toL xsiv. p. 353,
' Annalem der Fhyaik, No. 4, 1903.
* Puhl. Litk QbitTWiUoTy^ vol. iii. p. 226.
* Day and OrBCrand^ Attrvph, Joum, toI, lii. p. 31.
80
THE SYSTEM OF THE STABS
authentically learned from its quality regarding the temperatiue
of ita source.
The science of stellar thermotics is, in fact^ still in a
tentative stage. The most assured datum at ita command m
the temperature of the sun, which at least supplies a term of
comparison for the teraperaturee of the stare. It is fairly
certain that the efEective lieat of the solar photoephere, measured
on the thermometric scale, ia 6000" to 6500^ C. And there
ia some probability that the sun has never been, and will
never be, much hotter than it is now. But thia does not
imply that none of ita compeers exceed tt in thermal power.
Those of greater ma&s niuat develop proportionately more heat,
60 that it is quite likely that giant suns of the solar type,
aucb as Capella and Arcturus, radiate far more intensely per
unit of area than our sun, and have photoepberea hotter m
the due ratio of the " fourth power " increase^
Stars with banded spectra are generally admitted to have
made a further advance in cooling. Yet, despite the heavy
losses in total heat incident to protracted radiation^ their
superficial temperatures may have euffei-ed only a slight
decline. The development of flutinga in their q>ectra is not
decisive on this point. Beceut investigations tend to show
that it is an index^ not so much to the degree of excitement
produced by heat, as to the kind of agitation set up by
electricity in the originating vapour,* Nor have we any
abfw^Iute ssBurance that heat -expenditure proceeds uninter-
ruptedly. Current hypotheses on the subject possibly need
revision. Eegenerative agencies may. under given circum-
stances, be called into pltiy. The many suggestions of
" radiology " (as the new science of radio-activity might be
designated) cannot be inconsiderately set aside. They are^
however, too vaguely conveyed to be profitably discussed.
The cosmical effects of these novel phenomena elude just yet
our mental grasp. They may prove to be of stupendous
Importance; to the future is reserved the task of unfolding
their character and scope.
* Trowbridge, Awer. Jowrn. of ScituvXt Tol. UL p. 117, 1697 ; Hale, Snct/,
BriL Tfi). xxxii. p. 779, aiC. Spectroscopy ; Fringfthaim, Jiappi/rit dv Gon^f*
Inttmationat di FAytiqv^^ t, ii. p. 108*
CHAPTER VII
TEMPORARY STARS
Thk facta connected with the light-changes of stars arc in the
highest degree strange and flUTprising ; and wonder does not
lofBBn as faiailiaritj with them grows. They are of everyday
occurrence ; they can be predict&d beforehand, in many cases
with nearly as close accuracy as an eclipse of the 8un or
m(X)ni and they affect in manifold ways a great number of
objects. Stellar variability is of every kind and degi-ee.
With the regulai-ity of clockwork some stars lose and legnin
a fixed proportion of their light ; others show fitful aeeeB-
iiona of luminosity succeeded by equally fitful relapses into
obfloority; many waver, in appearance lawlessly, about a.
datuna-level of lustre itself perhaps slowly rising or sinking.
The rule of change of a great number is that of an evident,
though strongly disturbed periodicity ; a. few seem to
spend all their powei-a of shining in one amazing outburatt
after which they return to their pristine invisibility or
msignificancc.
The amount is aa much diversified as the manner of
fluctnation. Changes of brightness so minute as almost to
defy detection are linked on by a succession of graduated
examples to conflagrations in which emissive intensity ia
multiplied a thoueaud times or more in a few honra The
range of variation is in some stars sensibly uniform; they
subaide during each crisis of change to the same precise point
j.of dinmese, and recover without aubtraction or excess, just so
lucb light as they had before. In others it is widely
egular. The limits of fluctuation in one period furnish no
31 6
s:
THE SYSTEM OF THE STABS
precedent to be conformed to in the next Nothing is pre-
deteTmined ; the intensitj of each phase seems to depend
upon a complex set of conditions unlikely to recur twice in
the Bame precise combination.
The first effort to regularise the phenomena of variable
stars was made by Professor K C Pickering in 1880,' His
Bve clnsses, though often enough (as might be expected) con-
fused at the borders, are still sufficiently distinct to form a
useful framework for the facta. They are as follows : Class I.
includes temporary or "new" stars; Class II., stare like
" Ikfira " Ceti, strikingly variable in periods of several months;
Glass IIL, stars subject to irregular fluctuations ; Class IV.,
variables with periods of a few days exemplified by B Gephei
and /9 Lyrae ; Class V,, " Algol-variables," or stars like Algol
in Perseus imdergoing brief obscurations at fixed intervaLk
We will take each in turn, beginning with the first.
A temporary star may be defined as a variable attaining
one single, vivid maximum. A swift rise to such a height as
to constitute a virtually " new " object, followed by a slower
yet prompt decline, characterise these outbursts, close upon
thirty of which have been more or less credibly recorded
within historical times. The genuineness of those stated to
bavg occurred in the follo^ving years ^ is, in only a very few
cases, open to cavil.
134 EC. in Scorpio; the star of Hipparchus,
123 A.D. in Ophiuchua.
Dec. 10, 173, between a and ^ Centauri. Conspicuous;
scintillated strougly ; visible eight months.
386 (April to July) between X and <ft Sagittarii.
389, near a AquiUe, said by Cuspinianus to have eqmdled
Venus ; vanished after three weeks.
March 393, in the Tail of the Scorpion*
827 (?) in Scorpio. Observed during four months at
Babylon. There is some uncertainty about the date, none
about the fact.
May to August 1006, in Scorpio,^ Described by Epi-
damnus, th© monk of St GaU^ as " oculos verberans."
^ Proceedings Atasr. Acad. toL xvL p. 17.
* S** Humboldt's CoMmat. toI. iiL j». 20& (Ott^'e tranfllation).
' Sclibafeld, Astr. J^ttch. No. 30»4.
TEMPORAEY STAES
83
all photographic detections.
July 1203^ in the Tail of the Scorpion; said to have
T«aeixibled Saturn.
1230. Id OpMuchua
15 72, Tyeho's star in Caaaiopeia
1604^ Kepler*s star in Ophiuchus.
1670, in ViUpecuIa,
1848, in Ophiuchus.
I860* in Scorpia
1866, in Corona Borealis,
1876, in Cygnus.
1885, in Andromeda.
1887, in Perseus; discoTered by photography.
1891, in Auriga.
1893, in J^orma ;
1895, in Carina ;
1895, in Centaurus;
1898, in Sagittarius; I
1899, in Aquila; J
1901j in Perseus,
1903, in Gemini; found on the Oxford chart -plates.
Making a total of twenty-aeven^ besides four or five question-
able instances mentioned in Chinese anuala.
The moat noteworthy feature of thia liat ia the curiously
partial distribution of the objects enumerated in it, All but
one of them lie in the thoroughfare of the Milky Way, and
nisie are clustered together in the section of it marked by
the stars of the Scorpion and the Serpent-tamer. In time
also the grouping of the apparitions is strikingly unequal.
The oocurreoce of three within the seven yeaiB 386 to
393 A.D. was succeeded by a blank of four and a half
centuries. Kepler's came pretty dose upon Tycho's star ;
none were recorded between 1670 and 1848; then, within
little more than half a centviry, seven " Novae " attracted
visual attention, and six made their marks upon sensitive
plates.
The brightest sidereal object known to us by authentic
description was the " stranger-star " in Cassiopeia, observed
by Tycho Brabe.^ He first saw it November 11, 1572, but it
* Wolf, QiKhieMe der Aitrontymi*^ p. 414 j Kaisert De Sttrrenhemtl, Part L
. £fiS ; Lyun, &>te.rvat.urifj vol, xvi. p. 268 ; Drejer, ihid.^ voU ixiv. p. 106.
34
THE SYSTEM OF THE STAKS
bad ah-eiady been noticed by Wolfgang Schuler at Wittenbei^,
November 6, and by Lindauer at Wmterthiir, Kovember 7,
while Maurolycus entered upon its systematic study at Meaaina,
November 8. Observed by Tycho to be the rival of Venus, it
fihowed to keen eyee at midday, and at night through clouds
thick enough to obscure every other star. After about three
weeks, however, it began to fade, and in March 1574 die-
appeartsd linally. Ita colour was at first dazzlingly white^ then
for a while ruddy, and from May 1573 onward, pale with a
livid cast. Rapid aciutillatiou distinguished it throughoaL*
There is no reason to suppose the outburst other than solitary.
The sppearaneea in the years 945 and 1264 connected with
it by a Bohemian astrologer named Cyprian Leowitz * were
almost certainly apocryphah'
The " new " star (designated " B CassiopeiBB ") can atill be
perceived smouldering in the sjiot where it once blazed.
Tycho'a measurementa, reduced and discussed by Argelander.
located it within one minute of arc of a reddish^ eleventh
magnitude star, the character of which, as di8d.oa&d by the
observations of Hind tind Plummer in 1870-4, and of Sofarik,
188S-90,* fully warrants the inference of its identity with
the famous " temporary " Not only is it variable to the
extent of nearly a magnitude, but it frequently seems hazy
and ill-defined, as if through some abnormality in the quality
of its light.
The star of 1604 ran a parallel course to that of 1572.
Discovered by Maestlin, October 9, and observed by Galileo at
Padua, October 10, it quickly overtopped Jupiter, but by the
end of March 1605 had sunk to the third magnitude, and a
year later vanished. Kepler describes it as " sparkling like a
diamond with prismatic tints/' ^ but says nothing of progresBive
changes of colour, " Nova Serpentarii," has left behind no
clearly identifiable representative.
The next " new star " wag discovered near fi Gygni on June
^ Tjroho, De ifovd Stelld attT» 1672, p. 303.
5 Tyoho, Judieixim de Novd Stettd.
* Lynn, Observai&ri/, vol. vU pp, 126, l5l ; Sadierj BngiiBh Mechanic, toL
iim p. 402 ; Tycho Bruhe, Frogymnaimataf p, 331.
* Monthly Jfoticev^ voL xixiv. p. 168 ; i^n*& Caiatogug cf kncien VariabtM,
p. 164; A3tr. Nach. Ko. 2960.
* Kcplflri Opcfa^ t. U. p. 620.
TEMPORAEY STARS
d5
20, 1670, by Anthelmue, a Carthusian monk at Dijon. It
was then of the third magnitude, but its decline^ unlike that
oE oth^B of its class, was iuterrupfced by two reappearaaceB
Kparated by intervals of invisibility. Between March and
May 1671, it rose from the fourth to the third raiik^ then
died out, only ftickering up to the fliith magnitude in March
1672.^ Almost exactly in its assigned position, Mr. Hind
poked up, April 24. 1852, a star between the tenth and
eleventh magnitude, which, when reobeerved in 1861, had
loet more than half its lights and gave the bluiTed image
eharacteristic of many auperaiinnated Novsj^.'^ The triple
mft-rimnTTi of Anthelm's Btar assimilates it to Janaon'a
wiable P Cygni,^ which has itself often been classed as a
Nova,
An object unequivocally aueh was detected by Mr. Hind in
Ophiuchus^ April 28, 1848, when it was of 6'7 magnitude,
and intensely reddish yellow.* Four days later it had
mounted above the fifth magnitude, from which eminence it
filowly descended, making no lasting halt until, in 1874-5, it
bad got down to the thirteenth magnitude,*
With the spectroscopic study of temporary stare, a fresh
chapter in our knowledge of them opened. Through the
magic of the prism, more was ascertained as to their essential
nature in five minutes than could have been learned in as
many centiiriea with the telescope alone. On May 12, 1866j
Mr. John Birmingham, of Millbrook, near Tuam in Ireland,
was amazed to perceive an unfamiliar star of the second
magnitude shining in the constellation of the Northern Crown.
On May 16, the application of Sir William Huggina'a spectro-
gtiope showed the object to be wrapped in a mantle of blazing
bydrogeo. Five bright lines (three of them due to hydrogen)
stood out from a range of continuous light broken up into
jEones by flatings of strong absorption.^ The incandescence of
the star was hence largely atmospheric, and for the real, &om
the rapid rate at which it fell away, could have been only
^ J, Coaciiu^ £l4mmtMd'A9iTano7nUj p. &&,
* MiMiKiji Notii*tf toL txL p. 231 ; A'atittif yoL xxxii p. 555. The staf ia
Ko. 1814 in tb« Gri»«iwifib Cttologue for 1S72.
> See anU, ^ 82. * Aatn Nock. Noi. 636, d3S, 672.
» itmihiij Koti&a, toI. xii, p, 232.
' I^daecdmgw Royal Society, rol. xv, p. 140.
96
THE SYSTEM OF THE STAKS
" akin-deep." Although the light dwreased hj a. d&ily half
magnitude, and its colour changed from white to orange, no
alteration took place in the character of the spectrmu. Tha
bright rays, however, faded fiomewhat less quickly than their
continuous background.
The vieibiUty of the object to the naked eye lasted only
eight days, and al^eady^ in the beginning of June, it had sunk
to the ninth magnitude. Its alow subsequent decline waa
interrupted by fluctuations, thought by Schmidt to be
periodical in about ninety-fauT days.^ When observed by
Vogel, March 28, 1873, and again by Barnard in 1902, it
wa3 of about 9*5 magnitude^ and gave an ordinary stellar
spectrum.^ Virtually, it had resumed the conditions of ite
existence when Schoufeld entered it aa of 9"5 magnitude in
the Bonn Durchniuaterung. Ita leap upward to the aecond
magnitude, involving a th&ttsand -fold gain of light, waa
accomplished with extraordinary suddenness. Two hours
and a half previously to Birmingham's discovery, Schmidt
surveyed at Athena the constellation in which the blaze waa
about to occur, and noticed nothing unuBual- He was certain
that the star could not then have been aa bright as the fifth
magnitude.
Although its character aa a Nova seems undoubted, the
name of " T Coronae " waa bestowed upon it in conformity
with Argelander'a system of nomenclature, by which the
variables in each constellation are designated, in the order of
their discovery, by the Konoan capital letters from R onward.
Only stars otherwi&e anonymoua, however, are included in the
distijictive series thus created, so that many variables ure still
entitled in the ordinary way by Greek letters.
The stellar apparition that ensued after ten years was, in
Bome of its featurea, the most remarkable of all. Dr. Schmidt
noticed at Athens^ November 24, 13V6j a atar of the third
magnitude near p Cygni, in a spot till then untenanted by
any known stellar inmate. The weather having been cloudy
during the previous four days, there waa no possibility of
tracing the steps of its ascent, but it ran down very rapidly,
and ceased to be visible to the naked eye on December 15*
* MonaUUri^i, BerliD, ia73, p. 304 ; Monihly Ifaikes, vol. IxiL p. 41B.
J
TEMTORABY STARS
B*r
Its changes of colour pursued an inverse order to tfaoBe of
ita predecessor From golden yellow it turned white, and
eTeotually bluish.
The earliest spectroscopic examination of " Nova Cygai "
waa miide by M. Corau at Paris, December 2 and 4.^ Just
tha same range of bright linea waa measured by him which
would start into view in the solar spectrum upon a considerable
augmentation of incandescence in the sun's gaseoua sur-
roundings. Besides thiee, if not four, hydrogen lines, there
were the yellow helium ray (wave length 6875), with severul
of ite ffubsequently identified companions, the magnesium
^^^up &, and probably the sodium D. The star, at the height
^Bf ita outburst, scarcely seemed to diverge from the type of
^^3 LyRe and y Cassiopeije. The C of hydrogen was vivid ;
the continuous spectrum strong. But as the light diminished
penmrkable changes supervened.* Bed hydrogen insensibly
yielded its supremacy to greeu ; only a faded remnant of the
general prismatic radiance survived in the yellow and blue ;
helimn ceased to glow ; and the lazuHte band of y Velonim
(nitrogen ?), identified by Copeland, January 2,* gained
K expected prominence.
Meanwhile, the chief nebula-line, usurping the place, as it
Ip^ of an adjacent green line of helium, had been steadily
■|iing to the front; and when observations, suspended in
March owing to the encroachments of daylight, were resumed
by Dr. Copeland at Dnnecht, September 2, 1877, it stood
alone.* All the surviving liglit of tlie object — by that time
Bonk to 10*5 magnitude — was concentrated in that solitary
green ray, and a minute planetary nebula was^ in appearance,
substituted for a star. But this too proved to be a phase
scarcely less transient than the rest Three years later, when
the Nova hatl dropped a couple of magnitudes lower still,
^^indications were obtained at Harvard College of its affording
^hm ordinary stellar spectrum.^ They were fully confirmed
^^from the evidence of a spectrogram taken by Mr. Palmer,
with the Crossley reflector^ August 12, 1901, whit;h showed
^ Oomptit Rttvdus, t IxxxiiL p. 1172.
* Loekyer* Proc Rayal Society, vol. xUii. p. 13B,
■ Ct>p§Tr%icva, vol, ii. pp. X02, 112. * Ibid. p. 108.
» Annual lifpoTly ie79-B0, p. 7.
88
THE SYSTEM OF THE STABS
the faint rays of Kova Cygni to be uiimigtaka.bly contmuoi
Profeesor Barnard observed them ahortly afterwards with
Yerkes 40-iiich reftitctor to be vigually iU-defiued and bluisfai
the star being estimated at about 15 5 m^oitude.^ He could
detect no change in ita position rektive to the surrounding
stars mapped twenty -four years earlier by Copeland and
Lohse.
The Novfe of 1866 and 1876 appear to have been of
essentially the same character, notwithstanding some variety
in the phenomena attending their decay. But they were
not more closely assimilated by the analogous peculiaritiM
of their light than the pair we are now about to describe by
the singular circumstances of their situation. On May 18,
1860j a nebula in - Scorpio, numbered 80 on Mesaier's list
(6093 in Dreyer's New General Catalogue) was observed by
Dr. Auwers at Berlin.^ It pre^nted its usual appearance
of a somewhat hazy ball of light, brightening gradually inward,
and resolvable with difficulty into separate stellar poiute*
together constituting a closely -packed, and most likely ex-
oessively remote globular cluster. Three nights later he
looked again, and saw that these minnows had a triton in
their midst. A seventh magnitude star shone close to the
centre of the stellar group. The existence of the new-comer
lasted visibly just three weeks. Before May 25, a decline set
in ; it hiid made conaiderable progress when, on May 23, Mr,
Pogson (uninformed of Auwers's discovery) was startled by the
apparent substitution of a star for the nebula/ the dim
luminosity of which seemed actually obliterated by the keen
stellar radiance emanating from within it. It recovered, how-
ever, very speedily from this merely optical effacement. On
Jtme 10 its normal aspect was almost restored, and has never
since been disturbed.
After the lapse of a quarter of a century the significance
of the event was accentuated by its repetition. This time the
great nebula in the girdle of Andromeda was the scene of the
outbreak. The unlooked-for addition to it of a " star-like
^ Lick Svlletin^ No. 34 ; jrfatrepA, Jpum. vol. ndii. pp. 232, 233.
'J Monthly A'cNtic«j, vol. Ixu* p. 10£i ; cf. J. O. Lohse, ibid. vol. xlriL
p. 494,
* Jttr. JVfflcA. No. 3287. * Mmthltf Noticta, va\. ni, p. 32-
M
DQcleiis " was aonounced by Dt, Hartwig at Dorpat, August
31, 1885; bat it turned out that the change had already
\wen perceived by Mr. Isauc W. Ward of Belfast, August 19,
and two oights earlier at Eouen Uy M. Ludovic Gully, who
«et it down aa au effect of bad definition.^ Concordant
obeen'atioos by Tempel at Florence* Max Wolf at Heidelberg^
V)d Engelmaon at Leipzig showed decisively that the strange
object made no show down to 10 p.m. on August 16 ;"^ and a
photograph taken by the late Dr. Cotiinion in August 1884
gave positive assurance that a year earlier its place bad no
stellar occupant as bright aa the fifteenth magnitude.' What
were virtually the first taya of the Nova reached the earth
August IV, 1385.
Between that date and Auguat 31 it mounted from the
ninth to the seventh magnitude ; then without delay
' Bitered upon nearly a& swift a downward course, cheeked
ur only one decided pause. Even the largest telescopes
^^Ped to keep it in view after March 1886. The full yellow
oolour, by which the star at first contrasted effectively with
the silvery background it was projected upon, faded with its
light. No haze or glow blurred its image^ which remained
sharply stellar with a power of 1100 on the great Princeton
refractor, when the adjacent nucleus of the nebula melted
into a confused luminous blot.^ Attempts, incomplete from
the nature of the case, made by Dr. Franz at Konigsberg,
and by Professor Hall at Washington, to determine the parallax
of Nova AndromedjE, gave only negative results.^ So far as
they were significant at ail, they indicated its immeasurable
remoteness from the earth, nor should it be overlooked that
Sir Robert Ball's similar experiment upon Nova Cygni had
ifitimated a similar conclusion.^
The spectrum of Nova Andromeda was of a dubious
character. It bore witness to a completely different order of
incandescence from that of the " blaze-stars " in the Northern
Crown and the Swan. The bright rays which it perhaps
included were incouepicuoiis. None were definitely determined,
1 CUltt Titrtc. Oct 1, 1885. » AmIt, Nadt. Nas, 2682, 2fl83, 2691.
* Nature, vqI, xjntiL p. B22.
* VoojQg, SuUreai Mcutngw, vol. Iv, p. 282.
* AMr. Niiuk, 2816. • Dunsink 0&wn«W<rt«, Part V. p. 24.
THE SYSTEM OF THE STAItS
though the presence of several io the green and yellow ' -v
atroriglj suggested to Sir WilUam Huggins on September
and Dr. Copeland succeeded, on September 30, in getCis
rough measures of three vaguely disceraible accessiouB (
brightneBs.* The light, however, waa mainly continuous ;, aw
a general resemblance in quality of radiance was one o
many arguments proving a physical relationship between tht
atar and the nebula. This was, indeed, superHaously evident
That one stellar coufiagmtiou should by chance be projects
almost accurately upou the core of a nebula in reality difl
connected from it, is just conceivable ; that ttco aucb higbl;
improbable events should occur within twenty-five yeara c
each other distances possibility. A third was barely rescue
by photographic agency from irrevocable oblivion.* Diacoveie
by Mrs. Fleming when its course was already nearly ra
enough waa nevertheless learned about Nova Centauri to plai
beyond doubt its analogy with its two predecessore. Tl
nebula, in an outlying part of which it was lodged, ia catalogui
as N.G.C. 5253 ; the spectrum of the star, fortunately reeordi
by a casual exposure in July 1S95, showed the same irregular
continuous character with that of Nova Andromedae* "W
may then feel assured that the Kovse of I860 and 1885,
well as that of 1895, were situated within the substano^
the several nebnlre which they temporarily illuminated. ■
This collocation obviously falls into line with the galact
aflnnitiea of other temporary stars. The Milky Way is a plai
of condensation for all small stars, but more especially, and
a marked degree, for stars as well as nebuliE of a gaeeoi
nature; Temporary stars are closely cognate with these, n
merely through the brief gaseous incandescence bringing the
to our notice, but through the symptoms of nebuloaity whii
Burvive it. Opportunities for their study have lately bei
nnmetoua and varied. Dr« Anderson of Edinburgh la di
tiuguished as the visual discoverer of the two moat remarkat
Novie that have appeared for some centuries. He anjaotmci
the addition of a guest to the stellar family of the Chariots
February 1, 1892 ; but the Harvard photographs were fom
* SepijTi Brit. AtaacieUion, 1885, p. 93f>.
" AfotUhly Noticts, vol. xlvii. p. 64-
' F^ty^fiTBt ffarmrd Rtpart, p. 7.
TKMPORAEY STARS
91
have Biiently noted the event on Deceuibet 10, 1891, and
^ stars omximum brightness was fixed from their evidence at
ii magnitude on December 20. Speetrographic methods,
iy\iUed for the first time to anch an outburat. disclosed some
profoimdly significant peculiarities, since ascertained to be
^oeraUy characteristic of " temporary '* star-light. They con-
sist mainly in the great width of the spectral lines, in the
duplication of the bright by a corresponding dark series, and
k tbeir large relative displacements. A fine spectrogram of
yova Aurigffi, taken at Harvard College during au early stage
of its development, is reproduced in Plate VI. Three briUiant
hjdrogen-lines, beginniDg with F on the right, are visible in
it with their obscure, more refrangible companions; the H
and K of calcium are aimilarly conspicuoua to the left ; while
the hydrogen-aeries ia continued in a less pronounced manner
bejrond them in the ultra-violet. It is instructive to compuie
with it (oee Plate VII.) a map of the same spectrum, drawn by
Father Sidgreaves from two photographs taken at Stonyhurst,
February 3, 1892. It ib in two sections. The upper contains
Cthe lines apparently present, the lower those that were
ent and indubitable. The shorter wave-lengths, it will be
noticed are here on the right hand ; F is in the middle, and D,
undivided and distended, is placed near the extreme left. The
hypothesis of a double origin for this extraordinary spectruin
irresistibly suggested itself. Two stars, one shining with vivid
gaseous emissions, the other showing heavy absorptiou-Unes^
were supposed to be in the act of rushiug past each other
with enormous opposite velocities, a grazing collision, or tidal
influence being invoked to account for the conflagration by
which they were rendered suddenly conspicuous. Accumulated
incongruitiea, however^ have thrown discredit upon the " two-
Btar " theory, and it has now few adlierents. That an encounter
BO wonderfully circumatanced shoidd occur just once was con-
ceivable ; but the repetition of virtually identical occurrences
year after year transcended the powers of reasonable assent
Nova Aurigve followed the example of a nebular trans-
formation set by Nova Cygni, the change being in its
case accompanied by a very considerable recovery of lustre.
^he ator, then of sixteenth magnitude, was lost sight of in
ril 1892; in August, its light, multiplied some three
THE SYSTEM OF Tl
hnjidred times, waa mostly collected into tbe greeo ray of
nebulium (X 5007). Nor did it begin to ebb away again for
many months, aud thea only at the slow rate of about half a
magnitude yearly. Mr, C. I), Perrine observed it in August
1903 to be of the fourteenth magnitude ; and actually
succeeded in obtaining a legible epectrographic impreasioc of ^_
its faint rays. They proved to have nearly lost their gaseooa ^M
character ; the continuous streak yielded by them included
only bare traces of bright liuea.^ The rule, in fact, seems
general for temporary stars of reversion to a stellar type after
a more or less prolonged nebulous interlude.
Four new stars, discovered photographically by Mra
flemiiig,— Nova Normie in 1893, Nova Carina in 1895»Nova
Sagitt^rii in 1898.andNova Aquilseiu 1900,— followed closely
in the track of Nova Auriga^ They deviated very little from
the pattern of its spectrum* and they underwent similar
Tnetamoiphoses, only vanishing more quickly and more com-
pletely. They were then essentially phenomena of the same
order, though probably on a reduced scale^ since the duration
of a Nova's phases may serve as a rough measure of its real
mf^itude. Clearly outbursts of the kind ate incidents that
occur with method, and call for an explanation capable of
being uniformly applied.
The difficulty of finding one comprehenaive enough for
the purpose was not lessened by the strange disclosures con-
nected with the apparition of Nova Vex-sei. Early in the
morning of February 22, 1901, Dr. Anderson saw with
aatouishment that Algol had a twin-companion, which, thirty
hours later, was super-eminent in the northern sky. It was
not until Februaiy 24 that its light was distinctively that of a
Nova ; but the seeming delay may have been due to its
prompt discovery. None of its predecessors had been caught
on the rise and at once spectroscopically examined. If they
hiid, it would probably have been found that the gaseous
blaze invariably needs some time to develop. It took place
in Nova Persei precisely in the same way as in Nova Aurigse
^ Lick Bulletin, No. 48 ; at Palmv, ibid. Kow 3fi -, Buiurd, Mb^Uhty
IfoHces^ vol. liii. p. 418.
' That of Koira Sfligitt*rii sbowod no conspicuoua d»rk linos wlien photo-
graphed April 1&, 1893 ; but this was a comparatively late rscord ; it is funply
|NOsatble that the usual cbianKscuro effects liad been apparent a month previaudy.
TEMPORABY STABS
n
and its l^s noted imitators. That is to saj, the bright bands
weie shadowed on their blue sides by beavy bars of fibsorption ;
And these were shifted from their normal places by amouDta
oorrespoiidiag, oa Doppler's principle, to the well-uigh ld-
credible approaching velocity of one thousand miles a second 1
The decline of the gbar was interrupted and irresolute,
X)tiru)g March, indeed, the intemiptiona amounted to vivid
spasms of recovery periodical in three days. Yet the loss of
light progressed despite of them. By September 1-901 the
once brilliant Nova had ceased to be visible to the naked eye.*
The singular nature of the corresponding spectrum t^an be
gathered from an inspection of Plate VHI., Fig, 1, in which, by
the kind permission of Father Sidgreavea, two of the Stonyhuret
photographs are reproduced. The differences between them,
it shonld be noted, are mainly of instrumental origin ; so that
the sum of what each records gives a fair picture of the
emission^raya of Nova Persei after it had dropped below the
aith magnitude. It had descended to the tenth in October
1902; and its colour throughout that year was dull white
or bluish,' whereas it had at fiist been strongly red. A
Bptxitrogram taken by Mr. Perrine, July 30* 1903, when it
was of about the twelfth magnitude, indicated that the nebular
rays for some tiuae predominant had lost strength concomitantly
with the usual restoration of continuoua Hght;^ and we may
be sure that the equalisation will progress until every spectral
trace of the strange cataclysm of February 1901 has becomef
efifaced
One of its accompaniments or conaequeDces was absolutely
without precedent. A circumferential nebidit was partially
photographed by Dr, Max Wolf, August 23, 1901 ;* and it
came out fts & complete series of spires issuing, it might be
said, from the Nova as their origin, in a Yerkes photograph
of September 20. Later impressianSj secured at the two great
American obaervatorieB, supplied evidence, the startling purport
rf which was independently perceived by Mr. Perrine * and
> Jost, JUr, Nach, No. 3811,
■ Bftrsurd. Uor^tkl^ Noiisa, to]. IxiL p. 41S ; Rimbaut 1.1111 Williwna, ibidf
Jtuu 1902.
> LukButletin, No. 43.
* Aftr. ^afJi. Nob. a73fl. 3762, . . fi3.
' Lick Bulhliix, No. 30.
94
THE SYSTEM OF THE STABS
Mr. Bitchey, that the nebula was expanding at a portentous
rate, its awathed folds spreading outward, month by month,
like the ripploa on a water-aurfmie disturbed by the tall of a
Htone. Moreover, thia had been going on steadily from the
initial date of the star's visibility. A Croaaley -reflector plaie
was found to have been impressed in ten minutes, March 29,
1901, with narrow nebulous coils, the obvious progenitors of
thoBe fully disclosed six months later. For they were narrower
in the computed proportion of the time elapsed, and would, at
the Bame rate of e^cpanaioii, have started from their focuB in
the star a few days before it? observed outbreak. In Plate IX.
the Lick photographa of March and November are shown in
juxtaposition. The augmented spread of the nebulosity during
the interval can be gauged by using the small star to the
north-weat of the Nova as a point for comparison. In the
earlier picture it lies far out in the clear sky, like a rock near
high-water mark at low tide ; in the second, it is heavily
involved in folds of coamie cloud.
Theories of the expanding nebula round Nova Persei had
to meet arduous conditions The star has no appreciable
parallax ; aad the indefinite remotenesa thus implitd for it
gave almoet an assurance that the speed of the observed
movements iu its neighbourhood could not have been infeiior
to that of light transmission. Hence the idea occurred Bimul-
tftneously to Professors Kapteyn and Seeliger, and to Mr.
W. E. Wilson, that the motion concerned was ethereal, not
material^ Wliat we saw resulted, they thought, from the
progressive illxmiinatioa by the sudden stellar blaze of a pie-
existent dark formation. The rays photographed were those
of the Nova reflected from nebulous particles multitudinoualy
strewn round its place. The supposition^ indeed, of a dark
star lurking m the midst of a series of spherical shells of
obscure filmy material "^ ia not one that invites ready aaaent ;
nor did the observed movements within the nebula fit in quite
satisfactorily with the illumination-hypotlieais. It had to
encounter, besides, the difficulty that the light proceeding
' Jsir. Na^h, NoH. 3756, 37&9 ; Nature, vol Uv, pp. IflS* SOS.
^ The etf&ot, viewed ftom the earth, wculd bftre b«en that of a ji&rmholDidikl
surfftco projected on a piano. S«q the demonstration hy O. Lu^ftics, Atiropk.
Jowrn. vol. xix. p. 131.
J
TEMPOBAKY STAES
9G
firom the nebiUa was not polarised, aa it s)iould have been
reflected ; and Professor Newcomb considered that the
Lce of the nebulous spires from the Nova must have been
Bi> great as to precludo the po&eibiUty of their shining per-
eeptiblj by means of its enfeebled light.' Thus the weight
of opinion ultimately favoured Professor Very's hypothesis*
that the nebulous &tructm'e connected with Nova Peraei
resulted from its actual emission of minute particles under
the stress of electrical repulsion, or the subtle agency of light-
p rean mre.
Kova Gerainoruin was discovered by Professor Turner as
an intruded star of the seventh magnitude ou a plate taken
at Oxford, March 16, 1903. The Harvard College plioto-
graphic archives were then consulted, and a record of the
star's tna:cimum on March 6, at 5-0 magnitude, was extracted
from them; while a negative of March 1, showing stars down
nearly to the twelfth magnitude, preserved no trace of it.
Mr. Newall found its spectrum^ on March 26, to be ablaze
ftdth hydrogen and helium ; and a photograph of so much of it
as could be brought into focus at one exposure with the Yerkea
Bgfractor, obtained by Professor Frost, March 28, is repro-
duced in Plate VIIL, Fig. 2, Its predominant feature la the
strong effulgence of the Wolf-Rayet lazulite band ; the green
hydrogen ray to the right is of only half its width ; the faint-
nB9S of H7 (blue hydrogen) is partly due to its unfavourable
situation ; but Ho was perceived visually to be of great
intensity, and lent to the star its characteristic crimson tint.'
Colour and brightness faded together, and very rapidly, the
transience of the conflagration suggesting that it affected a
comparatively small mass. The decadent Nova was observed
by Professor Barnard, September 1, 1903, as a hazy star of
11 '5 magnitude,^ yielding, it had been ascertained at Lick,
August 17, a purely aebular Bpeetrum ;* and it will doubtless
sink ere long to virtual extinction.
The manifold experience of recent years has taught m
' Aitr. Journ. No, 5^0,
* A$tr. AS'ac/t. No. 3771 ; Amer. Journal qf Seifnct, vol. xri. p. 49.
' Ytrkt^ BaUetiii, No. 19; Astrx^k. Joum. vdL xvlL p^ 376i
• Turnerf Montfdy Nfflicet^ vol. IxiiL p. 5fi6.
" H. D. Curtis, Lick £%U€tin, No. 48 ; PublwUions Aatr, Faeific Societ^f
OCL 1903,
96 THK SYSTEM OF THE STARS
that a representative " temporary " specbrum passes through
five well-marked stages. To begin with, it seeme^thongh for
a very brief intervul — that of an ordinary helium-star. Next, ,
it displays a series of brilliant rays^ set off by dark eatellites,
always of shorter wave-lengths. Later, blue bands emerge,
and the light partakes markedly of the Wclf-Eayet peculiarities.
Fourthly, it becomes ooncentrated Into the green rays of
nebulium. Finally, it reverts to whiteness, and disperses into
a dim, featureless prismatic band. A strictly methodical
course of change is then traversed by tbe^ bodies. They
undergo transformations of a prescribed kind in a settled
order. Nor are any of thoir phaaea neceaaarily and essentially
unstable, since each is exhibited permanently by the members
of other sidereal families. The conditions to which Novee are
temporarily subjected cannot, then, be adequately explained
without reference to the fact that they are durable elsewhere.
They cannot depend for their production upon the fleeting
effects of catastrophes. This consideration seems to dispose of
collision and explosion theoriea of stellar outbursts. For the
displaced and coupled lines accompanying their vivid phases,
which such theories are specially designed to account for, do
not exclusively distinguish " new " stars. They occur as well in
the spectra of permanent though peculiar denizens of the sky.
The most familiar examples are P Cygni and rj Carina. Both
these stars now shine steadily, though both underwent striking
vicissitudes in. the pa^t ; and both show spectra perfectly similar
to those of Nov(e near their maxima. Their remarkable quality
of light accordingly corresponds to a state of things capable of
persisting year after year, decade after decade. The causes
which produce it must act uniformly and for an indefinite lengtli
of time. They are not brought into action casually through
some -momentary combination. Now thie inferenc-e obvioualy
applies likewise to Novee. The spectral phenomena shown by
them are, it is true, of a transient nature. Yet they are the
same observed to be constant in other stars. 'No rationale,
accordingly, which expounds them on the exclusive basis of a
passing catastrophe can be true.
The Nelmlnaity round Narii IVrw^i,
1. lu Mink '2. Ill NtvvL'Ujl.er, UHJI.
EEN two and three thousand stars are certainly or veiy
probably variable, and known objects of the kind multiply
with the more syBtematic use of photographic methods. In
Chandler's Third Catalogue (1896)/ 393 were enumerated;
aeven years later, 1309 figured in the Harvard Provisional
Catalogue^ with its Firat Supplement,^ . In 1904, no les&
than 407 new variables were brought to light by llifl»
vitt'a comparisoQB of Harvard plates taken at diGTerent
and detections go on apace^ both at Harvard * and
at Heidelberg.* So far, only a small proportion (417) of
the stars recognised as variable have had periods assigned
to them ; with most acquaintance has been made too re-
cently for the puipose ; yet a large residue seem entirely
Uwless in light change. Periodical stars are divided into
those with " long " and those with "short" periods. Nor is
the distinction an arbitrary one. The 6tars seem to separate of
themselves into two principal groups, undergoing fluctuationa
in cycles of respectively less than thirty, and of 120 to 460
days. The paucity of stars with periods of intermediate
leogtha is shown graphically in Fig. 2, where the height of the
curve represents the number of stars subject to changes pro-
portionate in duration to the horizontal distance from left to
right.
Variations requiring several months for their completion
» Aiir, Joumai, No. 378-
• Harvard A-miah, vol. xJviii. p. fll.
' Jfarvard Circuiar, No, 77.
' lind. No* 9S.
» M, Woir, Aftr, Jfach. No. 400C.
97 7
J
98
THE SYSTEM OF THE STABS
differ both in degree and kind from those run through in ft
few days. They are of much greater amplitude, ranging over
five to eight instead of, at the most, two magnitudes ; they
are accomplished with less punctuality; and they are fre-
quently attended by symptoms of gaseous ignition almort
wholly foreign to quicker vicissitudes. Most important of all,
they affect bodies of peculiar constitution. Nearly all long-
period variables are red stars with banded spectra ; those of
short period are white or yellowish in colour, and display
Sirian or solar spectra. Quality of light is thus the pro-
50
—
■~
—
-~
_—
~~
—
—
—
—
—
""■
ys_
-
-
^
n
^
1
^
4B
J
\
1*
r
/
\
f
L
40
j'
\
A
^.
/
^
>
^
|l
/
>
r
\
\
a*
/
C 331
i
t
t; ojd
f
\
—I
>
\
/
\
1 *"
-
„
-
-
-
.
'
/
\
= u
■
J
r
1
-
f
i
■
y
\
/
1
f
s
^
h
/
_
S
-^
^
\
/
^
s
_
^
f
s
-1
"
between
60
!6
a
5
1^
1,
fe
1*
to
2
Z
r
b
3
QO
30
3.
3
3D
>0
3i
3
10
4.
4
4
JO
id
4f
4
B3
to
LO
MO
540
Flu. 2.— Distribution of 8S4 Periodit of Variable Staw.
dominant factor in determining the law of stellar light-changes,
and is itself dependent, as we have seen, upon atmospheric
properties. The rule is, in fact, almost unfailing that short
periods are attended by slight, long periods by strong
absorption, and that the conditions producing redness in stars
not only favour variability in general, but almost absolutely
prescribe its type.
Periods of between one and two hundred days may be
called " long " ; but as Fig. 2 shows, they are not of plentiful
occurrence. Such fluctuations as now engage our attention
usually demand more than 200 days for their accomplish-
STAKS VARIABLE IN LOKG PEKIODS
99
It, and are seldom prolonged beyond 450. Dr. Chandler
riders 320 days as the average duration of change for long*
iod variables;^ the prevalencej however^ among them of
iod& of about one jeai is remarkable, and cannot be
ited for by mere accidents of observation. Tlie first
best known apeeimen of the olaaa. the members of which,
January 1. 1904, numbered 397,^ anticipates by about a
' aooth the rule of annual recurrence.
When Bayer, in 1603, affijted in his cbarta the Greek
letter o to a small star in the neck of the Whale, he had no
sospicion of its identity with a supposed " Nova " which had
di^ppeared seven years pre\'ioiiBly, after blazing up to the
second magnitude. Its diBCOverer, on August 13, 1596, was
David FabriciuB, of Osteel in East Friealand ; but though he
»w the object again, February 15, 1609, he left it to John
Phocylides Holwarda, pi-ofeasor of philoaopby at Franeker in
Holland, to ascertain its true character in 1639 ; aud the
repetition of the phasea in cycles of 333 dayjs was eBtablished
in 1667 by Boulliau.^ The name '* Mira," bestowed by
Hevelius upon the changing star in Cetus, commemorates the
iaiazemeut excited by the detection of stellar periodicity.
The phenomena it presents would 3eem incredible were
they less well established. Once in eleven months the star
mounts up in about 125 days from below the niuth to near
the third, or even to the second magnitude ; then after a pause
«f two or three weeks, drops again to it3 former low level in
once and a half times, on an average, the duration of its
rise. The brightest maximum on record was observed by
Sir "William Hersehel, November 6, 1779, when Mira waa
little inferior to Aldebaran ; * the faintest minimum, that of
1783, is said to have carried it below the tenth magnitude-
An eitent of eight magnitudes may then be aesigued to
the oBcillations of this strange object, which accordingly
emit&t at certain timeg, fully jif teen hundred times as much
light as at others. That each maximum is a genuine con-
flagration has been proved by Bpectroscopic ob&ervation ; the
conflagrations recur yearly, with approximate regularity, and
^ Aatr. Jcttm. Ko. Ifi3.
■ ffarvard CirmlaTj No. 7*. * Monilwa ad Attronomot, p. 7.
* Phil. Trant. t*]. In. p. 338.
5:]G0K^
100
THE SYSTEM OF THE STAES
after three centuries of notified activitj, give no signa of
exhaustion !
The height of the maxima, however, varies greatly. Th0
consecutive ones of 1887 and 1888 (represented £rom Colonel
Markwick's observations in Fig. 3) showed a nearly fourfold
difference of intensity ; but Heis's remark that high and low
maxima tend to alternate has not in the long run proved con-
sonant with facts. There is no rule by which the brilliancy
of impending phases can be predicted. That of November
1868, in which the star just failed to reach the fifth magnitude,
was, it is true, preceded by a high maximum, but several
average or low maxima followed it. All that can be said is
that exceptionally bright apparitions are isolated ; they do not
come in sets, but one by one, at considerable intervals, — at
Mae
35
4-0
4-B
S-0
flJ S 10 15
ias7
FiQ, 8.— Tvo consecutive Hudmft of Mlis Get!.
intervals, if M. Guthnick's conclusion proves correct, of 59^
years. The high maxima of 1779, 1839, and 1898 suggested
this period, prescribed — it is thought possible — by extra tidal
disturbances due to the periastron passages of a distant satellite
revolving in a very eccentric orbit.^ The next brilliant phase
need not be looked for, on this showing, until 1957.
At minimum, Mira rarely descends far below the ninth
magnitude. Fig. 4 portrays, from the observations of Mr.
Stebbins,^ the gradations by which it lost and regained light
in 1902-3. Although the star appears never to become
actually inert, its changes during six weeks amount to no
more than flutterings about the lowest level of brightness.
The progressive reddening of its rays as they grow dim is
held by M. Osthoff to be explicable as a physiological effect *
» Astr. Nach. No, 3746.
* Attroph. Joum, voL xviii. p. 346.
s Aatr. Nach. No. 3940.
n
— 1
^
^
/
'^
^
L>
■^
"■^
\
k
s
K
f
-
^^
<
■^
^
-.^
^
■
13S'
)^l
t 1
1
s ^
2
S 3
3
5 4
4
5 a
18
aa
> \
1
b 2
2
S 3
3
6 W 45 5tt
H STAilS VARIABLE IN LONG PERIODS 101 '^M
^Ipctf^ variatioQg are, nevertbekas, evident,^ and must cou- ^^M
tribute to the result. ^^M
The periodicity of Mira obeya a highly complex law. ^^B
Beviations to the extent of a fortnight &0La the '* mean period '* ^^M
of 331 days are commoD, and the maxiiaum of Septemher 29, ^^^
1840, wafi a full month late.^ Its perturbations may, indeed, ^^^
be themaelveB periodical, but if so, their law has not yet been ^^H
saccessfuUy formulated. Aj^lander detected the influence of ^^M
ft wave of disturbance with an amplitude of tweuty-five days, ^^M
and embrar,ing eighty-eight periods ; ' Schwab's obeervationa ^^M
indicated subordinate ripples of change In six and a half days ;* ^^H
and there are half-efifaced traces of several oscillationa besides.^ ^^H
Tet none are quite eecui^ly established Guthnick, howeverj ^^H
4-0
N
1
^
s
ho
•-0
\
r^
s
/
S
^^
/
'^
k
/
^
^
^_,
•^
'■^
"^
JijweSO JuLvaO AUCL29 &(i>r.2a Oct.2S 1Nov^7 De«.27 Jk>j^6 F(ft.S5 HalS'
Fio. 4.— Mlulmuai Of Xli* Oat), IWS4,
haa entire confidence in the reality of an inequality coverin
200 cycles (180 years), which is donbtleaa the equivalent t
one suspected by Argelnnder with a period of 160 years. Tli
tc»t pf verified prediction will eventually decide whether he i
right The shape of the light-curve, too, varies notably. It
peaks are aomelimeB much blunter than at others ; and th
Btar» which usually retains its full lustre during a fortnigh
has been known to remain twice that time stationary. Sti
more aingulaTly, the otherwise invariable rule of an increos
more rapid than the ensuing decrease waa reversed in 1841
Sixty-two days were occupied in aacending from the eixth t
^^fe 1 Astroph. Jourrt. toL xviiu p. 300.
^^^^^^^^K ^ ArgeUtider, Astr, Nadv. No. 419.
^^^^^^^^H ' BofVMr Bcohacht'angtn, Bd. vii. p. 332.
^^^^^^^ « Attr, NaeA. N<i. 27S1.
^^^^^V " Afgelancter ia Humboldt's Cosmot, vol. iii- p. 234.
102
THE SYSTEM OF THE STABS
the third magnitude, forty-mne only in smking back to
datum level The anomaly, due to what might he called
unprepared retardation of the maximmu^ recalls the ahn
course of the sunspot cycle which culminated at the
of 1883.
The spectrum of Mira is a splendid example of
third type. Eleven bauds of profound shadow, sharp to'
the violet, gently gradated towards the red, throw out ini
strong relief the iutervening brilliant zones ; while dark lia
of metallic abgorption, and vivid hydrogen -rays, vary the effei
and add to the intricacy of the characters to be deciphft
The more refrangible members of the hydrogen series are thoai
chiefly brightened in this star ; no trace of C betrays itself U
the moat attentive scrutiny ; F has never been seen, and i
only occnaioually photographed,^ Its violet aBsociate, He, il
also exceedingly dim, either intrineieally, or because of ttw
obacuring effect of a coincident cakium-band The brilliant'
phase of Miia in 1393 was attended by a curious triplicatioQ
of the blue hydrogen -lines,* as if through powerful magnetic
action. But the phenomenon has not recurred; hence the
polarising esperimente, by which its nature could be estab-
liahed, have yet to be tried. The dark lines in this 8i>ectrum
are affected by motion-shifts corresponding to a recession of
the star from the earth at the rate of 66 kilometres (40 miles)
a second ; ^ the bright lines are much leea displaced. Yet
there is no evidence that the absorption- and emission-raysj
although they act thus independently, belong to distinct bodies.
Mira is^ to all appearance, a slngly-coustituted star.
The same may be said of a variable in the neck of the
Swan^ which Bayer, ignorant of its changing character, set
down in his maps aa of the fifth magnitude. It still retaim
the name he gave it of " j^ Cygni" Missed by GJottfried
Kirch in July 1686/ it reappeared October 19, and sub'
aequently disclosed to his vigilant watch fluctuations even
wider than those of the " wonderful " star in Cetus. It deacendf
below the thirteenth and rises nearly to the fourth magnitude
> StebbioB, Aatroph. Joum. vol, xviii, p. 3Q4.
3 CunpbeU, ibid. tqL ix. p. S\.
* StebbiuBr ibid. rol. iviiL p. 352.
*■ Miaceltanta S*rolinensiA, U L p. 20S.
I STAHS VAKIABTK m LONG PERIODS
^kaetimea indeed stopping short when barelj visible
^bad eyft, bub more commoulv temainini? lucid fot a
103 ^^B
to the ^H
couplo ^1
^B liiontb& iN'or is its course much better regulated as regards ^H
^pna. "EzTor&" up to forty days often attach to its phaaes, ^H
Hbd the attempt to correct them by the introduction of cyclical ^H
Herms haa proved only partially Buc(^e3eflll.^ The period, ^H
Hitimated at 402 days by Kirch, now averages 406. Gibers ^H
1
r
V
^
\
f
\
\^
/^
X'
\
N
^
1
H B-2
\
/
/
\
■
/
\
J
\
/
\
f »«
1
\
J
\
/
\
/
^
L
^
108
f
1
I
/
Y
/
/
11-4
1
noti
and
cipa
aace
it, o
1
j
/
^-
r
J'' 3S M 79 uiO 12S tao rr& soo 225 350 ats uo 32s 390 376 400 435 450 479 soo
Fia. 5.— Llgbt-cniTS of R Normw.
sed that it had b^n ete-adily lengthening down to 1818
it 18 lengthenixig still. The compensatory process ant
ted by him has not set in. As usual in such casea, th
nt to maximum is much more rapid than the descent fror
Octtpyittg at present about 171 days.*
Tewwr B*6b, Bd. vii. p. 33{( ; Ma'n.^eiifut Jahreaberieht, Bd. xL {h ItO,
_ ' Sobnmacber'i Jmhrbwh, iSil, p. S3,
k * Chandler, Third Catalogue. 18&e.
^1
u ^^^1
THE SYSTEM OF THE STARS
The colonnaded spectrmn of x ^ff°' ^ appropriate to
•oarlet colour. Moreover, OQ May 19, 188 9» when tb© star
was near a maximtmi, Mr. EapiE perceived evidence in it of
diiect radiation by hydjwgen which seems to he quite similarly
conditioned to the blaie in Mira. The firet and fifth members
of the series (Ha and He) are missing ; the second (H)3) i»
perhaps leae evasively present. There is besides a discrepancy
in the positions of the bright and dark syatemB of linee
analogous to that perceived in the spectrum of Mira/ and
obviously connected with the peculiar processes of light-change
characteristic of such stars.
The light-curve of E Norma is depicted in Fig, 5 from
Mr. Lones's observations in 1898*99 at the Eoyal Obaerva-
tory, Cape of Good Hope.* It is of a very unusual character.
Fia- A,— Amu of ITtciiIe od tba Snn, 1B7S-[)f».
Each cycle includes a pronounced double maximum, resulting,
we can scarcely doubt, from the full and unrestricted develop-
ment of a tendency, half- suppressed in most variable stars,
to arrest the ebb of light at a certain interval after the
culminating crisis. The vicissitudes of solar agitation, too,
undergo a similar phase of hesitancy, as may be gathered from
Fig. 6, which portrays, from the Greenwich observations, the
virtually double facular maxima of 1882 and 1884, and of
1892 and 1S95. The variability of li Norm© was first
noted by Grould in 1871. An average period of 481 days
is conformed to ; hut ext^ifiive divagations from it are
patent.
They are, however, insignificant compared with those of
^ Ebnhvd, Atr, JVocA. Ko. 3766 ; Aatroph. Jtmm. ToL xriii. [h IftS.
Annalt ofiht Cape ObaervaUiry, voh Is. p. 107 B.
STAES VARIABLE IN LONG PERIODS
105
M«E
-
^
\
10-5
\
{\
\
/^
\
\
y
\
J
OJ bQ WO ■}bO ZOO 260
Fifl, 7.— Lfghl-curr* of U Lupl <IonM),
U Lapi. Indeed, thiB atar harely pretends to regularity.
Sometimes, it is true, the eoidden failures of light distinguish-
ing it succeed each other at intervaJa of about eighty-eeven
days ; but an interruption i& sure to supervene, baffliog all
attempts at anticipation, and the oBcUlatioas are then resumed
aa if by a freah impulse. In Fig. 7 two auoceaaive minima
are represented — one complete, the
other aeemingly abortive- Mr.
lo&ee diacovered this singular
object in 189 8>^ through its unex-
plained absence from the Cape
DurchmuBteriLng plates, and
vatched the capricea of its in-
stability durlDg three years.
By fer the longest period
attributed, on reasonably
good evidence, to a variable star was assigned to e Aurigee
bj Dr. Lttdendorff of Potsdam in 1903.* As a white star
with a spectrum resembling that of a Cygni, it should not be
predisposed to instability ; and the amplitude of its changes
is, in fact, of no more than aeven-tentha of a magnitude,
implying a reduction of brightness by one-half. Moreover,
they take place very gradually, and are rarely observed. For
the most part, the star shines with approximate constancy at
'i 3'3 magnitude. Its phases of dimness were believed to occur
quite irregularly, until Dr. Lndendorff showed, by an exhaustive
discussion, that they are subject to a periodicity of slightly
more than twenty-seven years. Decline and recovery occupy
thirteen or fourteen months ; an intervening stationary time
of least light lasta just ten; so that the entire oscillation
needs close upon two years for its accomplishment. Three
were recorded in the nineteenth century, a fourth in 1901-2.
^^b renmins to be seen whether futui*e minima will honour the
^Bl^^ifis of calculation as they fall due. Illusory effects of
^periodicity have often been perceived in stars fundamentally
irregular, and e Aurigte may still evade the law of order
which it has temporarily obeyed. Its character as a spectro-
scopic binary, established by Drs. Vogel and Eberhard in
^ Aslr. Journal, No. 143.
' ji9tr. Nach. Noa. 3918-20.
106
THE SYSTEM OF THE STARS
1902,^ cannot well be supposed extraneous to its luminoaa
T&riability ; but the mode of cotmection remains enigmatical,
atEice the oocurrence of edipBes ia preeludeil by the eonditionB
of tnovemeat that appear lo prevail in the system.^
We now come to that unique star, r^ Caiinse, Its actual
appearance is insigolficaDt. Invigible to the naked eye, it is
teldBoopically distinguished only by it« leddiab colour and
slightly superior brightness from the crowd of Bmall etats
embroidering one of the finest of the southerti nebulffi, named
the " Key-hole Nebula " from the aperture of that ah^pe with
which it is centrally perforated. Close to one edge of the
aperture, in the densest part of the nebula, tj Carin^e is placed
Nor can we suppose its poeitioa fortuitous. There is every
reaaon to believe the star to be really plunged in nebuloufl
substance ; and the peculiarity of its enviromuent combines,
we must suppose^ with peculiarities of constitution to produce
the exceptional character of its changes.
The first observation of 17 Carinae was made by Hatley at
St Helena in 1677. when it was of the fourth magnitude;
had it been as bright in the second century A<D., Ptolemy
would presumably have recorded it, since, as Mr. Innee points
out.* the chief stars in Crux and the Centaur, which culminate
about the same altitude, are included in the Almagest.
Soon after the youug English astronomer n^ade his
hurried survey of the southern sky, the variable had a notable
accession of lustre. Pfere Noel, a Jesuit missionary in China,
rated it as of the second stellar rank, 1685-89,* and so it
appeared to LaoaiUe in 1751; yet the discrepancy with
Halley's appraisement remained unnoticed. The higher
estimate was confirmed by those of Fallows, Brisbane, and
Johnson in 1822, 1826, and 1832 respectively, au intervening
decline having been noted only by the traveller Burchell, who,
familiar with the star as of the fourth magnitude in 1811-15,
was surprised one night in 1827, at San Paolo in Brazil, to
it temporarily raised to a level with the finest brilliants
' SitzungsbtrichU, Berlia, November 27, 1902.
- A. M. Gierke, Oiatrvaioryt toI. titu, p. 118.
' Annah Cape Obftrvatpry, Tol. ix. p. 75 B, Henderson lb referred ta ei :
auttaur af tbe remark.
* Wiimeeke, Attr. Nach. Ko. 1^4 ; Klein, SiHm, Bd. vi, p. 2&B.
STAKS VAEUBLE IN LONG PERIODS 107
of the aky. Another, and a atUl more vigorous outburst,
was witnessed by Sir John Herschel, December 16, 1837.
■Without previous note of warning, the star all at once
iieftrly tripled ite Ught, and before the end of the year fully
tu&tched a Centauri. Since then it has been kept under
strict Hurveillance as a notorious charaoter^ and not without
reason, After a partial decline and seveKil preliminary
•* Sutterings," it reached a final maximum m April IB-IS,
when Sirius alone among the fixed stars slightly outshone it.
This high position was moreover fairly wt:il maintained for
a^ or ten years, Gilliaa, at Santiago in 1850, found it very
'Httle inferior to Canopua in liglit, and in colour more deeply
tinged with red than Mars.^ Still of the fir&t magnitude in
1856.* it fell to the second in 1858, to the third in 1859,
and ceased to be visible to the nalied eye early in IS 68.*
For sixteen further years the slow ebb of Ught continued,
and the magnitude of the once e£^gent orb* carefully
determined by Mr. Fiulay at the Gape, was in March 1886
only 7 '6.* This proved to be the beginning of a stationary
minimum of indefinite duration. The star hag suspended its
fluctuations, and it is impossible to say when it may resume
them. Quite piobably ita history is one that " does not repeat
itself," Our coutinuouB knowledge of it is embodied in the
accompanying diagram (Fig. S). A single vast oscillation is
indicated, occupying about a century for its completion, and
diversified by secondary fluctuations of a very conspicuous
character (innumerable minor ones ai-e ignored in the figure).
The data at present available^ however, afford no grounds for
concluding this oscillafcion to occur regularly. Attempts to
aaeign a period to the variations of this object have signally
failed. Wolf's of forty-six,^ and Loomie'e of seventy years*
were both palpably too short ; larger time allowances encoun-
te'rfid obvious difficulties ; and y CariuiL^ was, by general con-
sent, abandoned to ita own lawless cotii-sea. Protracted periods
of light-change have, in several other easee^ been suggested,
^ Abbott, Monthly yoiicM, voL xxi. p. 230.
* Moe»t4, Attr. yaek. No. 1054.
' Tebbutt^ MonOUy Nolwt, vol, mi. p. 210.
* MoiUKty NoliCAt, Tol, ilvi. p. 340.
' Ibid. Tol. iiUL p. 20&.
'■ Ihid. ToL siii. p. 2e8.
THE SYSTEM OF THE STABS
bul Iwve in lume been verified^ onkn I>r. Lodendorff^s
tveoty-seTen jean fisr c Ami^ prove an exception.
stvB thej were aactibed to, wben Ukft Um£ caotc for a
tioo of their preemned cjclical changes, sbowed a total
of oonibnuity with what wae eipect^i of tbem. As eram|
may be mentioned 63 Cygni^ to which Mr. Eepin attribatedj
period of five, and R Cepbei, tbooght by Mr, Pogson to ol
one of seventj-three years.
Thus the gro&t southern variable cannot be depended
I
Mas-
n
i
^
J
^.
s
f
s
•04
/
\
1
.
M
f
\
1-4
h
J
1
_1
30
J\
./
'
I
,
y
\
\
1
/
'i
*^
'
— 1
i
XM
\
\
^
v^
V
—
—
—
-
1 <
k «
i
li
' i
li
f i
M
!: ^
n
M
\i
1 (
F -
il
' 4
'2
I
li
i
!i
j
upon to revive its past splendoors. There is nothing inevit-
able about the kind of fluctuation it exemplifles. One might
indeed any of it, in Jtick Cade'8 phra&e, " then is it in order
when it is tnost out of order/' IrregiUar light-change seems
to develop all its resources in the vicissitudes of ij Carinte.
They have included quick, yet sustained ascents in brightnesa,
and also evanescent kindlings. Stationary epochs huve been
followed by epoclis of inetabiUty ; at some times the star has
shown a tendency to establish itself at halting-places, at others
to slip along an inclined plane of change. In all this it
differs materially from temporary stars, which leap up, as if
STAES VARIABLE IN LONG PERIODS
109
hj a single impulse, to their Bolitaiy maximum, after which
ihsj loae m a few months the whole of the light they had
•equired. The nature of its light, on the other hand»
jasimilate& it to the temporary clasa. Sir David Gill's study
photographs takea with the McCleaa apparatus in 1899
QELStrated a close agreemeDt l>etweea the speictra of the
aoaldering variable and of Nova Aurigse when near
lunL* Hydrogen-lines, broad and bright, with dark
apanions on their more refrangible sides, were the leading
iture of both; and a feature no leas enigmatical in the one
than in the other. Yet the fact, as already remarked,
of profottud importance that the conditiousj transiently
praeent in Novte have been rendered permanent both in
ff Caiinse and in P Cygni, the qiiaai-Nova of 1600^ now an
imexceptionally steady fifth-magnitude luminary.
Among the miscellaneous objects comprised in Pickering's
class of variables are some slightly changeable third-
brilliants. Sir William Herschel added in 1V95 a
HeixuHs to the list of eeven fluctuating stars then known*
A period of two months assigned by him to its oscillation
between 3'1 and 3'9 magnitudes has proved illusory. During
some years the swing appears almost to ceaae, then is
hurriedly resumed, but with no settled order. The analogous
rariationg of Betelgeux and ^ Pegasi are equally unmethodical.
A. conspicuous brightening of the former star attracted much
attention in the autumn of 1902, but speedily subsided.
^_ The extraordinary character of a star long known as
^V Variabilis CorouEe/' now called " R Corouse," was discovered
^Hy Figott in 1795 ; a near neighbour of the "blaze star'* of
^■1366, its changes are of the nature of extinctions rather than
^^f outbursts. Ordinarily of 5 '5 magnitude, it occasionally
drops out of sight with small telescopes, and after lingering
below the tenth, or even the twelfth uuigtiitude for many
months, slowly regaiiifl its lost light. But its phases, at times
suspended, as during the seven years, 1817-13 24,* are
^tiid
1. ' Monthly ybtiutt toL IxL p. 456, App. iv.; cf. Earvavd AnnalSf vol.
nriii. p. 175 (Miu A. J. Cunnoii),
' Phil. Trans. toI. Ixxivi. p. i52.
* ArgelAucler, Soniur Biob. Bd. »'ii. p, 374 ; Olbera, Berlinf-r Jahrhixh,
110 THE SYSTEM OF THE STABS
&l others iU-Kkuked. Thxa at tfa« v&mimiuii obaerred bj
Sawyer October 13. 1885, the etar waa ettU of 7 4 magni-
tade.^ It abows ft peculiar spectrum oeeditig closer in-
vestigation,
B Cepbej is a star which, ^ce the beginning of thft
present century, has loBt JJ of its ladiaace, aad at preiieiit
in no way tends towards rec<»verr. In the time of HeveliuB
it was of the fifth magnitude, and Grodmbridge's observati<m
of it in 1S07 showed it to be then stUl unchanged. Bj
1840} however, it bad sunk to the tenth, and has never aiitoa
ii»ji aJ:*ove the eighth magnitude.* Its identity with the
" 24 Cepbei " of Hevelius, itacked out by Pogaon in 1856/ is
tmiversoUy admitted. Of late years it has shown no eign
of variability. Its light, considered by Schonfeld to be
tinged with red, appeared bluish to Farley in 1838*
Genuinely red stare are ordinarily subject to shiftings
of photometric staading. Among twenty - two such, kept
in view by M. Safarik at Prague, from 1883 to 1888,
for the express purpose of testing their constancy, only
nine remained without noticeable change, two were found
periodically, six irregularly variable, and five either vanish^
or lost great part of their light. Earlier observations of
several of these objects certified the progress of their decline
during twenty to twenty-five yeara.^ An example of a sudden
acqtiiaition of lustre is a£forded by a small red star in the
same field of view with y Cygni. Between December 1886
and June 188G, Mr, Espin perceived it to have risen iu rank
by a whole magnitude,^ that is. to be giving out two and n
half times as much light as six months previously. And so
far as is known the gain has been kept.
The track of recent astronomical progress is strewn with
the JiUpidated remnants of hypotheses invented to explain
the strange phenomena of stellar variability. Nevertheless,
much has been learnt as to their relationships and essential
natiire. The gaseous incandescence^ for instance, visible in
1 Jttr, Joum. No. 151,
« Bcb<JiLfeld, Mawtheimgr Jahrabmcht, Bd. xL p. 118 ; Oore'a Oataloyue^
08B4J, p. 200.
' Monthlif NoUeett toL xtiL p. 39,
• Aitr. Jfae\, No. W74.
' JourTtal Liv. Atir, iSoc toL v. p. 2.
4
STAES VABIABLE IK LONG PERIODS 111
Ibe spectra of periodic&l »lara near their maxima brings them
■into 8nch close physical i-elationship with temporary stoi'S as
: absolutely to prohibit the speculative separation of the two
kinds of change they respectively exhibit A theory stendfl
eelf-condemned which deals with them on diHereut principles.
Moreover, the association of variability with processes of
liuniooiis change in stellar atmospheres has been rendered
obrioiiB; and this at once diapoaes of darkening expediente,
M by Blag-fonnation, vaporous obBCuratioQs, and axial rotation,
bringing bright acd dark sides alternately into view. Equally
inadmissible is the rationale of stellar fluctuations by inter-
mittent chemical associations and dissociations at the atmo-
spberic outskirts of cooling bodies.' For the increase of light
&t maximum demonstrably ensues upon a real access of
incandescence, and is not a mere appearance due to the
dissipation of absorbing vapours. The fires really die down
and leap up at regular intervals ; they are not merely screened
oCr and disclosed.
Attempts have several times been made to explain the
periotlicity of stars through the influence of satellites revolving
round them in highly ew^ntric orbits. Klinkerfues suggested
great atmospheric tides, raised at successive peribeliou-paasages,^
as a means of bringing about periodic interceptions of light.
Plaasmann's ' view of tidal effects is wider, and perhaps
embraces a partial truth. For, just aa in the earth the
unequal attractions of aun and moon on its centre and
surface sometimes provoke, though they could not produce,
earthquakes, so the tide -raising power of bodies making
very close approaches to stars in a critical state of heat-
equilibrium may serve as the occasions of lujuinous outbursts
of a temporary or recurrent nature.
Sir Norman Lockyer's meteoritic hypothesis included the
pregnant idea that variables are to be regarded as " incipient
double stars." * But it had a different application to that
imagined for it by its author. There is no sound reason for
1 Br«Hter, Sssai d'un< TVoWe du SqUU ti /ka £tmUt Variahkt, Delft, 1880.
* OoUingiteAe ^achriehUn, 1&S5, p, S ; aee also Dr. WilaiDg's conunents Id
> Did Veriitiderlichtn Bemty Ebla, 18S8.
' Ftoc Soyal ^eUty^ toL xliv. p. SO.
112 THE SYSTEM OF THE STARS
believmg stare like Mira to be oomposed of twin meteor-
flvanns blaitiig tbrougb pemstral ooUlsione. That tbeir
lommoeity maj be affected hy the tide-raismg power of
UBseeu companioDfl, it would indeed be rash categorically to
deny ; yet thero is no evidence to support the opiniou,
while the periodicity of the objecta in question is of so diS'
turbed a kind as to raise almost insuperable obstacles agalEBt
connecting it with moTements necessarily punctual. More*
over, periodical cannot be sbaiply divided off from irtegd&t
variablea Every degree of perturbation, up to the total
Bubversion of laws of change, lb met with among them. Man)r
stars seem at timsa diapoaed to conform to a period which
they later ignore* In others, method is indicated, though too
vaguely to be defined, while the majority oscillate, with wide
allowance of amplitude, about a period itself often subject to
periodical or secular change. It is evident that the immediate
and unmodified interaction of revolving masses cannot explain
breaches of regularity widening out to its total destruction.
The time has scarcely yet come to formulate a general
theory of gteltar variability, but we may, at any rate, try to
render our ideas on the subject coherent, admitting provision-
ally those that are consistent with known facta, rejecting
summarily those that contradict them. It will then become
possible to realise with some distinctness the conditions under
which alone any such theory could be regarded as adequate.
As long ago as 1852^ M. Rudolf Wolf adverted to the
analogous character of the curves representing sunspot
frequency and stellar light-change.^ They are not only of
the same general form, but they are marked by precisely the
same kind of irregularities. Both are steeper in ascent ttian
in descent ; both rise into peaks of unequal heights at unequal
distances apart. Mira, ^ Cygni, K Hydrae, and the rest, have,
like the sun, retarded and accelerated, high and low or abortive
maxima. The representation in Fig, 9, from the Greenwich
observations, of the changes in sunspot frequency during the
decennial period 1867-1877, is the very counterpart of the
Ught-curve of a variable star. Especially charaeteristie is the
break in the descending branch reflecting a partial recovery
1 ifiUhnlitngen Naiur/orKh. OueilaeJui/i, Bam, lSb% {>, 201.
STARS VARIABLE IN LONG PERIODS 113 ^H
i& the downward course towardB miaimum, to which variable ^^^k
Etara of HifTerent classes are proue, and which maj even^ as ^^^k
ttk R Nonn^, assume the importance of a Becoud co-ordinate ^^|
mudmum. Moreover, the How of change in sun and stars ^^|
alike is broken and disturbed by the superposition upon the ^^|
normal period of subordinate and superior cycles ranging from ^^H
i few days perhaps to centuries, ^^H
The presumption tlien of their similai' ori^u is very ^^H
sLrung: nor are we wholly without evidence of a physical ^^H
nature to the same effect The development of bright lines ^^H
' in the spectra of variable stars near their maxima is paralleled ^^|
1^ .»
jTX
f
=—
f
V
}
V
A
f
\
{
y
f^\
W feo
1
\
■ 1^
/
V
'
1^ o
^
\
■■ »!^
\
■ ^40
}
\
^1 £ ^"
/
L
■ ^^°
/
\,
f
_ ... .
\
/
^
=—
*-•
^^^H 1807 (558 1B6Q TQ70 1071 1fi72 1873 1574 1375 1678 1877 ^^H
^^^^B Year* ^^H
^^^^^P Fto. 0,— Gnrv* of Soiupot Fnniucncy, 1347-77 <BlllA> ^^^|
in the sun by the iucrease of emissive intensity in the oorona ^^|
as eunspots increase^ as well as by the attendant development ^^|
of calcium Hocculi shining by direct radiation. Atmospheric ^^|
incandescence is thus in both cases heightened, although in ^^|
irnrneusely different degrees: and continuation is afforded to ^^|
what was already certified by the congruous shapes of the ^^^k
two curves, namely^ that the maximum of spots in the sun ^^^k
corresponds with the maximum of light in stars, and iiic^ ^^^k
verad. It is the more necessary to bear this in mind, because ^^U
obscurations by spots have sometimes been alleged as a cause ^^|
of stellar variability. That just the opposite is the truth has ^^U
been further certified by a beautiful mathematical investiga- ^^^W
tioQ set on foot by Professor Turner in 1904.' Submitting y 1
^^k ' ifvnihly N^tieatf ToL bdr. p. S13. ^^^|
THE SYSTEM OF THE STARS
to the methods of harmonic analysis eleil&r Ught^urres and
the curve rej'resentiag solar cycJiDul activity, he obtained
cc9ults of emphatic import aa to the identity (it might be
said) of the constructive principle at their base, provided that
maxima of spote be regarded as the coiTelatives of maxima of
brightnesa. But tba agreement vaniahed when the trial was
made of inverting the reUtionahip., i
The conclusion that Bolar and at^llar disturbances are alike
in kind clears the ground for further investigation, for,
beeidea obliging u8 to reject cauBed for the latter which
are demonstrably unconcerned with the former, it renders
snnapot studies tlirectly available for Bolving the problem of
stellar variability. Now what do we really know about the
production of sunspots ? Not much more than that they arijs^
incidentally to the great cii-culatory process by which photo-
flpheric radiations are maintained. They arise, beyond question,
when it ia most active and tumultuous. Nor is there anything
to show that the variation in their niuubers depends upon au
external causa It seems, on the contrary, to result &om
peculiarities inherent to the solar constitution — from the in-
tncate movements proceeding withijj the vast globe, and
accommodating themselves somehow to those due to the
swirl of its rotation — from fluctuating relations of heat and
pressure — from the alternate accumulation and discharge
of explosive forces, perhapa of a molecular nature. Similarly,
the secret of stellar light-^ioiBsitudes is held by the stars
themselves, although superinduced modifications may also, in
some cases, be recognised. But that their periodicity is
essentially self-regulated becomes manifest through the con-
sideration that it is materially influenced by colour. Not
only a very large proportion of red stars are variable^ but
nearly all variables of long period are red. The length of
the period^ too, ia very distinctly connected with the intensity
of the colomr. This was first noticed in 1873 by Dr. Schmidt
of Athens;^ it was reaffirmed by Mr. S. C. Chandler, who
concluded, after an elaborate study of all the facts, that " the
redness of variable stars is, in general, a function of the lengths
of their periods of light variation. The redder the tint the
longer the period." '^ And Mr. Yendell has quite lately
* A^iir, Nach. No. 1SS7. » At(r. Journ. Nos. ISO, 1»3.
STARS VARIABLE IN LONG PERIODS 115
leached a similar conclusioa^ Many individual exceptions to
the rule might be cited. But it prevails in a large sense ; and
its prevalence enforces the obvious truth that the explanation
of redness in stars lies very close to the explanation of their
vambilitj in long periods.
1 A^r. Joum. No. S64.
CHAPTER iX
TARUBIR STLRS QF SHORT PSKIOD
We have seen, in the lost chapter, that stara vajyiiig their
light in perjotis of leas thau thirtj' days stand apart in
several important respects from those undergoing slower
changea. The distinction \a aocentuated bj the tendency
apparent in each claae to group its members as far as possible
&om the frontder-line of separation. Thu^j most long periods
exceed two hundred days, while a large majority of short
periods fall below eight. The total number of stars so far
found to be variable within a calendar month is eighty
(besides a multitude of faint objects crowded tt^ther in
clusters); of these seventy complete an oscillation in less
than ten days, while sixteen bare periods measured by hours.
Fig. 10 gives a graphical conspectua of these facte.
Variables of short period are, as we have said, nearly all
white or yellow stars, showing spectra of the Sirian or solar
type. They fluctuate much less extensively and much more
precisely than Mira-variable-s. In many rapid stara the light
ebbs and Hows like clockwork as to titue^ and as to measure,
viitb deviations scarcely of the tenth of a magnitude ftom a
settled standard. These remarkable changes progress gradually
and continuously in Pickering's fourth class of variables; in
hiB fifth class they only interrupt, although at perfectly regular
intervals, the usually steadfast shimng of certain stars. Of
these two kinds the former is conspicuously exemplified in
Lyrse — a star of which we have already made the acquaintance
in connection with its gaseous spectrum — the latter in Algol.
Further distinctions, however, have to be mada Class IV,
really comprises three separate families, which may conveni-
ng
■
^^
■
n
IRfW
1
n
W
1
p
i
P
i
1
!t
TESTi
i
■
■
ff
n
■ ently be designated as Cepheid variaMea. Cluster variables^ and
I Geminid -variables. Their several characteristica we ehall now
1 briefly indi(?ate.
H One peculiarity, full of meaning in itself and in its
m implications, is common to thero all. They are, probably
■ without exception, close binary eysteme revolving in the
■ period of light-cbange. Tbia was long ago suspected of atara
1 undergoing brief phases of obscuration ; and the fact, as regards
^^L Algol, was definitely ascertained by Dr, Vogel in 1888. Aboat
^^M thirty analogous objects ars already known, and there ia slight
^1
1
-
—
—
i
I
^1
/
\
/
^
j
i
1
V
1
N
f
\
\
V
/
I
V
\
)
J
V
/
V
s
/
>
/
N
/
S
Under 1'^ 2 3 4 S b 7 B d 10 11 t2 13 {4 15 16 17 IB 19 2fl ^^^H
Fta. la—DtKtiibaUoQ of 60 Vuiible-Bur Periods under 30^. ^^H
ri^ of ertor in describing theiu genericaUy as ** eclipsing atata."
"Far more surprieiug was the discovery that stars fluctuating
in a manner inconfiistent with the eclipse hypothesis shared,
nevertheless, their compound nature. Take^ as an example,
& Cephei, the light-curve of which is depicted in Fig. 11. It
is by no means Bymmetrical. The ascending is much steeper
th&n the descending branch, and the latter is besides markedly
f inflected. Now the great majority of sporadically occurring
short-period variables belong to the type thus illustrated. In
many, it is true, the pause in the decline from maximum is feebly
accentuated or imperceptible ; but most gain brightness about
118
THE SYSTEM OF THE STARS
twice aa quickly as they part with it, and all accomplish their
changea by uuinterrupted gradations. They are continually
on the moTe ; tliey have no definite halting-places, either at
maximum or at niiuimum. This mode of yariation is clearly
irreconcilable with eclipse-conditions, and the anticipations of
reason have been confirmed by experience. Yet the objects in
question are, in point of fact, binary stars, and their revolutiosa
Btrictly control their light-changes. This is known from the
synchroniam of the two kinds of observed effect— of the
spectroscopic alterations due to orbital movement, and of the
photometric periodicity. The variable radial velocity of
S Cephei was detected by Belopobky in 1894;^ and that of
7} Aquilio, a star similarly Tariable, in the following year.*
In both systems the companion -body is obscure ; in both the
occurrence of eclipses is precluded by the circumstances of
Mat
/
'\
V
f
\
j
'
^
■^
At
/
"^^
4.
+■7
[y
^■^
•
H
j ^
i
4
b
Fio. 11.— Liglit-OlUTo of DoltoCeptini.
movement. Both atar8 give spectra of the solar type. The
further recognition, aa spectroacopically double, of the Cepheid
variables, X, W, and Y Sagittarii,^ of T Vulpecula? * and
S Sagittse, adds weight to the accumulating evidence that
the peculiarity may be generalised. Thei-e need be no hesita-
tion in affirming that the pattern of variation set by B Cephei
ia prescribed by the circling, in an identical period, of a
usually non-luminous companion.
" Cluster variables " are met with by the score in certain
globular clusters, and scarcely at all in the open sky. Hence
their current title. Their discovery by Professor Bailey in
* Aatr. Nach. No. 3257 ; Jatroph. JourK. vol. t p. 160 ; Bull, de L'Ac
ds St PiUrthouTQ, Not. U94, No. 3, p. 288.
* Atiroph. Journ, rols. vi. p. 3&3 (B^Jopolaky) ■ ix. p. 59 (Wright).
■ Sli|)het^ B-uileUn of iht LovMii ObservaU/ry, No. 11 j B. H. Ciuttss, Lick
Bull No. 62. t
* Frn«t, Attroph. Jonm. vol. xx. p. 206.
iCffl^^
VARIABLE STABS OF SHORT PERIOD 119
1895 remarkably illoatraled tlie perfection to which the,
photographic method has been brought. To individualise th*i
minute^ throagiiig components of compressed clustera would,
outil lately, have been regarded as «. notable feat ; to follow
their variationa of lustre through brief cycles of about twelve
hours, and to determine their special character, might well
hare seemed impossible. The camera alone is competent
to undertake work at once so delicate and so comprehensive.
With two or three of the most powerful telescopies in the
world, these tiny Ughb-apecks can, indeed, be observed to
good purpose (^ Professor Barnard haa shown) ; but only
Mac-
13-0
V.
\
<,
{"]
\
14*0
\
s^
J
N
b
53^
^^
/
'
! •
r '
1
1
'
13*0
^
/^
\
HO
'^
^
-
/
\
W -
r -i
'. •
J
*' •
b ■
i
f .
i -^
Flo. 13.— TyTdcoJ Lighl-Can-H ol Clii«t«r VarUbles.
one by one^ and they demand wholesale treatment. Some
etar-globes contain shoals of variablea ; over 500 have so
far been regiatered, besides upwards of a thousand in the
Magellanic Clouds,' The variations of stars in clusters, mote-
over, are by no means vague or indeterminate. They are
executed with punctuality and precision in perioda^ very
generally, of leaa than one day. Three light-curves, two
typical and one individual, are shown in FigS- 12 and 13.
They are ci>pied from Professor Bailey's dravrings illustrative
of his elaborate discussion of the conditions of variability in
the great eouthem cluster to Centauri.' And they are, in all
' Pickering, Harvard Circ*ilar, Noa. 82. 9&, 100.
* Uarvani Annals, toI. xxsviii. 1902*
120
THE SYSTEM OF THE STARS
13-0
13-6
14-0
0^ ,t -2 ^a '4 -5 -fi -7
Fid. 19.— LletiMTorre oJlTo. 4i Onega CeDtcari.
auch groups, strangely imiform. A swift riae to maiimum,
and & proloaged halt at minimum, are their lading tmita
Cluster variables are dis'
"^'^^ ^ tmguished from Cepheid
vnrjablea. partly by the
auddeimeaa of their up-
springing, but most eesen-
tially by the relatively
protracted duration of their
dim phases. About half of
each period is gpeut at a dead level of low light ; then all at
once tripled brightness supervenes, to ebb away again by slower
gradations.
Why stars thus singularly afifected should so strongly tend
to herd together, none can at present attempt to divine ; but
the exceptions to the rule of aggregation claim particular
attention^ if only for their rarity. One of them is S Arse,
noticed as variable by Mr. Innes in 1898.^ The curve by
which he delineated its course of change is copied on a reduced
Mac.
9-0
9-2
j
/>
I
r\
\
1
'
\
\
/
V
■-^
^
/
^
i
> •
I
1
(
i ^
I
^
D 1
Fio. U.— Ught-OurT«i>f S Ana.
scale in Fig. 14. Scarcely distinguishable from one of Bailey's
typical tracings for the variables in q> Centauri, it shows a
stationary minimum lasting four houra, then a more than two-
fold increase of lustre within an hour and half, followed by a
leisurely decline in approximately five and a half, by which
the cycle of nearly eleven hours is completed, Y Lyrse is
almost the alter ego of S Ats&. Mr. Stanley "Williams deter-
mined its period to be 12^ 4^^, the riae from 11-3 to 12"3
' Capt AniuiU, vol. ix. p. I2Gs;
Monikly Notka, vol, Ixi. p, 108-
AstT, Jitu/m. Nob. 401-92 (Eoberti) ;
VARIABLE STABS OF SHORT PERIOD 121
m&goitade being accompLiahed in 1^ 30*^; and he baa eince
asBOciated with it a star in Cygnus (designated " UY Cygni **)
following nearly the same preecription of change.^ Madame
Oer&aM's cliister-vaiiable, also situated in Gygnus, i& beUeved
to have the extraordinarily short period of 3*^ 12"^ and an
oaeillat ion -amplitude uf approximately one magnitude. Dia-
covered photographically in 1904, it demands special and
adroit study.
The third aub-claas of short-period variables, called
* QezDinids" from their exemplar ^ Geminorum, alter in
brightness by continuous and aymmetrical gradations. Their
maxima are placed about midway between tlteir minima. All
(we need not hesitate to eay) are binary systems^ but some at
least are eicempt from eclipses. The line, however, separating
thidDi from occulting variables is very feebly traced. Whether
or no eclipses occur has to be decided by a distinct investiga-
tion for each individual star, and the process of decision
advances slowly. Only in one ease a conclusive reply has
been obtained, and it is in the negative. B^lopoleky and
Campbell independently, in 1898,^ recognified f Geminorum
as a spectroscopic pair revolving in the period of light-
change ( 1 0"* 4^), One component ia invisible, yet the
observed minima are not due to its intervention, siiice their
epochs are not those of conjunction. Eclipaea can naturally
only take place when the two bodies concerned are in the
same line of sight ; and the spectroecope intimates their being
in the same line of sight by the reduction to zero of their
radial velocity. They must, in other words, at the time of
ocjcultation, be moving across the line of sight. The non-
fulfilment of this condition by f Geminorum excludes it
peremptorily from the number of eclipsing variables.
The light-carve of U Vulpecuhe (fiee Fig. 15)* so closely
imitates that of ^ Geminorum that we need have no doubt of
the atarB being similarly circumstanced, S Antliae, formerly
taken for an Algol variable, belongs to the same category. At
its maxima the How of change is so slack as to suggest au
^ Monthly N^oliixg, vols, liiii. p. 304 ; liv. p. 686.
* AHr. yacA. No. 8565 ; Aitroph. Joum. vols, ir, p. S6 ; xLii. p. 90.
' MnJierind Eflropf, A9tr. Nadi. No. S483 ; LmKutj ibid. Wo, 3670;
Itarnirii Cireviar, No, 41.
122
THE SYSTEM OF THE STAES
actual Btatidstill, vrhile the minima are oompaiatiyelj Bharp^
jMid the entire cycle u aocamplished in 7** 47* It hag
yieldeii, so far, no spectroscopic signs of duplicity.
««
s.
1
; t
,^
S.
\\
/
!>
Is
/
\
—
s
/
N
/
'
s
/
S
y
'^
i^
p
3
4
S
t
1
1
Fio. li-— Ll^t-Gumt 0* tJ Vu!i»«rai».
Some Greminid stars are subject to what may be called a
double periodicity. They dip, that is to say, to a secondary
miDimum placed half-way between two equal maxitna. Thia
mode of variation is brilliantly illustrate in )3 Lyrse, the
saddle-back curve of which is shown in Fi^. 1 6. Its fluctua-
Mkc V\
15
tions, detected by Goodricke in 1784, were completely tracked
out by Argelander in 1844.^ Their cause ia nevertheless slill
involved in perplexity. The star is known to be binary, but
the complex changes in its bright-line spectrum profoundly
embarrass measurements of its velocity. The evidence at
hand does not preclude the hypothesis of disparate obscura-
tions at the primary and secondary minima respectively ; it
does not, however, enforce it, and a solution to the enigma
presented by this star will perhaps be most easily obtained by
the indirect means of studying it at second-hand in analogous
objects of less complicated relationships.
D% SUllA ff Lyrtt DitquUitio.
VAfilABLE STABS OF SHORT PERIOD 123
One Bucb is found in V Puppis, the light-curve of which,
as drawu by Mr. A- W. Roberts, is shown in Fig. 17- Its
similarity with that of ^ Lyrie doee not need to he pointed
out. If the oecurreDCti of a double eclipse can be proved in
one esse it may be preHuined in the other. A Bpectroscopic
pronouncement on the point is awaited with much interest,
and should not he difficidt to procure. Already, in 1895,
V Puppis was ascertained by Professor Pickering to be a
spectroaoopic binary, composed of two unequally bright stara.^
Nevertheless we are still ignorant aa to whether their move-
ntentB satisfy the requiremeata of the occultation- theory.
Meantime the photometric data collected by Mr. Koberts have
been shown by him to agree remarkably well with the light-
variation resTilting from the mutual eclipsea of two bodies
0E3 t 9 r5 iS S S 2A~^ S3"
Flo. 1?.— Llght-Ciirv«of VPuppts.
i'i 4i
circulating in contact.- Actually in contact they should be,
perliape even confluent ; but this involves no mechanical
imposeibility* It would, however, involve the consequence that
th@ mean density of the double globe of V Puppis could mot
exceed ^-^ that of the sun. Other analogues of ^ Lyne are
U Fegasi, E Sagittae^ with a period of 70, and V Vulpecuhe,
accomplishing its changes in 75 days.^ That the spectroscope
will eventually supply evidence of their binary chara^iter is
scarcely doubtful, but it does not follow that all or any of
them are eehpsiug binaries.
"We would now invite oiu* readers* attention to the five
hght-curvea grouped together in Fig. 18. They are copied
torn an instructive paper presented by Mr. A. W. Eobeits of
* Harvard Cireulart No. 14,
■ Attropk, Jaum, vol, JEiii, p, iSl.
> Arlr. J^aek. Ko. 3929 (SUuIef Williama}.
VARIABLE STARS OF SHORT PERIOD 125
Lovedttle to the South Afrioim Aaeoctation for the Advaace-
ment of Science at its first meeting lu 1903. It embodies his
principal cooclusions regardiog stellar cclipseg, and vividly
illostrateft both the variety of conditions under which they
tike pl&c« and the difficulty of pronouncing, In certain casea^
for or against their genuine occurrence. Thua, the light-^urvo
of R' Centauri (No. 5, the lowest In the dhigram) is that of a
Geminid star. The stationary maximum character is tic of
AJgol variables is absent. Mr Roberts, nevevthelessj consider*
the star to be composed of two egg-shaped bodies rotating
oa a common axis in 14^ S2"^, and sending us more or less
light according as we see them broadside or end-on.* The
forms corresponding to the observed variations in brightneas
are depicted in Fig. 19, the dotted lines indicating Darwin's
figure of ecjuilibrium for a liquid globe on the brink of fission
through accelerated rotation. The close agreement between
;,be forms arrived at from photometric and mechanical con-
Jderations reepectively U of strongly peraufisive import.
Curve No. 4 in our figure is of an intermediate type.
X Cajime verges towards the condition of unceasiog change
viaible in p Lyrae and S Antliae ; yet brief intervals of stable
shining appear to interrupt the proceaeea of decline and
recovery^ which Mr. Roberts expounds as the phases of a
protracted double eclipse. Two stars, somewhat uoequaUy
brilliant, are beUeved to be concerned in them, the minima
being slightly unequal The orbital period of 26 hours thiis
includes two light-periods.
' jiftr. Jourti. Noa. 37B, 384; Aslroph. Jmrn. vol. x. p< 312; Uonlhly
Noticti, roU btiii. p. 627.
126
THE SYSTEM OF THE STARS
The variability of K* Velorota, suspected by Kapte
eetabliahed by Innes in 190 1^ and further defined by Rol
It has ft pericul of 1** 20^" ; and the light-curve (Fi^
JSo. 3) intimates the occun^uce, within that apan, of
abortive, as well as of a sharply pronounced eclipse,
bright and a dusky st^ir are thus perc^iyed to be combined
thia system. Each timo that they come into coujiiDCti
there is a noticeable diminution of their joint light, but the efll
Ib conspicuous only when the lu£fcrous body pas&es behind
companion.
The curve of R Ane (No, 2) includes no seoondl
drop. This shows tlio occulting globe to be sensibly obscn
Its concealment mukos no difference in the sum -total
light. I
S Velorum is one of many variablofi detected during t
construction of the Cape Photographic Durehmusterung. 1
Ci Eay Woods first noted its fluctuations in 1894,^ and M
Roberta ably investigated the oatui'e of the fiystcm in whi(
they arise.' A large semi-obscure star has, it appears, a ixA
paratively small but much brighter comiianion revolving i
5^ 22^^ The obscuration represented by the profoul
gap in the curve (Fig. 18^ !No. 1) is due to the tram
of the dim primary over its lucent satellite, which
completely hides duj'ing a minimum lasting 6^ 35". F
so long, in short, one star is, to our vision, substituted I
another. Thia ingenious theory^ however, is hampered by tl
anomalous consequence that the hiatrons globe must, on i
showing, be twenty times denser than ita obscure attendai
Ite final acceptance depends upon the verdict of the specti
We have insensibly passed on from Geminid stars to €
consideration of Algol variables. These, which foim Pickering
Class V,, are of very peculiar interest from the amount of pi
cise knowledge which they place at our disposal. Tht
characterSj accordingly, invite close scrutiny and minute coi
parison with theory. Variability is in them by short aceesa
and consists always in a temporary loss of light. Tbi
undergo, in fact, what are now known to be real eclipses
1 ^str. Jou-m. No. 508. ^ Monthly Nctix^t^ toL Iv. p. 2n.
' A^r. /oum. No, 327 ; A^to^k, Jowik, tdU, it. pr 270 i x, p« 314,
A
intervalB, wMle shiniug, for the most part, as steadily
■ binary stars. Their detection is for this reason so difficult
iintil the era of pliotogruphic discovery began, acxjuaint-
with them was casual and scanty. "Novr, however, about
ty figure in our catalogues, the designations of which are
BQ in Table III. of our Appendix ; and Che list excludes auch
ious instances as S Antliae, in which the occurrenoe of
lipees is still auh jvdice.
The eponym of the claee is curiously exact in its changes,
''iich have been long and accurately observed. Their extra-
linary character was determined, and an explanation of them
interpositions of a dark satellite suggested by Goodricke in
r83, since when some 15,600 minima have occurred in a
Etnuer perfectly consistent with the hypotheaia. It became
en of great interest to test its absolute truth, and the first
Qeane of doing so were afforded by Professor Pickeringa strict
L'^ntiuiry into the conditiona of the gupposed recurring eclipse.^
t*They proved to be all but perfectly complied with. Outside
«f the twelve hours during which the " Demon-star " parts
ritb and regains two-thirds of its light, it displays the re-
red uniform lustre. The oac-iUation ia the same^ or very
rly the aame^ in duration and extent now that it was fifty
ago, and that it probably will be fifty years hence. The
cision of itn performance seemed to correspond far better
with the reaulta of geometrical rule and measure than with
those of the complex interaction of physical causes ; and the
spectroscope testified in the same sense by showing the sur-
iving light at minimum to be of unchanged quiility. It \b
amed, as if in large meaaut'e cut off, but betrays no symptom
of intrinsic modification. These singular correspondences have
not proved dec^iptive. The poatulated eclipses actually take
place.
The manner in which their genuineness has been estab-
lished illustrates the singular versatility of modern metboda
of research. No problem in which distant lighb-sourcea
are concemefl seems hopelessly beyond their grasp. The
received explanation of Algol's chfinges evidently involved
the mutual revolution, in a period identical with theirs^ of the
eclipsed and eclipsing bodies. And since their orbits, to admit
' Proc Am*r, Acttd. ti>1. viii. (ISSl), p, 17 ; OhtcrveUory, vol. It, p. 116,
128
THE SrSTEM OF THE STAES
of a transit of the satellite over the prmiaiy, should Me ai
edgowise to our sight, practically the whole of their velociV
should, in the course of each revolution, be direct*^ alti3n]»i
straight away &om and stmigbt towards the earth.
accordingly, spectniecopic meaeuies, recommended by Profi
Pickering/ were clearly applicable ; and their phofcoj
execution by Prafeasor Vogel in 1888-89 * eventuated in one
of the most remarkable verifications of theoiy on record.
Before each minimum Algol wa* found to be movicg
away from the eun (independently of a continuous translation
towards him of 2^ miles a aecoud) at the rate of 26^ Euglisb
miles per aecx)nd ; after each minimum, to be approochiog
with an equal speed ; while at intermediate timee the Im*
printed lines, by resimiing their normal positions in the
spectrum, proved the star to be then moving perpendicularly
to the viBuul ray< Multiplying this velocity (of 26 J miles) hj
the number of seconds in Algol's period (247,735) we get ao
orbital ciivimifepence corresponding to a diameter of (ia round
numbers) two million milea. Moreover, since the proportionate
dimensiuns of the bright and dark bodies are aliowu by the
amount of obscuration of one by the other to be vety nearly
as 100 to 83, their relative miisees would also be known, if
we conld be sm-e that they are of the same mean density
The assimiptiou as regards a mass sbining with great brilliancy
and one almost totally dark is certainly a hazardous one> bot
it receives some warrant from tlie example of the sun and
Jupiter. By its aid Profeesur Vogel mrived at the following
ppoviaional data for the system of Algol -. —
DianieUr of AJgol
„ satellite
Difitance from centre to centre
Orbital velocity of Algol .
„ ,^ sateUite
Uaffi of Algol
,. aateUite .
1,061,000 English iiuie&
834,300 „
3,230,000 „
2&'Z milei -pes sea
05-4
* mUt DlUIL
t
In the accompanying diagram G marks the centre of
gravity round which both stars revolve with velocities in-
Tersely proportional to their maases. Thus, Algol travels in
^ Proe. Ayfter. Aoad, toI. viiL p. 34.
* Attr. N*i6k. No^ 2H7.
VARIABLE STAES OF SHORT PERIOD 129
\Algcl
•C
AH orbit of only half the compass of that of its compamon.
because possessed of twice its attractive force. It is easy to
aee, too, that the duration of the eclipse compared with the
length of the period gives the relation hetween the diameter of
the occulted body and the diameter of the orbit of the occulting
bcNiy, 60 that the absolute dimensions of one becoming known,
thoee of the other follow.
The density allte of Algol and of its satellite must be less
than a quarter that of the sun, or 0"38 that of watet. They
are both then presumably gaseous. Some slight dLssynimetry
in the phase-curve, formerly per-
ceived or imagined, and set down
by Dr. Wilsing ' to the account of
ellipticity in the path pursued,
has not of late been verified.^
Although the interval between
AlgoVe succeaaive eclipses shortened
by eight seconds between 1790 and
1S80, when the process bociime
reversed; it does not follow that
the star's orbital period is subject
to alteration. Dr. Chandlez holds
^^e inequality to be merely apparent
^K-to represent the time occupied by light in crossing a wide
ellipse described by the occulting pair round a supposed dark
primary.* The visibility of the phases would, if that were so,
be alternately accelerated and delayed according as the body
undergoing them was on the hither or the farther side of its
great orbit Nor is it impossible that Chandler's theory may
ultimately be directly verified by the micrometrical measure-
meut of undulations in the proper movement of Algol *
corresponding to its suggested spacious citcuitings in a period
of about 118 years. M. Tisserand, on the other hand, rejecting
the idea of a triple system, explained the deviations of the
eclipses from their normal epochs by a progression of the
^^De of apsides due to the presumed spheroidal shape of the
^^ ' Astt, Na£h. No. aoao.
! " G. MiUler. Pfid. No, 3732 ; H. 0. VogeU F. J, S. Astr. Qei, Bd. xiiri,
^ 140.
> AHr. Joum. Noi. 26&-5S, 509. * Boaa. Hid. No. 813.
•^□Ark SatellTto
Fid, 20 — Algol during an E;cUpM.
130
THE SYSTEM OF THE STAHS
contiguous globes.^ This would necessarily bring about a
cjclical fluctuation in the eclipse -period. Yet here, too>
contouation iii etill UcJcing ; the implied eccentricity of tb«
star's orbit not being spectroaoopieally apparent.
It needa no argument to ptove tliat the edipee-theory of
the variable in the head of Medusa mnst apply to all other
memberg of the same sharply characteriBed class. Many d
them, however, present anomalies which are the more de-
serving of careful etndy that they may one day throw an
important light on the circumstancea imder which combina-
tions of the indicat*ad kind exist.
The light-change of S Canuri was discovered by Mr. Hiad
in I84S. and its peciUiar nature ascertained by Argelander in
1852,' The atar remains steady during thirteen-fourteentha
of its period, then declines, in eight hours and a half, to \ss»
than one quarter of its usual brightness, which it regains in
the course of thirteen hours more» The process of recovery,
besides being abnormally Blow, is interrupted soon after it baa
begun by a miurked pause,' represented graphically from
Schonfeld^s observations in Fig. 2 1. The compass of this
atar'a change appears to be by no means invariable. On April
14, 1832, Schmidt observed at Athens a minimimi nearly two
magnitudes :fednter than any he had seen before. During one
hour the star remained sunken nearly to the twelfth magnitude.'
The period of S Cancri is subject to a perturbation with a
range of about forty minutes^ and embracing rather more than
three hundred minima.^
Inequalities of this kind, which in Algol sum up to a few
seconds in a century, and grow to many minutes in S Cancri,
BIO in \ Tauri counted by hours.* Their method and cause
have stiH to be unravelled The companion of X Tauri ia
not, like that of Algol, entirely obscure. M. E^lopolaky
spectrographically resolved the variable, in 1897/ into an
uneqUiiUy bright pair, revolving in 3*^ 23^ the period of light-
^ Compttfi Stndua, t cii. p. 125.
* jistr. XiuJi. Nob. /&6, eCH, SOft.
• rurtetJahrtsehTi/i Aatr. Qes. Bd. ix, p. 230.
* AKr. Nach. No. 24B1.
AfgeUnder. Banner Peob. Bd. viii. p. 397 : Schonfeld^ Smtw, Bd, t. p.
' SobbitfeM, Jahrfsbtriehi, HaEiubelm, Bd, il, p. 7@.
» Ajtr. iVaeS. No. S47<.
VARIABLE STAKS OF SHOKT PERIOD 131
ige, A secondary minimum, detected by M. Plassmatm in
i90.^ corresponds to the octultation of B^lopolsky'a faint
iponent, as the chief minimum tloea to that of its prim&ry.
iie disparate couplad eclipses of R* Velorum (Fig- 18, No. 3)
thns repeated by X Tauri
The variations of U Cepheij first recognised by M. Ceraabi
M06COW, Jmie 23, 1880, are unusually rapid and extensive.
In four and a half hours the star is reduced to about one-
ninth its ordinary lustre, losing light, at one stage of its
ddcline, at the astonishing rate of more than one maguitude
an hour ! The obecurity laets an hour and a half, but not
MftC. &-2
s.
^-^
■"
V
>
/
a-fl
1
\
/
^
t
/
S'2
\
^
1
-j
B-4
Be
V
— = — -
7
\
, >
^
/
\^
O* 2 4 S a "lb 12 14 I© f8 20 22
Via. 21.— UtDimnm of S OsocrL
with entire umformity.^ The lowest point is touched at
first ' and a pause in the ascent, like that inflecting the light-
curve of S Cancri (see Fig. 21), is indicated. Mr. Yendell,
on the other liand, pronouncea the light-curve to be sym-
.etrioal, and regards the minima aa annular eclipses of two
inra' duration.* Some complicated irregularities in the period
of U Cephei have been ascertained by Dr. Chandler, and M.
Plasamann observed the minimum of April 27, 1902, to occur
2* 27" later than the calculated time.*
The period of Y Cygni, added to the list of Algol variables
* Plftsstoami, DU vtrandtrlKhin Sterne, p. 42 ; Journ. BrU. Avtr, A»9, toL
L pp. 137, 255. 5 Bohlin, Astr. Naeh. No. 3762.
* CliMdler, AUr. Joum, ITo. 199. p, 63, * A$tr. Jovm. No. 551,
9 Aatr. JVooi. No. 37M.
132
THE SYSTEM OF THE STABS
by Dr. Chandler, December 9, 1886, averages about a dnj
and a half,^ but iSuctuutes to an extent unparalleled is this
kind of star. The retardation of its phases between 1887
and 1888 amoiHiEod to seven hours, totally disconcerting pre-
diction, and the jieriod soon afterwards set about shorteniu^'
as rapidly aa it had lengthened before.* The actual change
does not exceed half a second at each of the returns, but these
are so numerous that the accumulating errors sum up in a
short time to a startling aggregate. They have been success-
fully rationalised by M. Dun^r ' on the principle applied hj
Tisaerand to the irregularities of Algol The phases of Y
Cygui, however, are duplicated, the conjoined stars being twins
in size and splendour. Hence they take it in turn to be
eclipsed, and revolve iu twice the mean interval between their
conjunctions. Their orbit has an eccentricity of 0^145 i its
major axis completes a gyration in forty-one years; and its
varying position with regard to the hue of eight determines
the amount by which any individual eclipse falls behind or
anticipates its due epoch. The system of Z Herculia, although
composed of diasiniiJar stara, exhibits analogous symptoms of
perturbation to those presented by Y Cygni*
Stellar eclipses, it need hardly be said, are purely relative
phenomena. Their occurrence depends upon the situation of
the observer. But the chance of their being visible from a
distant point augments very greatly yrith the closeness of the
revolving stars ; for which reason, and also because the phases
recur more frequently when the orbit is narrow, Algol
variables with periods exceeding four or five days are of
extreme rarity. Until 1902> S Cancri was the only such
instance known. In that year, however, Mrs. Fleming dis-
covered in VZ Cygni a star with an eclipse-interval of 31*3
days,^ or more than thrice as long as that of S CancrL Each
of its minima lasts two days, and the loss of light amounts
to two magnitudes. Secondary obscurations, symmetrically
dividing the period, have lately been detected by Hartwig,**
' 'ChftudtEr, Asir, Journ. Nos, 163, 185. '^ Ibid. No. 204.
^ Aitr. Naeh, No. 3467 i Astroph, Jovm. rol. xi. p. 175 ; Kncwkdgej toU,
icy. p. 87 ; rTi, p. ItJe,
* Dmn^r, Attr. Joum. Noa. 374, 3S4, 422 ; AstToph, Joum. toL i. p. 2S6 ;
Yendel], Aair. Journ. Noa. 328, JS6.
» B^CLTvard Circular, No, 66. ■ Aatr. Jfach. No. 3944.
VAEIABLE STAilS OF SHORT PERIOD 133
and occasion some perplexity hj their apparent recalcitrance
to the hypothesis of a double eclipse. Their observer^ in fact,
diacajrck that hypothesis, und suggests Insteud the view that
VZ Cygni is a " pear-shaped " body or " apioid," rotating in
what was taken for the period of its systemic circulation.
Eclipsing Rtara are remarkably tenuoua bodies. The com-
parison of the duration of their transits with the periods of
their revolution supplies means for deducing a limiting value
for their densities/ and it was fixed by Mr, H. N- Ruasell in
1899/ from an average of seventeen stars, at one-fourth that
of the sun. Mr. A, W, Roberta, working independently on
the aame lines, found the mean consistency of four southern
Algol-paira to be about one-eighth the solar."^ The range
of variety in this respect among such stars is evidently very
con^derable ; but all appear to be less compact than our buq.
The circumstance is also noteworthy that eclipsing stars agree
in showing a Siriau or a helium spectrum. Nu exception to
the rule at least has yet come to our notice. The solar type,
on the other hand, predominates among ordinary short-period
variables. Variable stars of all classes are probably at
enormous distances — even on the celestial scale — from the
^arth. There is no sign that any of them are included among
le stars in our comparative vicinity. One of the best means
forming a rough judgment on this point is by the amount
of apparent motion ; and variables remain in general nearly
fixed in the sky, Mira, perhaps the most mobile, shifts its
po&ition indeed to the not wholly iuconaiderebla (jxteiit of
twenty-five seconds of arc in a century^ but measures for
parallax would be much embarrassed by its changes of magai-
.de, and have not yet been attempted. Dr. Chase'a deter-
ation of a distance for Algol ' about ten times that of
firiua is the only piece of direct information yet obtained as
to the remoteness of variable stars.
Their distribution over the sphere presents some noticeable
pectdiarities. Contrary to what might have been expected,
short-period variables^ although on tlie whole much brighter
objects than those of long period, tend much more decidedly
to concentration in the Milky Way, while Che preference for
' Maiven H*1l, Ob$ervfif<rnj, vol, ii. p. 22^.
* Attroph. Jtmm. tdL x. p. 316. =* Jhid. p. 30S. * AaCt. Jmim. No. 31B.
^^d(
^Bhin.
134
THE SYSTEM OF THE STABS
its plane belongs cbieSy to tadnt Btarfi amoDg those not van-
M&. In Algol 6tar9 it is lees strong than in periodical stars
of FicXering^B fourth class. These be, for the most part,
alo&g a gre&t circle nearly, but not quite coincident with the
medi&l tine of the gal^n'.^ It is remarkable that their cod-
densation-levei (as i& showa by its being projected into a ffreat
ciicle) pasaee thit^ugh the sun. Within the zone itself, there
is an evident disposition towards clnaterLag. Where the
Milky W*aj divides in Cyguufl, the variables follow ita southern
branch, and they are thickly sown over the whole sky-r^on
horn Lyra to Sagittarius.^ Indications abound that the con-
ditions of variability, and even of particular kinds of van-
ability, are localised in apace. Thus, in Sagittarios no lees
than four stars fluctuate in periods of six to seven days, and
many others are subject to slower or undetermined rioiflsitudes.
Two adjacent stars in the Southern Triangle vary in unusually
short periods. A small region near 17 Carini]& includes six
stars changeable in brightness.* Dr. Max Wolf has lately
puhliahed * a list of thirty - six variables grouped round
S AquiUe. The Orion nebula and the Magellanic Clouds are
veritable nests of fluctuating light-pointa. The new star
which appeared in Scorpio in 1860 marked the centre of a
group of nine or ten objects, all widely variable irregularly or
in long periods. Five stars of a similar nature, including two
virtually extinct Novxe, are collected in a small section of
Ophiuchua, and in general the sites of temporary stellar
apparitions are more or lesa closely dotted round with variables.
There is reason to suppose that the circumstances favouring
instability of light do not exist anywhere in the neighbour-
hood of the sun.
' Thfl northern pole of this oimle, according to Pickering, is sitnatod ia
E.A. lSh.,D«:. + 20'. Tliat of the Milky Tilay '» »a ^■■^- I2h 40m., Doc.+M".
* Chandler, Asir. Jottni. No. 103 ; riasiamami, Die ter&ndcrtii^ieu SUme, p. &5.
' Goto, ^Tnowltdge, vol. xiv. (i. 193. * Aitr. Naeh. No. i005.
stars differ obviously in colour. Three or four among
'the brightest strike the eye by their ^xlent glow^ others are
tinged with yellow, and the white light of several baa a
IMoiah gleam like that of polished steel. Keddinh tints are,
however, ia the few cases iu which they affect lucid stars,
^e most noticeable, and were the only oues remarked by the
ftncients.
Ptolemy designates as '* fiery red " (uTroKtppot) the following
Bix atars: Aldebaran, Arcturua, Betelgeux, Antares, Pollux,
and — mirah'Ue dictu — Sirioa ! all the rest being iudia-
criminately classed as " yellow " {^dv&oi'). Now Pollux at
present^ though by no means red, is at least yelLowiah, but
Sirius is undemably white with a cast of blue. A marked
change in its colour since the Alexandrian epoch thua appears
all but certain, the more so that Seneca makes express mention of
the dog-8tar as being " redder thau Mara." ' Horace baa " rubra
Canioula " as typical of the heat of summer,^ and Cioero, iu
his translation of Aratus, speaks of its " ruddy light." Sig-
nificant, too, in the same sense was the custom described by
the gramraarian Festus of sacrificing red dogs at the feast of
Bth« Floralia for the parpose of placating in the interests of
the approaching harve:at, the formidable and inimical dog-star.
The wliole auhjeet has been learnedly disciissed by Dr. See,^
who may be said to hare fairly established his contention
that the present white lustre of Sirius does not date back
more than a thousand or 1200 years. In the tenth century
1 QwBxl. Nat. I. L 3 Sat. ii. 6, 39.
' AaiTt and Axfrophytiw, voL ii» p. 269, etc.
1S6
136
THE SYSTEM OF THE STARS
the star was as^ui'edly no longer red. Al S^, 3
observer, pointedly omits it from the list of those excepi
coloured, while adding to it " Cot Hydrse " and Algol ^^ — Algol.
now a silvery orb, if there be one in the sky ; yet it ie worth
recording that Schmidt noticed the Perseus variable asyeUowiah
red in 1841, although he never in later years saw it otherwise
than white.*
The aame observer was amazed, March 21, 1852, to per-
ceive Arcturus without a trace of the Btroug colour familiar
to him in it during eleven previoua years. In comparisoii
with its paleness, Capella seemed bright yellowj Mara and
Betelgeux glowed almost like fire.^ It was some years before
the star resinned its original hue, and the reality of the
change, admitted by Argelander, was certified by the obeerv*-
tiona of Kaiser at Leyden.''
The periodical variations in colour of a Utsjb Ma}
the "Pointer" nejtt the pole, announced by Klein in 186'
were long tliabelieved in. Nevertheless, a aeries of obsej
tions with ZoUuer's polarising cotorimeter, executed in 181
by M. Kovesligethy, of the O Gyalla observatory in Hun]
gave evidence of alternating fluctuations between red
yellow in a period of 54^ days;*^ and essentially confirmai
results have recently been obtained by MM. Lau
Wirtz,^
The colours of the stars visible to the naked eye are f?
and pale compared with those disclosed by the telescope.
The real gems of the sky are found low down in the scale
of brightness. To some extent this is only what might
be expected- Intense tints result from strong Belective
abaorption in the atmospheres of the stars they distiuguieh,
and strong absorption impUea large loss of light. Stars shine
witli the rays that have sxirvived transmission tlu^ough the
glowing vapours in their neighbourhoodt and the more
nearly those rays are limited to one particular part of
* Schjellwup, Deaeription dei £tifiUi FitseSt p. 25.
" Astr. Nach. Ko. 10&9,
3 Ibid. No. &99,
' De Sterreniiemel verklaart, Ft. L p. 597.
" Afir. Nach. Nob. 1663, 2131.
" Siriu*, Bd. lir. p. 253.
^ Jahrlmeh der AslrmtanUfSj lid. liv. p. 135.
THE COLOURS OF THE STABS
137
rspectrum, the pmer and clearer the resulting tint will be.
A true prismatic hue could accordingly be produced only
through a vast reduction of brightness; but true prismatic
hues do not exist among the stars,^ the colours of which
aie always more or less copiously diluted vdth white light.
The science of stat'Coloiu's has hitherto made little
pipgiest^. Attempts to set up a standard chromatic scale
h&ve not been successful,^ and instrumental devit-ea for ensur-
ing just and equable judgments may sometimes induoe larger
erroTfi than they avert.^ Simple visual estimations} on the
other hand, must be treated with great reserve, since " personal
equation " in this matter often assumes enoi-mous proportions.
llie extreme of colour-bUndnese is reached by comparatively
few, but endless minor individuaUties of perception vitiate the
greater part of an accumulated mass of evidence which might
otherwise justify inferences of real change. From the com-
plex bundle of raya forming the image of a star, each retina
picks out and accentuates those to which it is most highly
sensitive, precluding the possibility of ^reement aa to delicate
tints between many different observers. With both the
Herschela, for instance, the equilibrium of colour was shifted
towards the red end of the spectrum. Struve's assistant,
Knorre, saw all stars indiscriminately white ; Admiral Smyth,
on the contrary, discjiminated between shades of colour alto-
gether inappreciable to most of those who hav6 profited by
his " Cycle of Celestial Ohjecta."
Even of the same observer the impressions do not always
agree. Fatigue and advancing years modiliy the colour-
sense ; and M. Safarik stated that stars invariably appeared
redder to his left than to his right eye.'* Atraaspheric condi-
tions* toOf are powerfully operative. Misty air blots out faint
tints and alters strong ones, azure visibly turning green
through its influence. Height above the horizon ia another
circumstance to be taken into account before any useful com-
pari^na can he made, while instrumental causes tend further
^ StriavB, Mensural JUicrotnelrictt, p, Ixiivi.
' See the system proiKised by FratLta, Monthly Notieu, vol. ilvii. p. 269.
' S«e the reaolti) giTon by Kijvoalii^othy, Ucber Hns neue Mtthodt der
FarheTifxetimmung cUr SlenKt H*J1g, 1^37.
* VisrUijahrasekri/t A^r. Qes. Jahrg. xjv. p, 378.
138
THE SYSTEM OF THE STABS
to perplex their npabot l^rge apertures help af theaiselves
to bring out colour/ espedallj in bihaU stora, bat the ooloor-
oorrection or groat re£ractors is always imperfect, ukd tlw
outHtanding blae fringe uaually conapicuoua in them roust bj
cunLntat give a retldiah coat to the image,' Baflectors produce
a aimilar effact through absorption of many of the higher rajs
by the silvered glass or apeculuni -metal fonning their mirtoa.
And since with high magnificat ion all hues merge, or ten<L to
merge, into yellow, only medium powers should he naed in
colour obserratioDA,
In this department then, di^repant statements by no
means necessarily imply actual variation. The former abound;
instances of the latter are met with, but can only be admitted
with extreme caution.
The study of star-colours divides naturally into two
bmnchea — one concerned with isolated, the other with com-
pound obJBcte. Inq^uiriea in the first case are simplified by
the curious and unexplained fact that elngle stars are never
markedly tingetl except with red or yellow, Vega makes the
nearest appruitch in the northern hemisphere to an independ-
ently blue star ; 7 Toucanse, a Eridani, and e Pavonia are
the " pale siipphires " of the southern sky. But they are very
pale indeed — so pale as to produce no definite impression of
colour upon ordinary eyes. Nor is the " emerald " tinge of
^ Librre much more decided. We have accordingly to deal
juat at present only with " red stars."
The earliest lint of thirty-three of them was drawn up by
I^lande in 1805." '* Ces dtoiles " von Zach remarked in re-
publishing it in 1822, "anncnceut toujoure quelque choae de
particulier ; or toute particularity merits d'etre obeerv^e." *
We have to a great extent got rid of the notion which pre-
sented itself to John Michell in 1767^^ that what they
"announce" is the impending extinction of their own fires;
but their pecuUarities have l>ecome, on that very account, all
the more worthy of attention. Eed stars are commonly
variable both in light and colour ; the display of colonnaded
1 StrnTe^ Jtf^Hfl. Mieri>mr. p. Ixxxiri, Mr. Frnoks held thfi oppEisite opiitioD.
» Webb, Studeni, vt>L v, p. 487.
• Connoisaanee des Ttmt pour Van 1808.
* Corratp, Astr, t. vii. p. 295. * PhiL Trans, vol. Ivii. p. 38A.
THE COLOURS OF THE STARS
139
zoned spectra belongA exclusively to them \ and they are
jiiently characterised by atmospheric incand^cence as well
by atmospheric instability. Few of them can be watched
and attentively without being caught in some singular
of change.
Their systeToatic study began with the publication in
1866 of SGhjellerup's Catalogue of 280 red stars ;^ ten
years later, Mr. Birmiugham of Tuam completed a eimilar
work compiisittg 658 entries,' and Mr. Chambers laid before
the Koyal Astronomical Society, April 6, IBS 7, a catalogue
founded on his personal observations during seventeen years."
Of V H nominally red stars in both hemispheres he had
examined 5 &9| being virtually all those visible in England}
with the result of finding the colour of most exaggerated.
" Orange" was to his eye the tint prevailing among them ; true
" reda " were scarce ; of stars meriting to be qualified ae
" carmine " or '* ruby " he had not met above a dozen.
More recent works of the kind have their value enhauced
by spectroscopic indications. Such were added in 1888 to
Sir. Espin'a edition of Birmingham's Hed Stars, augmented to
the number of 1472, and to Kriiger'a Catalog der Fdrhigen
Stfrn€ (Kiel, 1893), whicli includes 2153 more or less deeply-
tinted objects.
None present saturated colours. The perfect crimson of a
solar prominence cannot be matched among the stars. Their
hues result from atmosphenc action, and stellar atmospheres
are only partially effective in lifting the prismatic rays^ Eed
fitars are none the less striking telescopic objects. Their light,
even in the less distinguished speciinens, hafi a lurid glow
which at once marks them out from ordinary stars, and those
deeper tints shine with an ardour recalling the wrathful
itensity of a stormy eunaet. The contrast between a red and
a whtte star in the same field of view is sometimes most
viTid and beautifuL Thus, in the southern constellatiou
Grus, 71^ and tt* show like little burnished discs of capper and
silver respectivelyj seen under strong illumination.
■^ ^ Astr. Nach. No. 1591 ; reprintad with nuraftroua udditiona in VurUljahrs-
tehrift Attr. Qta. Jalirg. ix, p, 253.
* Memffiri It. Irish Acad, vol, xxvi. p. 249.
* Mpntkljf Notices, toL xlrii. p. S48.
140
THE SYSTEM OF THE STABS
Among odnFpicuoua stara, Antaree, in tba heart of the
Scorpion, is the ruddiest, Betelgeux comes next ; while Alde-
l^j&u and Arctunzs have figured isimemorially in th« short
list of visible fiery objects, to which Al Sftfi (as alieadj mat^
tioned) added a Hydrse. aud Father 'Soij-X y Cruds. But their
colouis are mere pale shades compared with those inatni-
meutallj brought into notice. '* Hiod'a criniBOa star" oihss-
wise knowTi aa R Leporis, appeared to ita diaeoverer in
1845 like " a drop of blood on a black field.'' As with most
other variables, however, increaee of light brings with it a
paling of colour. Near maximum, intense redneea givee place,
partly through a well -known phygiological effect/ to a ooppefy
hue. Its spectrum is of the fourth type, with particularly strong
absorption of the blue rays, a very small proportion of which
pfiuetrate ita dense veil of carbonaceous vapours.
A similar objet-t, now known as V Hydne, is No. 16 of
Lalande's, Ko. 136 of Schjellerup's Red Stars, and was re-
cord^ by Dr. Oopelaud at Dunsiok, March 32, 1876, ftS
" browu red," and of 7 '2 magnitude.* But three years later,
Dr. I>reyer found it risen to the gixth magnitude, and of a
" most magnLficent copper red," while Birmingham observed it
in 1874 as of the eighth, Duult in 18S4» as faded to S'S
magnitude. Ita fluctuations of light are comprised in a
nominal period of 575 days.
Close to one of the gems of the Southern Cross, an eighth-
magnitude star wag described by Sir John Herecbel to be of " the
folleet and deepest maroon red^ the most intense blood-red of
any star I have seen. It is like a drop of blood when con-
trasted with the whiteness of ^ Cnicis." * Among other
wuthem stars remarkable for colour are E Sculptoris, no
less "intensely scarlet" now than when Gould saw it nb Cor-
doba, R Doradi^s, glowing like a live coal out of the darkneaa
of space, and Lj Puppis, all of them noted variables.
In the northern hemisphere, V Cjgni bears the palm for
deptli of tint, especially as its light diminishes ; and not far
inferior to it are K CassiopeifB, R Leonis, R Crateris^ and
Mira, with U Cygni and U Caseiopcite, both splendidly 8et oif
1 Oflthoff, Aair, Kf7ck. No. 3910.
* Duntink Olacrvationa, vaL iv. p. 55.
* Capt Oiuervati<m$j p. 4*6.
THE COLOURS OF THE STARS
141
by the vicinity of blue attendants. Crimgon, indeed^ vergeB,
in these and other periodical starSf more and more towards
orange in their brightening phases, yet they remain pretty
constantly " red." A few casea of complete if temporary
change of colour have, however, been recorded. Thus, a
seventh-magnitude atnr in the Lynx (90 Schjellerup) noted
by Stritve as " rubra," by Secchi as " bella giaUa/' seemed to
Birmingham, January 13, 18*74, blue or bluish white, a con-
firmatoi-y and nearly cantemporaneous observation being made
&t Greenwich.* A star of 8^ magnitude (148 Sclijellerup)
called "scarlet" by Lord Eosae in 1861, "dark red" by
d'Arreat, December 8, 1866, showed " uo colour" to Birming-
ham, May 8, 1874, Dun^r found it, nevertheless, of a deep
orange red in 1884, and it is characterised by a fine colon-
naded spectrum. Again, Schjellerup was struck with the
redness of a star in Aquila^ in 1863, which, after an interval
of ten years, struck Birmingham as actually blue ; and
similarly a bluiBh-white object occupied the place. November
14, 1850, of a atar in Taurus (Schjellerup, 64 i) marked
" very red " by Hind, September 3, 1848,* which Dreyer per-
ceived as once more red in January 18T9» but Espin as white
with a continuous spectrum, January 10, 18BS. One further
instance may be mentioned. A fifth-magnitude atar in Argo,
known as r Velorum,^ was natorioualy red during Gould's stay
at Cordoba. But. !t seemed leaden white to the present
writer in the antumn of 1888, and was observed by Mr.
Tebbutt in March 1891 as barely tinged with red* Chough the
tinge became more decided on substituting an 8 -inch for a
4i-iDch equatoreal. The spectrum of r Velorum closely
resembles that of Aldebaran.
The changes of colour visible in tempomry stars have
generally been in an opposite direction to those of ordinary
variables. Their sanguine tints faded, instead of deepening
with the decline of their light. Thus, Tyeho's atar, though
it passed through an intermediate stage of redness, was of a
leaden white when it disappeared. T Coronse ran nearly the
^ Mevwira S. Iriah Aead, voL situ p. 2B9.
* No, 6S03 or the CctpenAo^t Caialoijui ; No, 214 of Se^tlUrup'f Eed
Start.
' Jf<»UA/y Xotieta, tqL xi. p. 46,
« The plftce of the Bt»r for 1900 u E.A* 10* 18»'l, D-ll* 9'.
same course. Nova Ophiuchi (1848) and Nova Aiadros
were ruddy lit tirst, colourless later. Nova Cygni from orange^
turned bluish. The colour changes of Nova Persei were not
thtj least curious part of its history. Purely white at its
outburst, February 22, 1901, it rapidly fluBhed to a deep red.
whic'li lightened to orange during the spasms of intermittent
brightening observed in March and ApriL The steady decline
of the star was nevertheless accompanied by a progressive loss
of colour, until on February 5» 1902, it showed to Frofesaar
Barnard greenish -white, like Neptune.^ Its nebular spectrum
was by that time fully developed ; but its antecedent redness
was unaccounted for by any marked absorption iii the blue or
green. Nova Geminorum similarly glowed vividly at first,
but blanched with the waning of its sudden access of ligbt
In its ease, however^ the predominance of red hydrogen in ita
emissions explained the initial ruddiness of its hue. Professor
Barnartl * was able, by suitably drawing out the eye-piece of
the YiTkea 40-iuch refractor, to form on the C-line a crimaoD
image of the star as purely tinted as a solar prominence;
This is the only ascertained instance of the production of
stellar colour by direct radiation instead of by complementary
absorption.
Red stars are very unequally scattered. Certain wide
tracts of the sky are nearly destitute of them; in some, they
oeour profusely. Tlie Milky Way between Aqnila, Lj-ra, and
Cyguna was called by Birmingham the " Red Beglon " ; * yet
other galactic consteUatious^ such as Perseus and Oa^opeia,
might be said, on a preliminaiy survey, to consist of white
atars.^
Evidently, however, real partialities of colour-distribution
must be to a great extent masked by the projection, to the
eye, of objects at indefinite distances from each other upon
the same portion of the sphere* Hence extensive loeal
eolloctions of similar stars may be so confused with overlying
tuid underlying aggregations as to be completely unrecognis-
fcble. Smaller groupings are more readily detected. It is by
* Uimthly Notiies, toL liiL p. 418.
■ A$trt!ph. Joum. ¥ol. irii. pp, 302, 376.
■ Mcmoira E. Jrixh Acad. va\. xxvL p. 26B,
* JVuika, Monthly Noticta, vol. xlvl p. 343 ; wtt ■icoOatholT, WfckcMehrift
/Ur Attr. Bd. xli. (1876) p. 328.
no accMetit that, in the immediate neighbourhood of one red
star» others are so apt to be met with; and the "brick red"
and " ruby " pairs included in Herschel's Cape list, may with
oonfidenoe be assumed to be severally in some sort of physical
coDoectioD. Red atarft, it was remarked by the same authority,
«re conspicuous in many clusters both by brightness and
situatiou ; and Father Seccbi wae etmck with the critical
positions of euch objects as regards spiral or radiated stellar
anangements in the Milky "Way.^
The principle of colour by association, barely indicated in
clusters* is in double stars carried out to the higb^t perfec-
tion. Kature is inexhaustible in her display among them of
harmonies, contrasts, and delicate gradations of hue. They
not only vividly sparkle in green and gold, azure and crimsoa,
but shine in the sober radiance of fawn and olive, lilaCj deep
purple, and ashen grey. Chalcedony, aquamarine, chrysolite,
agate, and onyx have counterparts in the heavens as well as
^mbies and emeralds, sards, sapphirea^ and topazes.
B Mariotte of Dijon, a physicist, but no astronomer, was the
vast to speak of blue stars. "Les ^toiles qui paraissent
blauefi/' he wrote in 1681, "out une lumi^re faible, maia
pure et sans melange d'exhalaisons." * But he gave no
examples, and it is not easy to divine what class of objects he
alluded bo. The chromatic observation of double stars was
really begun by Father Christian Mayer at Mannheim in
1776; although the interest of his preliminary efforts wag
absorbed in the splendour of Herschers similar but vastly
more extenaive and assured results. He not only discovered a
great number of exquisitely tinted couples, but by liia success
emphasised the importance of systematic attention to colour in
double stars.
His example was followed by F. G* W. Struve, who in
1837 clasaified from this point of view 596 of the brightest
known stellar pairs. The upshot was to prove agreement in
colour the tulo, contrast the exception.^ Just half, or 295 of
the objects examined were uniformly white ; 118 had both
components yellow or reddish with slight differeucea of
' AUi dei Nvovi Xinc«i', t. Til. p. 72-
* Oetivret, t. i. p. 287.
' £Ml«a Doi^h*, pp. 33-34 ; Aftnsura Mierouu p. Ixxxii.
144
THE SYSTEM OF THE STAKS
intensity ; sixty - three were tinctured with blue. The
iustances of getiuioe contrast nuinbered 120, and in aii of
these the Bmall star was called blue. The rule is, moreover,
without exception^ that no prLmary member of a disaimiltirly
tinted pair is blue.
The reality of chromatic contrasts in double stars was
established by the persistence of colour in satellites during the
obliteration of their primaries by an interposed wire or bar;
and besides^ as Struve remarked, optically produced huee
should be invariably complementary, which is far from being
the case in stars. A curious proof of this independence was
afforded by a double occultation of Autares and its coijnpSLaion
observed by Dawes in 1856, The small star, emerging first
from behind the moon, seemed as perfectly green viewed thns
alone as when half lost In the glare of the great red star ii
is attached to.' The same phenomenon was reobsorved in
1SY8.
The connection between inequality of brightneaa and un-
litenesB of tint in coupled stars did not escape Struve's notice.'
He found a mean difference of less than half a magnitude
between the exactly similar members of 375 pairs, of over
one magnitude for 101 etara showing varied shades of the
same colour, and of nearly two magnitudes in 120 cases
of contrasted tints. Professor Holden, taking account of
physical pairs only, reached, in 1880j an analogous rseulb'
Where there was identity of colour the average difference of
lustre proved to be only half a magnitude, where there was
diversity the luminous inequality mounted to two and a half
magnitudes. One hundred and twenty-two of the stars con-
sidered belonged to the first class, forty to the second. Now
markedly unequal are generally wide pairs^* so that disparity
of hue is seen to prevail in systems formed by a large star and
a comparatively small and remote companion ; while genuine
twin suns^ of not very different radiative power, and of
similar radiative quality, circulate as a rule rapidly and closely
^ Monthiy Notices, toI. X¥i. p. 113 ; Ntesten, del et Terre, t. ii. p, 96 ;
Webb, C«/, ObjedSt p. 389.
' jfmt, Jfiei-uwi. p, IsTtiiL
' Aintr. jQvm. o/Seiena, rgj, lix p. 467.
* Doberck, Astr^ J^ack. No. 2276. The Bc&rclty of dBiiilU cloae companioua
to bright sUri tuay be partly due to the dilEctilty of dtacoranug them.
J
THE COLOURS OF THE STARS
145
yd their common centte of gravity. Why this is so we
lot tell ; the bare fact is before ua.
Some beauMfullj coloured stars are, nevertheless, ascer-
led to bti in mutual revolution. The yellow and rose-red
mpobents of 7} CaaaiopeiEe Sni&h their circuit in about two
idred yeiira; those of e Bootis, chrome yellow and sea-water
blue, in probably upwarda of twelve hundred ; f Bootis and
y Cepbei, orange and purple, o Cephei and t Cygni, golden
and azmie pairs, are all in swifter or slower orbital movement.
A good many richly-tinted stars, on the other hand, appear
atationary, doubtless because their diietancea apart are so con-
sidexable ^ to make thair revolutions inordinately slow.
TbtiB the emerald-green companion of a Herculis has preaerved,
during a century, an invariable position with regard to the
ruddy star it depends upon, and Antares forms with its sea-
green satellite a somewhat similar and equally rigid combiua-
tion- The fixed pair j3 Cygni (Albireo) shining with "yellow
topaz " and " aquaccelestia blue " light, presents perhaps the
most lovely effect of colour in the heavens, nearly matched^
however, by the variable S Cephei and its ccerulean companion.
Among numerous other examples of contrasted or harmonising
tints in double stars may be mentioned y Androraedse, orange
and green ; 7 Delphinij yellow and pale emerald ; ij Persei,
golden and azure ; 24 Comae Berenices, orange and lilac; 12
Canum Venaticorum, pale yellow and fawn ; v Serpentis, sea-
green and lilac; a pair in Cassiopeia (S 163), copper colour
and blue; 17 Virginis, light rose and duaky red; o Draconia^
or&nge and emerald. A few red and green pairs seem
abnormal through the near approach to equality in the
roagoitudea of the components. One such was observed by
Herschel in Pisces; and Burnham noted in 1900 the reality
of the contrasted tint it presents.^ Another wag discovered
by Burnham himself in Pisces, But the fiery primaries are,
in both cases, likely to prove variable.
Bright white stars have not unfrequently small blue ones
in their vicinity. A distant companion of Eegulus seems as
if steeped in indigo ; Higel has an azure attendant ; \ Gemi-
noium one of an amethyatine shade; 84 Ceti and 62 Eridani
made up each of a white and a Ulac star; while the
' Mniaurt$ of DoithU Stan, p. 10.
146
THE SYSTEM OF THE STAKS
sapphire t Bootis La grouped closely with one, more loosely
with two olht-r subordinate blue objeots,*
Two questions at oncij suggest themselvea about the
colour* of double stare. To the first, Are they real ? a
decisively affirmative answer can be given ; but the second,
Are they permanent ? cannot be dispoeed of with 8«ch
promptitude. The subtlety of hues reBulting from a highly
complex set of retinal iuipresaions renders thera peculiarly
liable to subjective variation. As evidence of ohJecH've vaiia^
tion, then, mndom notes of colour ace of little or no uee.
Only the estimates of skilled observers, trained to the needfiil
precautions, furnished with suitable instnuuenta, above all,
owning normal eyesight, are worth weighing and comparing.
Under this rule of exclusiveness, the testimony requiring the
admission of real change eliriuks surprisingly in compass, but
does not whoUy disappear. Colour-vaidablee are to be found
among compound, no lees than among single stars.
Owing partly to instrumental, partly to personal causes,
the elder Struve perceived as purely white many stars seen
by Herechel with a tinge of red or yellow. Disagreemeata in
the opposite direction merit, then, particular attention, and
they are especially mai-ked in two cases,^ The components of
the splendid couple y I^ouis were described by Herschel in
1784 aa both white, the smaller inclining slightly to pale r«d*
But Struve saw them in 1837 golden yellow and "reddish"
green ; Admiral Smyth " bright orange and greenish yellow";
and strongly, though unequally yellow, they still I'emain,
Here then we have a presumption of genuine change, which,
in the companion instance of y Delphini, is raised almost to
certainty. Thcae last stars, noted by Herschel in 1779 as
both perfectly white, showed golden yellow and bluish green
to Struve's scrutiny. The progress of alteration may perhaps
be marked by the younger Herschel'a and South*a record of
them as white and yellowish in 1824.* Their dissimilar tints
of orange and green now strike the eye at the first glance with
the smallest telescope.''
' Fl*mm&rion, Catalogue des ^toila Dvubles, p. 76.
■ MlensuTie Mierom, p. IjEwvii.
t* Phil TruTis. vol. Ixxv. p. 48. • Ibid, vol, ciiv. p. SftS.
* NoblC| Hourt with a ThrU'ituh T«li$cope, p. Ill; Fi&x)It8, Jvum^ Brit,
Aatr. Au, voL v, p. 4&7.
THE COLOURS OJ THE STARS
147
Another pair famoas fqr colour-fluctaationB is 95 Herculis^
composed of tw<j equal Btars of 5^ magnitude^ ptatiM (to
appearance) immovabljr within 6" of each other. Familiar
with them as nvidly lioted objects, Professor Vl&zzi Smyth
waa astonished^ on pointing his telescope towards them from
the Peak of Teneriffe, July 29, 1856, to perceive them l>oth
white.' In the following year, nevertheless, they shone as
before in " apple green and cherry red " and were bo observed
by Admiral Smyth, Dawes, and others. Captain Higgens *
actually watched these colours fade and revive in 1362-63,
in the course of about a year; but no trace of them has
been seen of late; the stars of 95 Herculis are now of an
identical palish yellow.' Their spectra are not identical.
Dr. Vogel, in 1899, classed one as solar, the other as Sirian
in type. The history of these stars goes back to 1730, when
Herschel observed them as bluish white and white ; J. Her-
schel and South called them " bluish white and reddish " in
1824 ; Struve, 1828-32, greenish yellow and reddish yellow, in
precise agreement with Pickering's appraisement in 1878.*
Thus the " magnificent tints of orange and green " which
Secchi admired in 1855, and Piazzi Smyth missed in 1856,
were of a transitory chai^eter.
In the well-known binaiy, 70 Ophiuehi, there has been an
equally undoubted change. Except an " inclination to ted " in
the smaller, the elder Herschel perceived no colour in either
of these stars ; his son and Sir James South called them white
and " livid " ; yet they were recorded by Struve as of an espe-
cially intense yellow and purple, by Admiral Smyth as " pale
topaz and violet." They are now both yellow» very much as
they were seen by Secchi in 1S55, and by Franks in 1876 ;
the companion was, nevertheless, marked " purplieh " at
Harvard College in 1878i "rose-coloured" by Flammarion in
<!79.
i The three stars of f Cancri are usually yellow, but Dem-
waki noticed them as all white, 1854-56, the remoter
component turning yellowish or olive in 1864-65.^ This form
of concordant change through various shades of primrose or
' 8myth^ Sidtreal Chramotia, pp. 35, 76. * Ihid. p. flO,
]* Koble, Op. cit. p. 10&. * Harvard Annaht vol. xi. p. 150.
• AftK Nadi. Noa. lUO, 1674.
148
THE SYSTEM OF THE STAES
cowslip is not very rate amoDg revolving stars, while ll
devdopmeiit of colour la othex pairs teads towards
production of ooDtrast. It ofteii huppena, too, that
component only varies iu hue, in which case the change ed-
^ectB the Batellite star. The attendant, for example, of
H«rcxdis has appeared by turns ashen, " grape-red," blue, and
bluiah-green ; that of B Cygai was observed by Struve iig grey
in 1826-1833, but conspicuously red in 1836, blue by Dawes
in 1839-1841^ alternately red, blue, and violet by Secchi is
1856-57, grey once more by Denibowaki in 1862-63, red bj
Engehnann in 1865, aince when it has commonly seemed
light blue.* Again, the multiple star <r Oriouis includes two
if not three colour-variables ; the distant companion of 7
Leporis changed from pale green in 1S32 to garnet in 1861
and 1874. and the satellite of p Serpentia from lilac in 1332
to "native copper" in 1851.^
Eye - estimates of colour do not reach below the
surface ; they are mere indiqatiousj which the spectroscope
and the spectrograph can alone help us to interpret. But the
task is delicate for the eye. and until of late, was impossible
for the camera of discriminating the varieties in quality of
closely adjacent light-sources. Miss Maury managed^ never-
theless, to pick out on the Draper Memorial plates eighteen
" composite " spectra, in which the characters were so mixed
as to suggest a twofold origin ; * and her acumen has been
vindicated by the spectroscopic resolution of several of these
dubious objects into swiftly-revolving, unlike couples. Exact
determinations of the kind, however, were rendered possible
only through Sir William Huggins'a invention of a " reOecting
slit/' by means of which the spectra of stars no more than 2"
apart can be separately photograplied.* Successful impressions
were thus obtained from y Leonis, Cor Caroli (12 Canum
Venaticorum), and Cygni. Fnam previous observations of
the last- mentioned pair with a visual spectroscope, he had
found their complementary colours explicable (wholly or
in part) by complementary absorption ; * but this was not
' Eng«lm»]m, Asir. Xaeh. No. 1676.
» aroyth, Sid, Okromatia, p. 2fl ; Webb, Cet. Ohjeeit, p. 3&0.
^ Rarvatd AjiTiaU, vol. xxriii, p. 92.
* CifrnpUf Jievdv-t, Oct. 11, 1SB7 ; Aatropkys, Jov>rn. voL vi p. 824.
■ fhH. Tr&nt. vol. cUt. p, 431.
THE COLOURS OF THE STARS 149
tible in the more re&angible sections of their dispersed
photographed by himself and Lady Huggins in 1897.^
ue star yielded a Sirian, the yellow star a solar spectrum,
of perfectly normal quality. Their exceptional tints
• to be reserved for visual explanation.
it the improvement of methods has brought within view
alisation of the chief desiderata in stellar chromatic&
are, first, the definite correlation of the integral effect to
re with the analytical data furnished by the prism;
ly, the recognition of some fixed mode of correspond-
etween spectral and colour-variations. The foundations
len have been laid of a true science of stellar chromatics.
^ Atlas o/SUllar Spectra, pp. 168, 163.
I
A DOUBL£ Star is oue that divides into tvo with the help of a
more or leas powerful telescope. The effect ia a strange, and
might have appeared beforehand a most unlikely one. Yet it
is of quite ordinary occurrenca Double stars aiie no fre$k
of nature, but part of her settled plan ; or rather^ they enter
systematically into the design of the Mind which is in uid
above nature.
The fii'St recognised specimen of the class was ^ Uraae
Majoria, the middle " horse " of the Plough, called by the
Arabs " Mizar/' which Riccioli found at Bologaa, in 1650^ to
consist of a 2^ and a 4 magnitude star within foiirtees
aeconda of arc of each other. Both are white, and they
make a radiant dJaplay even in a very small telescope. The
accident of a bright comet observed by Robert Hooke passiiig.
on February 8, 1665, close to y Arietta ('* Mesarthini ") led to
his diecovery of its duplex nature. The components, each of
the fourth magnitude, and eight seconds apart, are perfectly
alike both in li^ht and colour. Meanwhile Huygens had, in
1656, seen $ Ononis to be triple — it disclosed itself as
quadruple in 16S4; a Crucis, in the southern hemisphere,
was divided by some Jesuit missionaries sent by Louis XIV.
to Siam in 1685, and a Centauri by Eichaud at Pondicberry
in 1689 ; making in all five double stars detected during the
seventeenth ceutur)*. Four more — 7 Virginia, Castor, 61
Cygni, and ^ Gygni^ — were taken note of by Bradley before
1765 J and in 1776, Father Christian Mayer began at
Mannheim a deliberate search for stellar couples. His thirt]
i&a
DOUBLE STABS
151
three di^coveriea in two years might be de^Hhed as the
prelimiDary washings from the rich lode atmck a few months
later by Sir William HerscheU
The plentifulnees of double &tars was in itself an iire-
fiistible argument for tbeir reality. That any two unconnected
bright stars should be projected closely side by side upon the
sphere was improbable; that such a eoutingency could be
repeated hundreds of times was what no sane man ought
to have been capable of beUeving. But human credulity is
nowhere more conepicuous than in what it is prepared to
attribute to chance ; and it needed such clear evidence of
mutually circling movements as Herschel was able to produce
in 1803 to establish the conviction of the "physiccU existenoe
of double stars-
The fact is one at which we can never cease to wonder. It
brings US face to face with a state of things entirely unfamiliar,
and of which the purpose lies beyond the scope of our limited
underatandinga. So accustomed are we to the " sole dominion "
of our own great star, that the presence of two suns in one
sphere might well at first sight appear incredible. Yet there
are many things " undreamt of in our philosophy " which are
uevertheless true. Every drop of stagaant water is a world of
uninterpreted mysteries ; what we choose to call the " order of
nature " is violated at every instant, inexplicably, by our own
volition ; and if that order be attended by anomalies upon the
earthy how much less shall we veoture to prescribe its course
in the heavens ?
The term " double star " is obviously quite indefinite^ apart
from some agreement as to its meaning ; and it was in fact
used by early observers in a far wider sense than it is now
usually considered to bear. Many of the small and remote
attendants upon brighter stars recorded by the Herschels
could scarcely be presumed to have any real connection with
them ; 3 2" was fixed by Struve as the maximum interval be-
tween the components of a genuine double star^ or 16", tuiless
both were britj;hter than the ninth magnitude ] the younger
Struve'a " Pulkowa Catalogue " included no at-ars beyond the
narrower limits and Mr. Biirnham rejects oil pairs below the
eighth magnitude above 5" apart. This progressive restriction
' See the writer's History of Astronomy, p. 18, 4th ed.
152
THE SYSTEM OF THE STAES
has almost necessarily accompanied the improvement
telescopes. With the powerfii! and perfect refractors now in
use, really close pairs accumulate faater than thej can con-
tinue to be obfserved ; and the t'ollectton of the innimieraUe
loosely yoked and ill-assorted couples they fuitber reveal would
be inane waate of time.
Already above twelve thoueand double stars, in the Her-
Bchelian sense, have been registered^ of ivhich some six
thousand correspond, by the closeness of their combination,
to strict ideas of what a double star should be; about 1400
are separated by 2" or less, and between 600 and 700 are
visibly revolving. These laat interesting cases multiply jusfe
now with especial rapidity. They are most apt to occur, as
might be expected, among those etars at the smallest apparent
distances &om each other, and requiring accordingly the
highest optical powers for their detection. Our acquaintance
with most of these ia so recent that their movements are only
coming to be recognised as one pair aftet another is re-
measured after a few years' interval
The singular profusion with which stars are planted sideh^
side with a bare hairhreadtk of sky between, became manifest
through Mr Burnham'a discoveries made at Chicago, 1871 to
1879. while he still pursued the profession of a stenograpber.
His thousand new pairs included 743 at an average distance
of l"'58.^ This means that the total interval from centre to
centre of these objects was just equal to the width of a human
hair held thirty-si^ feet from the eye. About oue-tentb of
that distance is the minimum at which, even with the great
Lick telescope, stars can be divided, but by no means the
minimum at which they can separately exist The spectro-
scope has demonstrated what it was logical to infer, that
numberless stars which must always, either through their
distance from ourselves or the closeness of their companions,
remain optically single, are nevertheless compound ; hence
of any given star, as of a chemical " element/' we can say,
not that it ia indivisible, but only that it has never been
divided.
Such stellar pairs as are known to be in orbital move-
ment are called " binary stare," to aigniiy that they form real
1 JftmotV* it. Atti". Soe. vol. iItIL p^ ai7.
J
DOUBLE STABS
153
al aystpems. The finest specimen qf this kind in the
northern heavens is Castor, or a Geniinomm, composed of
a second and a third magnitude star 5"' 18 ap^rt. They are
both white with a greeniah tinge, and can be divided with a
very modeiate telescope, so that the sight of this brilliant
and suggestive object is not reserved for the inner circle of
astronomera. Now it happens that Bradley observed the
relative eitttation of these stars in 1719, and the comparison
of hifi record with measures of tlie present day shows that
they have shifted in the interim to the extent of ISI"", or
ooaaiderably more than a third of a revolution. To complete
an entire one they would need at the same rate about 500
years. But they are likely to advance upon it. The moat
trustworthy orbit yet computed fixes their period at 347
years ;^ and although their movements have, in the past,
falsified many prediotionSj each sTiccessive investi^tor is in a
better position, because commanding a wider range of data
than hi* predeceBsors. The limits of uncertainty as regards
time of circulation shrink of themselves with every decade
that goes by.
The brightest ia ^o the widest pair of revolving stara in
the sky, and a third distinction — that of being nearer to ua
than any other known sidereal object — accounts for the first
two. In a Centauri are combined two stars so brilliant that
the lesser, though emitting only one-third as much light aa
ite neighbour, ia still somewhat above the second rank. It
ia of a deeper yellow than the primary star^ and must have
gained considerably in lustre during the last century unless
FeuiU^, Lacaille, Brisbane, and Bunlop all erred egregioualy
in calling it of fourth magnitude.^ Since they were observed
by the Franciscan monk, Louis FeuUlde, at Lima in 1709,
these stars have executed nearly two and a half revolutions.
Tliey traverse in eigbty-one years' an orbit about as much
elongated ae that in which Faye's comet travels round the
sun, and diverge, accordingly^ at '* apastron " to more than
thric-e their "periaatron" distance. They are now 22" apart,
and are separating fast, having in 187^ awept through their
■ Dobenk, ^j^r. Nac^t. No. 3070.
^ Seft flutamario^n'jj Ga-idtogiu, p. 81.
' T. J, J, See, ExxliUi&ti o/ihe StcUar Si^«(«™, p, 14S.
154
THE SYSTEM OF THE STAES
point of nearest approach. Th^ " mean radius/* or half tbe
Duyor axis of tbe c-ooiputed ellii^e, if seen square from tbe
tvtfa, would siibt^ud an angle of IV^'7, corresponding at the
star's distance of twenty-five biUiou miles to an actual spui
of (in roaud numbers) 2100 million milea; so that them
lustrous globes are sometimes almost aa close together as
Saturn is to the aun^ then, after two-^score years, at IJ timw
the distance of Neptune; Their mosa ia just twice, their light
about Ij times that of the sun.
The spectacle is beyond doubt amazing of two such
bodies united tbua organically into a single stately system.
That it includes many other members xxmj be taken for
granted, although we may never succeed in observing them,
and are unable, even in imagination, to bestow or arrange
them satisfactorily. Evidently, no planetary scheme or schemes
at all resembling our own can depend upon the stars of
a Centaim, A Mercury or a Vulcan, at the most, might
Gad shelter in the close vicinity of one from tbe dis-
turbing power of the other, its poBaible inhabitants enjoying
the combined or alternating radiance of a greater and a lesser
8un- Comets entering these predncta must be perplexed to
decide betweeu the two potentates claiming their allegiance,
and perhaps on occasions pay their court to each in tiuna,
throwing out tails, as they do so, of a highly anomalous
character. It has, however, been suggested that tbe clienta of
double stars circulate about both simultaneously, in orbits wide
enough to keep them beyond the reach of dangerous pertur-
bations from either. This is, of course, conceivable, if for
many reasons unlikely ; but the aurmiee can neither be verified
nor disproved.
The stars of 61 Cygni. like those of a Oentauri, share a
rapid onward movement through space They resemble them
too in spectrum and colour, and are counted among our nearest
stellar neighboura. Yet they are inconspicuous, one falling
short of the fifth,' the other of the sixth magnitude.
Although they have been under continuous ecrutiny since
1753, when Bradley noted the differences in their times of
transit, it is only within the last few years that the curvature
of their path haa become perceptible. Besides the forward
movement possessed in common by the two, the smaller alao
J
DOUBLE STARS
155
I
I
lifts its place senfiibly aa regards the larger star. But for b
lentury and upward the shiftiug appeared to take place along
straight line. If this had really been the case, the fact
3uld have aboUflhed the presumption of their binary char-
Facter, and compelled the belief, which was adopted by Captain
[Jacob in 1858/ and maintained so lately as 1891 by Mr.
Bombam,^ that the etars would eventually part company
and cease to have even an apparent connectioiu This, we
can now see clearly, was a false alarm. They are really
inaeparable ; although the circumstances of their revolution
must long remain unknown. Moreover, Dr. Wilaing'a an-
notincement in 139^^ that the motion of one or both com-
ponents was disturbed by the attraction of inviaible attendants,
Icicks coulirmation.
The systems of 70 Ophinchi and jj Cassiopeiee have much
in common. The stara forming them show elmilar spectra
and (apart from incidental variations) similar colours. They
progress through space at about the same rate/ and both are at
neairly the same distance of twenty light years from the earth.
Both, too, have proved somewhat recalcitrant to computation.
The orbit of 70 Ophiuchi, more especially, though one of the
earliest experimented upou^ can still only be regarded as
approximately determined. The stars have hitherto so
persistently refused to keep to their predicted places that
Madler, Jacob, and Sir John Herschel suspected disturbance
by an invisible member of their system calculated by Dr. See
in 1895* to revolve in a period of thirty-six years. The
bright companion, on this view, de8cril>e3 in eighty-eight years
an eccentric orbit with a major axis slightly less than that of
Neptune, while simultaneously tracing out, in thlrty-six years,
•' another ellipae, which in size considerably surpasses that of
the planet Mara." ^ Yet its vagaries of movement are not
even thus completely explicable. The mechanism of 70
Ophiuchi has still obscure springs.
The path of 13 Cassiopeia, traversed in 196 years (accord-
* Etit'jthurffh Hev} Phil, Joum, vol. vii. p, 107,
3 Aalr. Nach. No. 8047.
* Sii3U7tffsberichte^ Berlin, October 26, 1393,
* Sftdler, En^luh JfteJutnic, vdIb. xM. p, 410 ; xUv. p. 322.
* Anfr. Joum. No. 383,
' T. J. J. a««, Stellar ^ysteioi, ft, 220.
:
166
THE SYSTEM OF THE STARS
ing to Dr. See'a elemeats), is of an ampler Bweep. Its mean
radius is fifty-throe times that of the terrestrial, oearlj twice
that of Nepfcuue'a orbit. The stars, nevertheless, at their
neareat approaches come within less than once and a half
times the distance of Uranus from the sun, and since thej
together contain more than four times the Bolar quantiiy
of matter, perturbations of no slight intensitj would at
aueh times affect their perhaps visionary trains of attend&at
bodies.
Laplace's conjecture that space might hold as many dark
as bright masses has received some countenance from Ihd
phenomena of double stars. For among them are reckoned
effects of the attraction of unseen upon the movements of
seen bodies, wliile in two cases the detection of an imperfectly
luminous object has, like the discovery of Neptune^ ensued
upon the theoretical indication of its place.
From the nature of the proper notion of Sinus, Bessel
inferred in 1844 that it did not travel alone. The line traced
out by it must, were it solitary, have been straight, whereas
it undulated markedly and regularly once in about half a
century. Revolution in that period round an obscure com-
panion was indicated j the elements of the hypothetical Sirian
system were computed by Peters and Anwers, and the precise
position of the Sirian Katellite was assigned by Safford la
September 1861. On January 31 following, it was found
juflt in the right spot by Aivan G. Clark, of Cambridgeport,
MaeeachuBetta.
The companion of Sirius is a dull yellow star of tenth
magnitude, almost lost in the glittering radiance of its great
neighbour. Their apparent distance having diminished from
10" in 1862 to 4" in 1890. it was then barely distinguishable
to Mr. Burnhnm with the 36-inch Lick refractor.^ For six
years it remained wholly invisible ; unseen it passed periastron
in 1894; but in November 1896 re-emerged in its predicted
place, and has since steadily followed the track laid down for
it. The elements assigned to the pair by Dr. O. Ix)hse in
1904* when it had performed all but 30** of an entire circuit,
may accordingly be accepted as authoritative.
The system brought to our notice is a very remarkable
' Aatr, iV^wft. TTo. 2884.. » Ibid, No. 3965,
^
DOUBLE STARS
157
■ one. Its chief member i& a body ertremely bright in pro-
portion to its mass ; its secondary member b a body abnormally
niassive proportionately to its light. Siriua shines like four
thouaand, it gravitates like two of its companions. There
must hence bfl an enormous disparity of temperature between
them, with a probably corresponding difference of mean density.
Yet they are presumabl)'' of contemporaneoua origin.
At the distance of Sirius (about fifty billion miles) the
sun would appear aa a star of the second magnitude. A
cioUection of tweuty-one auna would barely supply the
emissions of that brilliant orb, the attractive energy of which
is, nevertheless, little more than twice that goveniing the
solar system. The revolutions of its satellite are completed
in 50^ years at a mean distance twenty times that of tha
earth from the sun^ with e^^cursions, at apastron, two hundred
milliojia of miles further than Neptune's. Now to con*
trol motion so swift in so spacious a path, 3|- times the
solar quantum of matter must be present; of which one-
third belongs to the satellite itself, constituting it a body
rather more ponderous than the sun, though giving no more
than xsW ^^ ^*^ light. Thus the contrast between the
components of this binary star could scarcely among visible
objects be more pronounced. And its significance ia accentu-
ated by its essential repetition in Procyon, the lesser dog-
star.
Since its motion was known to be disturbed in precisel}'
the same way aa the motion of Sirius, no doubt was enter-
tained of its belonging to a binary combination. But the
second member of that combination long evaded search, and
was at last identified by Professor Sehaeberle at Lick, November
13, 1896, in the modest guise of a thirteenth-magnitude star
4"' 2 from its primary. So far. its movements tally well with
the period of forty years, hypothetically attributed to them by
Anwers in 1361 ; but indicate probably a markedly eccentric
orbit instead of the nearly circular one assigned by him.'
Schaebeile's satellite again exemplifies the strangely disparate
nature of soma stellar couples. It exerts tliree-fifthe the
gravitational power of the sun, while emitting no more than
g^ of its light. Procyon ia further off from the earth than
1 Newcombj The Stan, p. 162.
158 THE SYSTEM OF THE STAES
Sinus, thoQgb cot in the proportioD of its inferiont/ in magni-
tade. Its actual lummomtj evaroelj amoonu to otte-fiftli tfast
ci the gretiter dog-sUr.
The detection of porti^Uj obscure stellar schemes goes ob
apiOQL The disturbances of motiou telescopicaUy app^mt
•Oggeited analogous diaturbaDces of motiou recogniadile
onlj witb the spectroscope ; and the hint has proved extt«-
ordinaril^ fniitfuL Stars like Procyoa are coiinected bj
innumerable gradatioos with stars like AlgoL This we shall
lAam in some detail further on.
There are other criteria besides that of visible revolution
in au orbit by which physical can be distinguished &om
optical double Btara. Since 1812, when Beeeel pointed out
tho concluaiveuess of the argument for real cotmection implied
in the advance together of the st&xs of 61 Cygni,* "common
proper motion " baa been ujiiverBally admitted aa a proof of
geiuiiue usaotiifition. Thua the lustroua pair y Arietis has
continued relatively fixed aince Bradley measured it in 1755;
yet its members are fellow -iravellera through apace, and
aiwuredly keep mutually circling aa they go, although so
slowly that a century and half count almost for nothing in
the majeBtic cycle of their revolutions. Again, the brightest
atar in the Soutbetn Cross is made up of two stars of re-
■pectively 1'6 ami 2*0 magnitude 5" apart, the situatione of
which have not penxsptibly changed since Duntop determined
thcni in 1826. This amounts to saying that their small
proper movement is identical And even independently of
thi» jH>9itive teat, the probabilities are enormously against the
accidental dose juxtaposition of two stars so brilliant and so
naarly «quai as those of a Crucis.
The circumstance teetifiea strongly to the prevalence q^|
phynioil conuectioD between stellar pairs, that the averag^^
difffirence of brightaess between them growa steadily with
thuir distance apart^ approximately equal being usually con-
tiguous objects. Every degree of inequality is indeed found
iu undoubted systems ; still the chances of optical association
must obviously increase vastly, even at the same distances, witl^l
increase of optical disparity. ^^
The background of the sky is so thickly strewn with small
* Mimat, Cttrrf^iondau, Bd. xzvL p. 160.
DOUBLE STARS
159
8tarB, that we cannot be surprised if some of them happen to
occupy critical situations. Bather, there is ground for
astonishment at finding that certain remote satellites of
bright stars seem indissolubly united to them. Reguhis, for
example, carries with it, as it pursues its way across the
Bphere, a star between the eighth and ninth magnitude^
discovered by Winlock at Washington to be itself closely
double. The interval between the pair and its governing
body amounts to nearly three minutes of arc. Castor, too,
has att-ached to it a tenth-magnitude star at 74'' ; one of
fleventh magnitude 90" to the south-west of a Crucis evidently
belongs to its ooit^go ; ^ and Aldebaran forms with a minute
object at 31" what seems to be a permanent eombination
resembling in its effect to the eye that of Mara with his outer
aatellite.'-
Where two close stars seem fixed, relatively and absolutely,
the ca^ for their physical union must dei>end upon circum-
stantial evidence alone. But this is sometimes of cogent
import Conti-ast of colour, for instance, may afford grounds
for a strong persuasion of real relationship. Certain tints, as
blue, greeuj and violet, only occur among mutually associated
stars. We cannot, then, suppose the association upon which
they depend for their production to be merely apparent.
The topaz and azure components of ^ Cygni have no
appreciable motion of any kind, and they are separated by a
gap of 34", exceeding the limit of distance of real double stare
as defined by Struve. Yet it is impossible to doubt that their
brilliant hues are truly expressive of the systemic union from
which they in some unknown way result. The same may be
said of S Cephei and its blight blue attendant, and of the
much closer and nearly equal stars 95 Hereulis, the inference
being here strengthened by the concerted changes of colour
recorded of them. We might be surej too, of the dependent
status of the emerald satellites of the red stars a HeicuUs
iind Antares, even if it were not independently proved by
a community with their primaries in very slow progressive
movement.
Nevertheleaa, some highly coloured pairs have been eon-
' Inues, RtfeTtnoe Cntaiogue, p. Ill a,
' Bumham, A»tr. ycteh. No& 21S9, 'iS7£ ; Generai Cai'ilogue, p. 49.
Ym
ttl^ mpplm tMlfecr wiMUt udioiiBa of
Wbn ecamoB to both aeabomof a pMc;^ leam bo n»m
Cpr doolit OB the anlQeetu We abill racttr to this bopac in «
ktcr cfaApCer.
8Un v^th MoertAtned pRifir fiMtioao cfaAnctenB tf
tlieiMBlv«* tlM lubire of their eompnooniiiipL For eiyier
Uujf lc«ep oa together or tbej ihoir npu of incipieBt wepan-
tioD, iknrlj bat sorely marking the diwtinfitinn between &
looting ttttion And mexe tempofuy oootiguity. In the latter
otto the moraaeat of one of the stozs referred to the other
neoanarily proceeds along a straight line, so that rectilineal
diJvplaoecuent is an infallible mark of an optical coupIeL One
caiiouHXy cloMe (S. 1516; occora in the oonstdlation Df»ca
Two ob&n, of 7 and 7'5 magnitude, pasaed in 1356 so near to
one another by the hazard of their paths nearlj inteisecting,
M to preiwnt Ibc e(f*ytst of two points of light, one inch apart,
at u furlong'ft dlHtaace from the eye. Their angolor aepara-
tioQ, Uven only 'i'^'6, ia now 13'', and it will continne to grow
indefinitely. Their absolute disconnection haa heen confirmed
by direct meaiiurenienta showing them to diifer extremely in
raiuoteneM from the earth. The larger of the two, by one
^ Oov^$ Rmdu$, i. UuviL pp. S36, 872.
' Manok, ICnoieledge, toL xil p. 17<}.
DOUBLE STAES
161
of ehose aingularitiefl which Hbound in the heavenft, fomifi a
genuine pair with a etar very much fainter than ita spurious
companion.
From what has been said, it is clear that a good deal of
patience is needed for the inyestigatlon of double gtars> Tbe
facts about them must often be allowed to ripen for a long
time before they can be turned to account. Sooner or later,
however, their fruit cannot f^il to appear. There is. perhaps,
no other branch of science in which induatry is 30 sure to bo
rewarded with definite results. The £rst step i6 to separate
perspective from physical couplea ■, this can only be done by
the persistent repetition of exact measures. The next is to
detect nascent circulatory movements in true binary pairs,
or to keep watch on them us they progreaa. Their careful
comparison with theory may at any time bring surprising
novelties to light. For each steUar system is in effect a
world by itself, original in its design, varied in its relation-
ships, teeming with details of high signi&caiice. But at
present only an imperfectly traced outline of the construction
gf some three-score among hundreds of them is before us ;
their multitude distracting attention. Yet it would be better
to make intimate acquaintance with one than to know a score
superficially. All the rasources of modem inventiveness
should be enlisted in these inquiries. Not only the revolu-
tions, distances, and masses of double stars, their movements
etcross and in tbe line of sight, should he determined with
ever-iucrcasjng precision, but their colours and magnitudes,
and above all, their separate spectra, both visual and photo-
graphic, should be recorded. By such means as these, real
knowledge will be augmented far more than by the most
brilliant auoceaa in the telescopic detection of new pairs.
This has its own interest and value, but the recesses of
sidereal structure must be otherwise explored.
11
CHAPTER XII
BTKLLAB OKBITa
The strong presomption that the law of graTitation wotild
prove trujj univerBal has been fully borne out hj mvest^a-
liouB of stellar orbits. Binary stara circulate, it can be
unhesitatingly asserted, under the inf uenca of the identical
force by which the bud sways the movements of the planeta,
the earth the movements of the moon. This, it is true, does
not admit of mathematical demonstration, but the over-
whelming improbability of any other supposition enforces an
almost equal degree of certitude,^ The revolutions of the
stars are hence calculable, because conducted on faniiUar
principles; their velocities have the same relation to masB,
their perturbationB may lead to similar inferences as in the
Bolar system.
Observations, however, must precede calculations; and
they are rendered arduous in double stars by the extreme
minuteness of the intervals to be measured Many revolving
pairs never separate to the apparent extent of a single second
of arc ; yet this fraction of a second may represent, in abridg-
ment, a span of some thousands of millions of miles. In-
finitesimal errors, magoified in this proportion, become
of colossal importance, and often impenetrably disguise the
real aspect of the facts.
For determining the relative situations of adjacent stars,
two kinds of measurement are evidently needed. The fiiut
gives their distance apart^ the second the direction of the line
joining them as regards some fiied line of reference. That
selected is the " hour-circle/' or great circle passing through
* Tl^aerihnd, SuiUtin Jstronamiqtte, t. iv. p, 13.
142
J
STELLAK ORBITS
163
the pole and the larger star, and the angle made with it by
the line of junction of the pair ia called their " poaition^agle."
It is couuted from 0*" to 360°, in a direction opposite to that
of the movement of watch-hands, and a star is hence aaid to
be ia direct resolution if its circuit \s from north to south
through east, but in retrograde revolutiou^ if it ia oppositely
pursued.
i^ow the succeesive places, from year to year, of the moving
Btar, obtained in this way with absolute accuracy, would
fall into a perfect ellipse, the foresliortened delineation, as it
were, of the real ellipae traversed in space. For the star's
path ia seen by us projected against the sky, or rather upon the
plane touching the sphere at that point, while the actual orbit
may lie in any one of an infinite number of planes. The two
curves, nevertheless, have relations by which one can be
deduced from the other with geometrical certainty. Both are
eliipaea, and in both the " radius vector," or line drawn from
the satellite to the primary, describes equal areas in equal
times. But the position of the chief star at the focus of the
real ellipse is not maintained in its perspective repi-esentation,
in which the " projected focus " is often quite unsymmetrically
placed. Fig. 22 shows in juxtaposition the apparent and
actual ellipses traversed by a Ceutauri, as delineated and com-
puted by Dr. See. The distorting effects of perspective can
be estimated by noticing that, white the true epoch of
peiiastron was in 1875, the stars nevertheless continued to
draw together optically until 1877- Once then the seemin/f
orbit of a binary star is thoroughly ascertained, the problem
of determining its actual orbit is as good as solved, the
transition from one to the other being effected by a mathe-
matical operation of no considerable difficulty. Even when
the seeming orbit is a straight line the process remains
feasible, and in fact one of the most reliable stellar theoiiea
relates to a couple, the movements of which are conducted in
a plane passing, it may be said, accurately through the earth.'
The stars of 42 Comai Berenices appear simply to oscillate to
and £ro in a period of somewhat less than twenty-six years,
never diverging to a greater extent than about half a second,
^ O. Struve, Monthly Notices, toL xxit. p. 367 ; AUi dtlV Accad. Font. t.
xLt. p. 259.
Wia. %— Appftnnt and real Orblta at Alpha CenUnri^ frbs r«duc«l dii^nin oT Uig Api»n«,t
aUlpae La Sawcomti'a Stars hu bean anilnd of.)
travelling in paths eeen nearly edgewise are 7 Coronae
Borealis with a period of ninety-five, 44 Bootis with one of
261 years, and a bioary in Ophiuehua (S 2173) revolving in
forty-six years.
Nothing would at iirgt sight seem Baster than to lay down.
STELLAR ORBITS
165
from a sufficient store of data, the apparent track of a star.
Yet the task is often a moet embarrassing one. Owing to the
excessive imnuteness of the quantities concerned, the best
observ'ations can give only loose approximatioue to the real
facts. The margin of uncertainty, always veiy wide, at times
exoeeds any reasonable Umit, and computers are hence obliged,
as a rule, to reject some part of the materials before them as
mifileading and incompatible with the rest. But tlie exerdae
of discretion leads to diversity of results, and totally different
orbits can thua be deriTed from the same set of obeervationa
by varying their treatment so as to distribute differently
their inherent errors. Where only a moderate arc of the
orbit has been described, the problem of ideally completing
it admits, from the iudeterminateness of its conditions,
of no rigid solution. One might, in Mr. Burnham*a opinion,
as well guess the period as go through the formality of
calculating it.^ When the cftmpanion of Sirius» for instance,
had been eighteen years under scrutiny, it was Btill impossible
to decide whether it would return to its starting-point within
the halfKientury allotted to it while still an unseen agency of
disturbance, or depart on a remote excursion from its primary,
demanding some hundreds of years for its accomplishment.^
In no department of astronomy is the mischief of " per-
sonal equation " so sensible aa in the measurement of double
stara. Nearly all available data are prejudicially affected by
it, and those emanating from different individual Gources are
thus often rendered exceedingly inharmonious. Much labour
and ingenuity have been spent in determining its direction
and amount for various observers, with a view to freeing their
resulte from its effects ; and after all, it remains a question
whether the observations so elaborately corrected are not more
misleading than in their *' raw " state.
All these complications might be at once swept away if
it were possible effectively to substitute the camera for the
micrometer. The photographic method leaves no room for
systematic, very little for accidental e^Tors, G. P. Bond, of
Cambridge (U,S.), showed in 1857, long before the intro-
duction of the modem " dry plates," its wonderful capabilitias
1 Popular Aitronofn^t vol. i. p. 248.
' Plummen Monthly Notices, vol. iliL p. 83.
166
THE SYSTEM OF THE STARS
for the accurate regisiration of the varying relative situatitms
of double stara ; * and those capabilities were more fully
realised in 1886 by the skill of the MM. Hemy. Somespeci-
meua of the Paris photographs of double stars may be inspected
iQ Fig. 23. The repeated impressious shown of each p^ wen
obtained by allowing free play to the diumal motioa daring
certain definite intervals between succeaaiTe short exposures.
The line of displaceioent of the stars traces out conseqaentlj
part of a circle of declination, aad their angles of position are
directly measurable from plated embodying the data for their
own orientation. The eiactitode of determinations from them
proved very remarkable ; for ^ XJissd Majoria the *' mean error "
of eingle measured of distance amounts to only 0^*077* of
TV..i;.rus
fia. 33.— Four Daiibl* BUm photojcnpfanc! &t Puii. (Mouehs^
angle to 0*56.* And this ia no illusory preciBion, but the
statement of an unalterable fact. Unfortunately, however.
the calculation of stellar orbits from photographic meaatuces
must long continue impracticable.
Their application is at present restricted to Bucb pairs as
are neither very unequal nor very cloee. The ditfuaive bright-
ness of Sirius, for instance, leaves no pogsibility of getting a
separate print of its compinion, nor could even the much lesser
disparity between the stars of B Cygni be made compatible
with the distinct self-portraiture of both. Again, the minimum
interval at which even perfectly equal couples have hitherto
been successfully photographed exceeds two seconds, cloaer
objectB running together on the plate. But the closer objects
are just those most likely to be in rapid circulation ; and
measures of any others are only in a remote sense useful. In
I Aatr. yaeh. No. 1129.
* Monchu, La Photoyraphie jt9tr(»uiniq'U4, p. i4.
STELLAK ORBITS
167
>partioii, tbeOj ae Hfcar-couplea lead themselves to photo-
"graphic delineation, they are unprofitable to compntera ; while
those that repay computational labour for the most part
evade Tegistration with the camera.' l^ere are no doubt
exceptions, such as Coator and a Centauri \ and a jearly photo-
graphic rec^^rd of each pair of the kind would eventually supply a
stock of facta impaii'ed in value by no perplexing inconsistencies.
The apparent orbits of revolving stars will be virtually
inflcribed, one may hope, in future collections of negatives.
The process of drawing a smooth eurve will then no longer
admit any wide latitude of discretion ; and the representative
ellipse, instead of threading its way amid a straggling crowd
of outlying observational will paaa, not indeed actually through
(which would imply the annihilation of error), but very close
to all the given places.
Above eighty stellar orbits have eo far been computed by
Doberck, Gore, Glaaenapp, Bnrnham, See, and others. But
for the moat part tentatively, nor always with success. Pre-
dictions are often at fault; orbits are assigned only to be
discarded ; the moving stars show themselves regardless of the
trammels of theory. Thus, the persistent approach, since
188T, of the components of Castor makes it certain that the
millennial cycle ascribed to them by Thiele is much too long^
and suggests^ even apart from calculation, that Sir William
Herschera estimated period of 342 years may be nearer the
mark- The movementa, on the other hand, of the fine
southern pair, 6 Eridani, demand a continually lengthening
time-allowance; and Mr. Bnmham was inclined, in 1893, to
regard them as rectilinear, that is, of a definitively separatist
character.' The stars, none the less* seem at present to be
conforming pretty closely to Mr Gore's orbit, which should be
completed in 302 years.*
Premature attempts to determine stellar revolutions are
strongly deprecated by Mr. Bnmham, Some computed orbits
are so purely provisional that, ae he points out, many others
of a totally different form might be substituted for them with*
out doing any violence to the obaervationa. Among the
1 W, J, Hussey, PulL Astr. Soc. Pacijic, No, 74, p, 102,
* Aitr, and Aatrophyaia, vol. xii. p. 698.
^ lunea, Re/ertnct Cat, p. 13 A.
I6d
THE SYSTEM OF THE STABS
earliest of known couples is ^ Aquarii^ divided 1^ Fatba
GbxiBlian Mayer in 1777 into eqnal compoueats of the fourth
snagnltuda They are in alow circulation, having described in
the course of a centuiy and a quarter, an arc of leos than 60\
From the scanty data thus supplied, Dr. Boberck baa derived
an orbit traversed in 1578 years, the Lotigeel; period yet found
for a binary systenL But it i% or may be iUasory, Mt
Buroham Bcaroely goes too far in saying that the zuaBfitiTeA of
at leafit 500 years must be available before a aatisfactoiy
theory of this Btar's revolutions can be formulated.^
An opposite in&tance of uncertainty in calculation it
afforded by £ Equulei, which now ranks as the quickest of
visual binaries. Discovered by Otto Struve in 1852, it was
watched through many complete ciTcoits^ each of which was,
until 1900, held to occupy 11^ years. In that year, however,
Professor Hussey expreeaed a suspicion that the admitted
period was just twice too long ; * and it was amply justifidd
by the Btar's subsequent behavionr.* Confirmatory spectro-
Bcopic observations have also been made ; * and the pair
promises to supply a most useful link between stars measuiabte
with the micrometer and stai^ only resolvable on pmmatic
negatives. It was long &go perceived * that the combination
of both methodB, if rendered practicable, would lead to a far
more complete acquaintance with the systemic conditions of
stars than the employment of either of them separately. The
capabLUtiies of one, in fact, fill the lacunse left by those of the
other. Stellar orbits as computed from visual data are of
undetermined size. Their distances from the earth have to be
further ascertained before the scale of their construction
becomes known. But it can also be derived, under favourable
circumstances, from spectroscopic measurements of velocity In
the line of sight. For these give^ in miles per second, the
rate of circulation of such star-pairs as prove amentible to them ;
and the rate of travel and the period virtually combine to state
the dimensions of an orbit lying in a known plane. The mass
' Fop, Aiir, voL it. p, 475. * Pubi. Aatr. Soq. PoctjSc, No. 76.
* F«bL Liik Obtervatortf^ vol. v. p. 20Cp*
* lAck SvlUlin. No*. 4, 52.
' Fox Tftlbot, Heport Brit. Aa. \871, pt. ii. p. 34 ; Niven, UoTUkty ybtiwi^
Tol, XXI jv. p, 339 ; Pftlica. Attr. Nttth. No. 2941 ; Hattibaat. Proc. M. /rwA
Aead. vol. iv. «ct. ii. p. «63 ; T. J. J. See, AUr. Nath. No. 3314.
STELLAK ORBITS
169
of the atara pursuing it and their parallax can thence eosily
be deduced- And Profeaeor Huasey accordiugly derived for
5 Equulei a combined attractive power neatly twice that of
the eun^ and a parallax corresponding to a light-journey
of 46 yeara. These resultg are the first of aubetantial value
obtained by the application of the spectroscope to a telescopic
double star.
The pair that comes next to B Equulei in rapidity is
ic Pegasi, divided by Mr. Bumham in 1880 into 4*3 and 5"0
magnitude componentSf not much above one-tenth of a eecond
apart. They liave einc* then performed more than two
revolutions (period 11^ yeara) in an orbit viewed by ug under
an angle of only 9°. and coubeq^uently foreshortened into an
exceedingly narrow oval, the oscillations of the stars in which
be followed only with the most perfect appliances.
A Btandard collection of forty stellar orbits, with new
"elementa calculated by himself, was published by Dr, See in
1896/ Twenty-eight among them have periods falling short
of 100, fourteen of 50 years; and these comprise some of the
beat-determined^ though most recently discovered pairs —
^ Sagittarii, travelling in 18 years, 9 ArgCls in 22, Sb Pegasi
in 24, ^ Delphini in 27 years. The longest stellar period
likely to be authenticated is that of 370 years, assigned by
)r. See to o- CorouK Borealis, discerned by Herschel as double,
August 7, 1780, Yet, thirty years ago, Doberck found it to
'need 84G years to finiBh a circuit; and he was an expert in
researches of the kind. In general, as Mr. Burnhani has
insistently urged, revolutions require to be finished, or almost
finished, before they can be said to be ascertained. Among
the beat stellar theories extant is that of f UrsaB Majoria, one
of two fourth 'magnitude stars marking the hindmost paw of
the Great Bear. Divided by Herschel in 1780. this couple
was made by Savary, in 1828,^ the subject of the firBt experi-
ment in the extenaion of Newtonian principles to the sidereal
universe. It Hucceeded ; for the stars were found to describe,
as nearly as could be expected, the orbit csilculated for them
on the supposition that their mutual gravitation was the
Inence binding them together into a moving system. The
' S^ltUviA of the SUllar SyftiiM, p, 2*3.
* Conn, des Ttmps, 1830, pp. 56, 163.
n
170 THE SYSTEM OF THE STABS
valiUUy throughout the universe of Newton's law has nerer
since beeQ opeu to serious question*
The path of f UrstB h&& of Late been seYeraJ times re-
invegiigated, and with results so concord&nt ^ to give &
atrong assurance of their approximate accuracy. It is &
considerably elongated ellipse, the e-ccentriciiy being expreaaed
by the fraction |» which ia just twice that of the orbit of
Mercury, htdf that of the orbit of Encke'a comet. The period
of traversing it is 60 years ; its semi'iuajor axis vould
subtend, if seen without foreshortening, an angle of 2^". and
it lies in a plane inclined 56'* to the plane touching thf
sphere at that poiut.^
We are ignorant of the mass of this system because we
are ignorant of its distance from the earth ; but whatever its
distance and whatever its mass^ there seems no doubt that
the stars conjoined in it are intensely luminous. If of the
same meau density, they must be, st^uare mile for square mile
of aurface, of about two and a half times the solar brightnesa
Be terminations of the distances of binary stars are of speoia!
interest from their leading to a knowledge of their masses.
The connection is easily explained. Angular measurements,
which are the only ones possible to be got of objects out of
tangible reach, are convertible into definite linear values when
the radiua of the sphere they refer to becomes knowo^in
other words, when the interval of space between the eye and
the objects measured is ascertained. So that the dimensions,
in seconds of arc, of the orbits of stars at determined distances
give at once their dimensions in millions of miles, whence,
with the help of their periods of revolution, their masses
easily follow. For by the law of gravity the attractive power
of any system is proportional to the cube of the mean
distance of the bodies composing it, divided by the square of
their period. Employing^ then, as a unit of space in this
little calculation the distance of the earth from the sun, and
the year as our unit of time, we get the mass of each pair of
revolving stara in terms of the sun's raaaa. It comes out. of
course, larger in the ratio of the cube of the distance for the
1 Date oD tlifiSfl seToral faaadB, together with others defining the titiulaon of
petioatrou and of the liine of interaectioQ of tho orbiUl »nd refecum pluutt
coDfitituta whftt an eaU«d the "alemeiita" of ft«tAr*i moTementB.
STELLAH ORBITS
171
Bame period, and smallei* m the ratio of the square of the
period for the same distance. Swiftly-moving and spacious
syatems cotibaiti accordingly great quantities of matter,
aluggish ones comparatively little. Many radiant couples
maintain, decade after decade, an all but absolute hxity.
Alpha Crucis, 95 and a Herculia, 7 Arietis are eiamples. The
nascent diBplacemente of ^ TJrsai Majoris suggest the possible
accomptishment of a circuit in 1 0,00 yeaa-s ; those of 7 Delphini
might conaiafc with a period of four millenniums. This strange
inactivity intimates for the stars displaying it either an exceed-
ingly small mass^ or an inconceivable remoteness from the
earth.
A list of binaries moving in known orbits for which
par^a^es have been ascertained, will be found in Table IV.
of our Appendix, It is unfortunately brief; yet it embodies
some important information. One of these pairs. 35 Pegaai^
was divided by Burnham in 187S, and completed in 1904
its first observed round. The components, although no
brighter than sLxth and eleventh magnitudes, exert a gravitating
power (from Eumham'a elements)' eleven times that of our
fiun, Tliey wear the aspect, as Mr. Gore remarks, rather of a
aun and planet than of two suns. The primary eentuples the
light emitted by its satellite, and there is just the disparity
between them that would be presented by the sun and Jupiter
if of the same intrinsic brilliancy. These would, on the con-
dition supposed, and, at the distance (attributed to 85 Pegasi)
of sixty light-years, show as a pair of 7^ and 12j magnitude,
never above 0""23 asunder. The utmost powers of thegr&tt
Lick refractor would scarcely be adequate for their separation ;
but the real stars being respectively four times brighter than
the iUustrative sun and planet, can be kept under watch and
ward.
The masses of eight visual couples are fairly well known,
and their total value is just that of thirty-one suns. On an
average, then, any one of those systems contains nearly four
times as much attraetive ener^ as the solar system, each
individual star being equal in this respect to a pair of
Buns like ours. Were the extension of this result legi-
' Otneral Gaialcgue, p. 370 ; ComBtock, Aatroph. /(mm, roL xril. p. tf23.
The pftralUx of 65 PegAai U taa staaM to be well-usured.
t?2
the; System of the stars
timate, Che-iiiataDcee of all stars revolving in asccft&ised
orbits might be inferred from their assiuaed massiTeneaB (am
the relation between distance and mass is convertible^ ibI
upon this principle Madler derived what he eddied tbi
" hypothetical parallaxes " of binaries/ rodconing, howeTH,
the mass of each pair to be only that of a single sun. TIib
estimate is uow seen to be much too small, and the distaixa
founded upon it to fall proportionately short of the truth.'
But, indeed, no general conclusions of the kind are fit fioi
application to individual c^aea. The range of variety is »
great that only simulated knowledge can be obtained in ihi
way. Yet collective inferences are not therefore worth-
leas. Thus, from averaging the masses of only eight binaria,
we have gathered plausible gi-ounds for believing our sun to
occupy a low rank as a centre of attraction. It may be,
nevertheless, that the swifter binarieSj which can at preeec;
alone figure on such a list, give too high an average mass.
Calculationa based upon the orbital elements of revolving
stars t«ll nothing of their reiative masses. They apply onlj
to the common stock of matter in each system, leaving its
distribution to be otherwise tested. This cannot be done
except through the due apportionment of movement between
the members of the system — an arduous task, "just begun to
be grappled with.
There ia no such thing in nature as a stationary body
round which other bodies circulate. Answering tnotiou there
must always be, though on a scale reduced in the exact pro-
portion that the mass ia increased. The earth, for instance,
describes, under the influeuce of the moon, an ellipse precisely
similar to that described by the moon under the influence of
the earth, but eiglity-one times smaller. And the sun corre-
sponds in the same way to the revolutions of every one of the
planets, notwithstanding that the centre of his movement as
regards each of them, with the single exception of Jupiter,
lies far beneath his own surface. Binary stars, however, are
an
J"
m
itt
\i
^ Thb nimseB of r^TolvJug stan vary, eaUns paribtu, u the cubes of tbflii'
diataDces from the eartb. Of s7at«Qi& ideuticAl ib period &a<) ftpparent tnorc-
mtmU on<i twice u remote u anotber would be eight times as mw»iye, out thrct
tliUM u remote, twcDtj-Mveti timei ma maasiTe, and so on.
irobably often almost equally maasive, and therefore almoat
uaUy mobile bodiea. The fixity of one member of each
-jkair 13 purely conventional — an iudifipenaable lictiou without
"which meaeurementa would be impracticable. Those actually
made give the sum of the movenLenta of both stars, and an
orbit computed from them represents the Bum of their dis-
tixict orbits. Identical in shape and position with the tnie
eUipeeSj it differs from them only in size, its linear dimensions
in any direction being equal to both theira taken together.
The genuine centre of movement of two mutually ciitling
stars is their common centre of gravity, which lies on ^
straight line drawn from one to the other> at a distance from
each inversely proportional to its masa. The Btrictly similar
orbits traversed by each are then spacioua in the aame inverted
ratio. The larger fitar performs the smaller circuit, and vice
1626
I92S
fia. U— OrblU of Uie OompOnClit 8Um vf daasa^ Vlr^iali.
vend. In the case of their equality, their orbita must inter-
sect if elliptical, but coincide if circular, when the stars will
pursue each other along the same tracks while occupying in it,
at each successive moment, diametrically opposite poaitions }
nor could either, during an eternity of undisturbed revolution,
gain a hair's breadth upon the other. But circular move-
ment is not even approximated to by telescopic binaries,
which usually follow highly eccentric paths.
"We may take 7 Vii'giuis as an example of a pair moving
in equal ellipaes, the relations of which are shown in Fig. 24.
They have, it will be seen, a common focus, the seat of the
centre of gravity, from which the stars (being of equal mass)
must always be equally distant. Neither can approach to or
recede from this point of origin of the force acting upon them
without the other simultaneously doing the aame ; the two
muat be in periastron and retire towards apastron together,
losing and subsequently regaining velocity by the same grada-
m
THE SYSTEM OF THE STAES
tioQS, The Btara of a Centauri also travel in orbits se^Mf
eqiitil, but much leas elongated than those of 7 VirgiiUB {see
Fig. 2B>
The movements of unequal stars are Rimilaily oonducted
That is to eay, the proportion of their respective distances Trom
the common focus is invariable. They are accordingly always
found in cyarreaponding parts of their orbits, and at opposite
ends of a right line paasLpg through the focua. The manner
of thtiir revolutions can be realised by a glance at Fig. 26,
repreaenting the orbits of Sirius and its companion, the smaJI
ellipse belonging of course to the bright star.
Obviously, from what has been said, knowledge of the
relative masses of binary stars would ensue upon knowledge
of the relative dimensions of their separate orbits. This,
indeed, is not within easy reach. Befiaed measurements, in a
( 1S7J \iB75 j ( 'Ms/ W J
FlO. S6.— O^bft* prtiin CompaDcnt Stan
of Alptu Centiurl.
Pio. adw-'Orblta of SiHn« mai tt>
compuiion.
prolonged eeries, of the individual components must first be
secured* either with the transit-instrument or by micrometrical
refei*ence to some adjacent star.^ From the proper motions
of binary syetems information of the desired kind may, in
some cases, be elicited ; for the track pursued by each star is
necessarily, if their orbit be seen under a fairly wide angle,
a Binuous one^ like that of the moon round the sun» while
the centre of gravity of the two advances uniformly in a
straight line. Now this neutral point was, by Mr. Stone in
1876,'' and again after twenty years by Mr. Roberta,* fixed
about midway between the components of « Centauri. They
are, accordingly, almost equally massive; yet the ratio of
their luminosity is as four to one. Sirius, again, deviates
from rectilinear motion to nearly half the extent that its
companion does; it is, then, twice as maaaive, but 4300
* Pickering, iVmr. Anur. Acad, vol viii. p. « {1881J.
3 Monthly Natitts, voL xxxtL p. 258. ^ Aair. Nach. No. 33S0.
STELLAR OKBITS
175
rtimee more lumiaoua. And evidence of the same nature
shows ProcyoD, while outshining its satellite 4700 times,
to outweigh it no more than seven times. Analogous
instances are gradually multiplying. Profeseor Comstock
"has aftcertained that the faint companion of 85 Pegasi con-
itaina more matter, in the proportion of five to three, than its
'coxnparatively brilliant primaiy;^ and similarly, a fourfold
predominance in mass is assigned by M. Adalbert Prey to the
fiix times lees brilliant member of the interesting pair 70
' Ophiuchi.* There remalD si^ couples, the relative masses of
which have be.en determined by Mr. Lewia from the Greenwich
meridian cbaervations. They are: 7 VirgimSj f Heroulis,
Tf Casstopeiffi, 0^ Eridani, f Urwe Majoris, and f Scorpii.
Only for the first a normal regult (if we may call it so) was
obtained. The stars of 7 Virginis seem perfectly matched
in every respect — in average lustre, in speetrumj and m
atti^etive power. In all the other pairs, varied degrees of
disparity were met with, the component inferior as regards
light being uniformly superior in the government of motion.
In the system of ^ Herculis, which revolves in thirty-five
years, the mass seems evenly divided, while no more than
one-aixteenth of the total light is given by one of its members.
Mr. Lewis has, moreover, detected anomalies in the move-
ments of this pair suggesting the perturbative influence of
fttL invisible body. The disproportion between mass and
luminoaityi which appears to be ratber the rule than an
eicception among binary stars, has a most important bearing
upon their physical history; but we shall not learn its full
meaning until distinctions of spectrum are correlated with
discrepancies in relative brightness.
Professor Pickering * and Mr. Monek * of Dublin separately
lived the existence of a rehition between the movements
magnitudes of bmaries, rendering it possible to determine
' their comparative luminous power proportionately to mass
quite independently of their distances. It is necessary,
K^»"«Tever, to assume either that the components of each pair
AitTcqfh. Joum, vol. xvii. p. 223.
fine, ^m. Jcad. vol. vlli p. 14 (IfiSl).
(Aitrvatory^ toI, z. p. 96 ; ICncwUdge, tq], jai. p. lil ; Jtntm. Sri*. Attr.
An, rol viii. p. 179.
^ AatT, Nach. No. 394S.
1T6 THE SYSTEM OF THE STARS
are of similai- quality in this respect, or elae that one d
them is of negUgeable mafia ; nor doea the formula distioguidi
between extent of surface and intently of ablaing. TU
bodies cotididered may owe their differences in "maa-
brightness " either to variety in mean density, consequently in
the extent of shiumg siirfdce, or to variety in actual briUiancj-,
area per area. The etfectfi observed by us would be the supt
The results obtained confirm the prevalence of astonishing
v&rietieA in the emissive powers of stars. Taking ( Vztse u
the standard pair, Mr. Gore calculated in 1891 ' the relafcire
brightneas of about ^ty binaries moving in determined
orbits. The tabulated figures are curious, even setting aside
such objects as Castor and 7 Leonis, whieh came out phe-
nomenally brilliant beoauee of the exaggerated length of the
periods assigned to them by earlier computers. The duski^t
stars in the list are those composing 0^ Eridani, which revoN
in ISO years, and considerably exceed the sun in gravitatii]^
power, although claiming respectively only ninth and tenth
magnitude rank. Admitting their density to be the BamB
as that of f Ursae, they seem to be intrinsically 660 time*
leas luminous. On the other hand, X Ophiuchi and y Coron*
Borealis are, the first, twenty-nine, the second, twenty-oofl
times more brilliant ; if HercuKa and 7 Virginis, notwith-
standing the difference of their spectral types, are about on a
par in this respect, each couple sliining with five times the
standard lustre ; while TO Ophiuchi and if CasBiopei^ main-
tain the similarity of their general character by their agree-
ment in poflseasing a aurface-brightneea only one-third that
of f Ursaj. The only rule governing these diveraitiea is that,
on the whole, Sirian stars are much more lustrous propor-
tionately to their masses than solar. Corresponding data
regarding stare with banded spectra would be especially
valuable ; but are unattainable, since objects of the kind are
usually inimobiJef or inordinately alow in circulation.
The mo8t striking general peculiarity of binary orbits
their high eccentricity. Nearly all of them are greatly more
oval than the planetary paths round the aun, and a large
proportion approach to cometary shape. In the "mean
stellar ellipse," the focus of revolution is situated just half-
^ iV«, Soy, IrUh Acad, yqL i, Nft t, 8rd x^riBS.
STELLAE OKBITS
X7T
between tlic centime and one of its extremitiee. The stars
are, acoordingljr, aeparuted ut apaatron by four times their peri-
aatron tlistance. " The average eccentricity among the double
fttara/' Di\ See writes/ " is more than twelve times that found
in the planetary system, and this extraordinnry reault is
manifestly the expression of a fundamental law of nature,"
Indeed, an improved star-orbit is commonly more elongated
th&u the one it replacea Pi'ofesfior Kuasey, for instance, in
Tecalciilitting the elements of B Equulei, found it necessaiy
to triple the previously assigned ecceutricity.
The circulation of binary stars is indifferently retrograde
or direct. No tendency is perceptible towards concordance
regarding the direction in which their tracks are pursued
Nor do they affect a common plane. They lie at all posdble
angles towards the Milky Way, and seem wholly exempt from
ita influence.* Ths existence of a fundamental plane of
movement would be of high significance as regards the history
and relations of the sidereal world ; yet the whole drift of
modem research suggests, rather than the close and rigid
union between its parts which it would indicate, a loose con-
nection destined to be extensively modified by tijue,
^ EvoWtitnt GfUtA stellar Syxtems, y. 261.
' Ihid. |i, 24h, An aaalogoiia conclusion ha.d been aomevliat eatlier ruched
by Miw Alice Ereritt.
IS
The light-changes of double stars are commonly of a fitfal
aad icdeciaive kind. They may a£fect one or both members
of stationary pairs ; but visibly revolving stars, aa a riile,
conspire to vary, if they vary at all. The alternating fluc-
tuations of y Vii'giuis, discoverable only by close attentiou
to the swaying balance of lustre between the components, are
in this respect typicftL Eaeb may be described as nonnally
of the third magnitude, and eaeh in turn deeliues by about
half a magnitude and recovers within a few days, yet so that
the general preponderance during a cycle of several years re-
mains to the same star. The eiistenee of this double perio-
dicity was recognised in 1851 by M. Otto Struve, who» how-
ever, despaired of inveetigating it "with suceess in a latitude
where the stars subject to it never rise more than 30" above
the horizon.^ Xor has anything more definite been sjnoe
learned on the subject. Instability still persists. It is made
evident by frequent inversions of the position-angle, accord-
ing as oae or the other component, taken to be ^perior in
brightneaa, is chosen as the origin of measurement;^ but no
trace of regularity ia apparent in these inversions.
The pair circulates in the moat eccentric of ascertained
stellar orbits (see Fig. 24). The elHpse traversed by 7 Virginis
in 194 years is, in fact, proportionately somewhat narrower
than the path round the sun of Encke*s comet> bo that the
stars -mil in 1934 be separated by at least thirty timeB the
sky-interval between them in 1336, when they merged into
' OhMTvations de Pautkovsa, t, ii. p. \2Z.
' OorSj Knoioiedgi, vol. xxil. p. 201.
17s
VAltlABLE DOUBLE STABS
179
single telescopic object A spectrum of late Sirian pattern
combined -vnth a perceptible tinge of yellow in tlieir light
Kelative variability ia in 44 Bootis still more marked than
, 7 Virginia, But here a fundamental disparity between the
iponenta ia seldom and temporarily aboliahed. Noted by
[ereehel aa considerably unequal in 1781, they appeared to
perfectly matched in 1787- And it is worth noting that
iey had in the interim passed pcriastron* Struve observed,
fune 16, 1819, a difference between them of two magnitudes,
^hich had fiunk to half a magnitude in 1833. Argelander
Bund them precisely equal June 6, 1830; Dawes perceived ^
Ipril 27, 1841, a slight advantage on the Ride of the usually
smaller star; while the superiority of its companiou was recorded
by M, Dun^r at Lund as ranging^ during the years 1869 to
1875, from 0'4 to 1'3 magnitudea^ Since their changes,
often simultaneous, are not always in the same direction, their
combined variability has never been conspicuous, the brighten-
ing of one tending, on the whole, to neutruliee the fading of
the other. The stars of 44 Botjtia, according to Doberck's
elements, traverse a highly eccentric orbit in a period of *261
years. Their tints, varying from yellow and sky - blue to
white and dull grey, cannot be without infliueuc-e upon their
photographic magnitudes, determined at raria in 1886 to be
5"3 and 6. Their joint light, though of the same spectroscopic
quality, has then only one-twelfth the intensity of that of 7
VirginiB.
The component stars of ^ Bobtia when photometrically
measured at Harvard College in 1883 were of 4'4 and 4"8
magnitudes, but the order of their brightness has been at
least three times reversed during a century of observation,'
Their period of revolution must be of prodigious length.
From 1796 to 1841 they appeared fixed; then a very slow
wheeling movement became perceptible, accompanied by a
diminution of distance, and it now taxes the powers of the
best telescopes to divide them.^ Their apectnim is of the
Sirian type.
' Lwtd Obtervatie^^9, 1876, p. 74.
Satvard AnnaUj vol. xir, p. 4fi8 ; Obxrvaiunu de Povlkffuxij t- Ix. p.
; Duater Mituret Mi6rovLariquei, p. €8.
" Croas]ey, Handbook cf Bmtbie SiaT$, p, 299 ; Tftmut, Jottrn. Liverpool
A»tr. Society, vol. v. p. 77.
THE SYSTEM OF THE STABS
An aoalogoaa object is a Pisciom, made ap of a fourth «i>d
ft fifib auigoitude stAr at 3* distaooe, and revolriog in a penoi
ttolikdy to be mucU lea» than two thoonad jeafR. Tht
larger certainly rahea in light, and perhaps also in ooIooe,
the RomUer oertaitily in oolour, and perbape alao in bght*
An obeenradon made by Mr. Tebbatt in New South WaW
August 22, 1887, gave a unique proof of the relative Tuit-
bility of a close double star in Virgo (OS 256). At its ooculto-
tion hj the moon on that night, the chief pftrt of the Light
went out with the disappearance of the reputed leaser «ttf,
the Lomponent whicb had of late passed for its |Htmaif
ling still for a few momeuts sepdrately but dizuty
\T«bIe.* Similar but less marked reversab had already been
noticed by 0, Strave and Beiubowski in this elowly circidat'
ing pair.'
Dr. Anderson haa alleged convincing proofs that Kridani,
now of the third magnitude, was assigned first rank by PtolMn5
and Al Sdfi/ The star is a fine pair just perceptibly revolv-
ing;* but there is nothing to tell whicb component hw
Buffered most from the ebb of light since the tenth century,
or whether it has affected both equally. The kind of varia-
bility mofib distinctive of double stars might be described aa
a tilting of the luminous balance, now in one direction, now
in the opposite, according to no settled law. It is exemplified,
^•ocordmg to M. flanunarion in 7 Artetis; it is, or has been,
ftlao present in 6 Serpeutia, 38 Geminorum, w Bootis, e Arietis,
and many other couples, most, if not all of which give spectra
of the Sirian type. Their agreement in the possession of this
particular quality of light is the more remarkable Irom its
being tije badge in solitary stars of e:[ceptional stability.
Every *' white star/' bo far known to be variable, has proved
also to be compound; and those of the Algol class are so far
from making an exception to this rule, that they rank with
the swiftest of poasihly existing binades.
Amoug the very few helium stars which have had
periods of light-change assigned to them are S Orionis and
' EtMrvarU Annali, vols. xi. [i, 112 ; xtv. j^ 433 ; Flammama, Catali
p. n.
^ Obtervatory^ vol, x, p. 381.
* KnowUdQtt vq\, rri. p. 134,
^ Obt. dA Pwlkcwa, t. ix. p.
" tmiea, lU/trtnce Cat. p, 20
VAKIABLE DOUBLE STABS
181
MonoccTotis ; and in each case on dubioue gi-ounde. The
first is widely double ; the second is the leading member of a
straggling cluster, and was thought by Winnecke in 1867
to change from 4'9 to 5*4 magnitude in 3^ 10'' 38°. It
has two close attendants^ both probably fixed. The system
has no appreciable proper motion. Both S Orionia and
S Moaocerotia are now known to be spectroscopic binaries.
The first was detected ae such by M- Deslandres, the second by
Professors Frost and Adams.
y Virginis combines the display of a firet-type spectnmi
with liability to considerable, though inteniiittent, variations
in light.^ Struck by its peculiar brilliancy, .Tune 6j 1866,
Schmidt investigated its history from the tenth century down-
ward, and concluded it to fluctuate irregularly from the fifth
to the eighth magnitude. The anomaly of such changes in
a Sirian star was brought more into harmony with other
example© by Biirnham's division of it at Chicago in 1879,
into two nearly equal components less than half a second
(0*''47) apart.^ His subsequent observations have given no
satisfactory evidence of alteration, eittier in brightness or
position, during twenty years.* This singularly interesting
system should not be neglected by the poBseasora of great
telescopes.
The variations of U Puppis in fourteen days, from 6 to
6*8 magnitude^ detected by Mr, Espin in 1883,* derive added
interest &om the strong probability that they integrate the
changes of two close components. The star is the chief
meanber of one of Struve's wide fi^ced couples {% 1097) ; after
being "elongated" by Dembowski in 1865, it was fuUy
resolved by Burnham in 1875 into an unequal pair at an
interval of 0"^80. No symptoms of orbital movement have
aa yet been derived from it, and those of luminous in-
stability seem suppressed. The case recalls the effaced
periodicity of S Monocerotis, and is, in a measure, typical.
lie spectrum is of the solar type.
A corresponding long-period star is ij Geminorum, per^
' AitT. Xtah. No. 1597 ; ffrtrvard Annals, vol xiv. p. 156 ; Qore, JTjuw-
ledgt, vol, xiii. p. 304.
» Obtervatory^ vol. iii. ji. 192. ' Oiri. Cat. p, 128,
* MonChiy Notices, vd. xUiL p. 433.
182
THE SYSTEM OF THE STABS
ceived by Mr. Buruham during a visit to Mount Hamilton in
1881, to form "a splendid unequal pair, likely to prove u)
interesting sjstem." ^ Its revolutions, shown by remeasu
menta in 1897 to be in alow progress,- will deserve the mc
attention that they are the first attributed to an Antaria^
8tar. Aa a variable^ ij Greminonim may be described as od
abortive Bpecimen of the Mira class. Its phaaes, run through
in a period of 229 days, are always ill-marked» and at tima
almost whoUy suspended. The share of the companion in
bringing about these arreats of change has yet to be de-
termined. Indeed, the more potent influence may belong Ui
a SGOoud, closer attendant apparent only through motion-shlfte
in the spectrum of the variable, detected by Professor Campbell
in 1903. Should it prove to revolve in 229 days, the fact will
be of great importance to the theory of long*period variability
The ahort'period variable, & Cephei, governs a somewhat
aimilarly constructed Bystem ; but its sea-blue satellite is
remote, and appears stationary. The primary of the chro-
matic pair, ^ Cygni, too, is undeniably variable, though its
variations are of an elusive kind. It shifts quite capriciou^y
ou the light-scale from 3*3 to 3'9 magnitude;* and recovers
by the same imperceptible gradations that it lost brightneae.
The fluctuations long imputed to the companion of S Cygni *
are probably of atmoapherio creation.^ The object, at all
times difficult and delicate, ia readUy obliterated by air-
troubles ; the more readily, perhaps, because of its variability
in colour. Struve found it of an ashen shade from 1326 to
1833; in 1836 of a bright red.'' It has since generally
appeared blue ; bub Dun^r saw it once olive, at other times
red ; and intervals of greyneea are on record. No orbit yet
computed for this pair inspires much confidence; Mr. Gore's,
kwith a period of 377 years, is doubtless the best derival
from inaurtieient materials.
The presumption of sympathy in light-change betwe
intimately united stars, although recommended by appearanc
Mtmlhiy Notices, vol. ilvii. p. 204 ; Astr. Nacli, No. 2&30.
* Gen. Cat. p. 76.
* Klflin, Astr. Nach. No, 1663.
* HeTeefael and South, PkiL Tratu. voU. ciiv. p. 331) ; oiri. p. 376.
^ Duair, Miituret Jilicriftnitriquet, p. 118.
• ^^OoloreamitiaegWigiUB," Jfnw. JUicrom. {k 297.
VARIABLE DOUBLE STAES
I; not yet been strictly tested; but the converse proposLtion,
iftt agreement in ILght-cUange implies physical conneclioD, ia
of all but eelf-evideut trutb. Two variables in Cygnus/ for
example, situated 24" apart, may safely be assumed to con-
stitute a system, their " ruddy and ccerulean " tints being a
confirmatory circumBtance. A still more etrikiug combination
presented by U Caasiopeiae and a blue companion at 59'',
rith which its atroug red glow at times contrasts splendidly.
le principal star fluctuates irregularly from the sixth to
low the ninth magnitude; the attendant from the eighth
''to the tenth. The probability of their being united by a
special tie is overwhelming. Accordant variabiUty of a
conspicuous kind is an argument for its existence to the full
as convincing as the posaeasion of a common proper motion,
The crimson tint of U Gygni, discovered by Mr. Knott in
1871 to vary from above the eighth to below the eleventh
magnitude in a period of 466 days, was described by Webb as
" one of the loveliest lq the sky." It is set off by the blue
rays of a companion at 6'', which seems to fluctuate in
colour, but little, if at all, in light. Their azure is, however,
no mere optical efifeet of contrast, since (though capable of
fading independently) * it survives without alteration the
telescopic extinction of the adjacent red luminary. V Cygni
is the only star belonging to the fourth spectral order open to
a suspicion of being in systemic connection with a neighbour.
A good many variables have satellites as to which no such
j8picion arises. Thus, the ninth-magnitude star within 46"
of the beautiful " carmine " tinted object S Orionis is undis-
tinguiflhed either hy colour or change, and they hence very
likely form only a perspective couple. The same inference
applies to three small stars contiguous respectively %o
R Cassiopeiae, R Crateris, and Mira Ceti, detachment through
the proper motion of the variable beings in the last case,
visibly in progress.
The light-changes of connected stars indicate duplicity as
le of the causes tending to produce fluctuations of a certain
ill - pronounced type. For we can safely assert, from the
k ^ h l470 = LBlaDtio 3B428.
" * Birroingham, Trofts. E. Iritfi Acad, rol. ixiri, [i. 3O0 ; GommiU, English
Maehanie^ ral. xlvi. |>, 340.
TKE SY3TKM OF THE STA£S
184
f chuacter of their ^ectn, that todst of tbe objects
tbem would shine stndiljr if single. This relation is
the more significaDt through tbe poeaibility first obscurelj
Lroi^ht into view bj Sir Norman Lockyer's meteoiitie Ui«0>7,
that rariabibtj of evei^ kind depends for its prodnctios
upon external action bj doflely drcoUting and to us invisitile
bodiM. A te«t too may be fumisbed by flnctuatibg couples
to tbe opinion that luminous insUbility belongs to a late
stage of Btellar existence. The contemporaneous origin and
similar constitution of members of binary systems axe indi-
cated to our minds as highly probable. If this be so.
development should, according to the received opinion, pco-
oeed, other things being equal, quickest in the amalleBt
m&aaes, mote slowly in the larger.^ Hence, if it were troa
that variability accompanied decline^ compauion-stars should,
one might suppo^, be far more unstable in light than their
primoxies. But this anticipation is far from being realised.
Variable primaries are more frequently met with than vari>
able satellites, tt is scarcely, indeed, too much to say that
in every undoubted case of variability in one member only of
a pair, the member it distinguishes is the principal star.
Nor, even if we were sure that the pace of evolution in
Btar-syatema in prescribed by masa, would it be safe to
conclude anything as to its distribution from observed diflfer-
enoee of brilliancy. Mass and luminosity are not comparable.
Predominance in light, as we have learned from repeated
experience, is no valid argument for predominance in quan-
tity of matter. This circum9tani« adds both difficulty and
interest to the far-reaching question of the origin, history.
and mutual relations of conjoined stars.
' Lwk^er, Prvc. Jt Socid^, voL jUf. p. 90.
CHAPTER XIV
SPBCTROSCOPIC BINARIES
The epectroHCopfc method of determining velocity has already
beeu frequently referred to in these pages. We may now
briefly explain the principle upon which it reats. Tins is
easy to apprehend, but extremely difficult to apply. Cliriatian
Doppler of Prague pointed out iu 1842 that the motion of a.
} iimi nous source towards or from the eye, or of the eye
towards or from a huninoua ft^urce. must alter the refrangi-
bility of the incident light. It must dimiuieh it if the
relative movement be of withdrawal ; it tnuet augment it if
it be of advance. For refraa|pbility depends upon wave-
lengthy and wave-length is the reciprocal of wave-frequency.
In other words, the more vibrations are pressed into a given
apace, the shorter they necessarily are, and the more re-
frangible the ray they conspire to form. But clearly, the
light-waven emitted by a body travelling towards iia arrive in
quicker auccesaiou than if it were at rest ; they are shortened
in the proportion of the rate of travel of the Inminoua object
to the velocity of the propagation of light; and being
shortened, they are rendered, ipso facto, more refrangible.
An opposite effect is produced by receding movement. The
Ught-wavea from a retreating body are lengthened ; there are
fewer of them in an inch or a mile ; and they are accordingly
rendered leas refrangible.
AJl this was fairly obvioua ; bnt it seemed questionable
whether any practical outcome conld be derived from the
recognition of its abstract truth. The doubt was removed
when Hippolyte Fizeau showed, in 1848, the feasibility of
using spectral lines as staudards of reference for measuring
1^5
186
THE SYSTEM OF THE STAES
the changes of refraugibility due to ead-on motion. Tba
rays, bright or dark, included in the spectrum of the travBl-
ling object Daturally slxifb with the whole of its light-gamut.
Bj juxtapofdtioti, accordingly, with correepondiug rays other*
wise derived, and, of coui-se, in their normal places, the
amount of their ahiftings becomes known, and heoce the
direction and rate of the movement prodaciag them. Ev^
then, twenty years bad to elapse before Sir William
HugginB made his pioneering experiments on the radial
velocities of the stars; and twenty years further before the
method was perfected by the adaptation to it, through
Dr. Vogel's initiative, of the camera.
The effects of motion on stellar spectra are illustrated in
Plate X.J which reproduces, by Sir David Gill's kind per'
mission, one of the admirable Bpectrograraa takett with the
McClean telescope by h is asaistan t , Mr. Lun t. The raja
analysed were those of a Phcenicis, a atar of ^ar type, which
retreats from the buh at the rate of 82 kilometres per
second, or nearly thrice as fast as the earth circulates in its
orbit. Let ua consider how this is learned from the photo-
graph. Five strips of dispersed blue light are included in it
A section of the solar spectrum is shown in two of them ;
the same part of the spectrum of the star adjusted to precise
correspondence with the solar prototype, appears in the
fourth strip from tlie top. The dark lines are in both
almost identical i and that many of them claim an origin
from iron-vapour, can be Been by a glance at the iron-spark
comparison-spectrum, in which the rays, obscure in the sun
and star, ahiue by direct emission. Now the iron*spectrum is
given twice : in the second, and in the fifth, or lowest strips ;
and there ia a conspicuous difference between the present-
ments of it. One is strongly displaced relatively to the
other. This displacement measures the motion-shift in the
spectrum of the atar. The iron-lines below are fiducial ; they
were photographed with the star, and served to determine its
receding speed. The liues above were photographed with the
sun, and being designed purely for purposes of identification.
are ai^anged to coincidence with the star-lines. The glaring
nature of the discrepancy between the adjusted and the
non^adjust^d iron-spectrum enables us to realise the poaai*
SPECTROSCOPIC BINARIES
187
bility of appreciating, by aimilof means, alterations of wave-
length due to yelocities of no more than one or two kilometres
a second.
Solitary atarSj lite our own, travel uniformly. Their rate
of transport does not vary sensibly from month to month,
from year to year, perhaps from century to centoiy. But
with binary atara the case is diflerent. Besides the constant
velocity belonging to the system as a whole, they circulate
round their common centre of gravity ; and the direction of
their orbital movement as regards the earth is continually
changing. Take, for instance, a pair revolving in the visual
plane. At some given moment their total speed of revolution
will lie across the line of sight. It will then be spectro-
Bcopically ineftective ; the rays characteristic of its light will
be in their standard places ; no shifts will be perceptible.
But when a quarter of a circuit from the points of con-
junction ha.s been described, and the stttrs are at the opposite
nodes of their orbit, the direction of movement, having
turned through a right angle, will be straight end-on. Hence
the spectral lines of the components will show contrary dis-
placements corresponding to the entire velocity of their
mutual ctrcUug. Two good spectrograms, accordingly, taken
at the critical instants of conjunction and elongation, suffice,
at least theoretically, both for the elimination of translatory
speed, and for the determination of the actual rate of
revolution ; and this, when the period is known, gives the
size of the orbit in miles or kilometres. Evidently, spectro-
scopic meaaui-ea at such times of visual pairs with securely
computed elements would make us acquainted with their
distance from the earth and joint gravitating power —
even if their paths were inclined, at a considerable, though
a known angle. The success of such investigations, it is
true, long seemed remote ; but it has now been achieved.
Prafesaor Hussey, in 1903, determined for B Equulei a
" spectroscopic parallas " which inspires no small confidence.*
And still more recently, Dr. Palmer of the Lick Obaervatory
has computed, from the radial velocities of a Oentauri, a
value for its parallax in all bat exact agreement with that
.derived from the most skilful heliometric observations.^ Few
^ Lick Bulletin, No. 32, Aee ante, p, 1S8.
3 lUd, No, «0.
THE SYSTEM OF THE STAES
telescopic bitmries, liowever, are circmnat&noed favoiirably
enough to invite the application of the method. The con-
ditions propitious to it a.re mpict motioti in a plane not much
inclined to the sight-Une, and considGTD.bie brilliancj in both
the moving objects. Pairs tlxat are easily divided mrely
circulate i|uickly enough for the discrimination of differences
in their radial velocities; and the most rapidly circulaLing
pairs are those most apt to defy visual separation. The
epGCtroscope, in fact, finds its opportunities just where the
telescope encounters batHing difficidtiee; and this reciprocal
relation, while it hiifi lielped to give almost indefinite et-
teneion to our acquaintanee with stellar systems, restricts
opportiuiities for combining the methods, bo as to connect
the angular measures furnished by one witb the linear orbital
dimeneioiiB obtained by the use of the other.
8(ai« revolving in or vety near the visual plane must
undergo, at any rate, partial eclipses. They are comparatively
fow; the great majority move in. patba sensibly, thou,
variously inclined to it. But hs the tilt increases, tbe
portion of the velocity available for spertroscopic measniC'
ment, because directed ratlially, obviously diminishes. Wholly
inacce^ible to it, in fact, are such couples — i^nd they may 14|I
very numerous — as circulate approximately at riglit anglee to
the li Lte of sight For those with orbits intermediately
situated, the apparent or measured radial velocity divided by
the cosine of the angle of deviation from horizontality gives
the actual radial VL>locity. If, for instance, the inclination
amoimted to 60°, only half the speed of revolution would tell
in Hue - displacements. An average value for it of about
30" is regarded as probable;^ and this would give 100
to 115 as the proportion of the observed to the true rates of
circulatory motion. But estimates of the kind serve only to
mislead if applied to inttividual systems. The safer oourae is
to admit that, in the absence of occultabion-phases, we cau
secure only minimum values for the velocities, distances
apart, and masses of binaries spectroscopically detected and
observed. ■■
They are extraordinarily numerous. Professor Campbell'
showed, in 1902,^ the probability that, among the entire
* Barr, Astroph. Jexim. toI. %i. p. 248. ^ Litk Bultetinf No,
SPECTKOSCOPIC BINARIES
189
kidtitucle of stars, one in six or seven is m constituted j and
Professor Frost added wonder to wonder by the Btatement
that helium-stars in particular yield ^ large a harvest of
binariea that the chances are nearly even whether a given
object of the kind will r^ist oc euixender to the reBolviog
powers qf the spectroscope.^ One of the moat curious facts
about close star-pairs is the prevalence of extreme inequalities
of lustre between their coiuponentB. In very many, one is
brilliantly luiniuaus, the other so far obacure that no spectro-
graphic impression can be derived from it. Some Batellites,
again^ shine dimly ; traces more or leas pronounced of their
action on the sensitive plate are perceptible ; while finaily,
twin-stars are occasionally met with scarcely distinguishable
by quantity or quality of light To this category belong ^
VtHiQ Majoris and ff Aurigso, the former detected by Professor
Pickering in 1889, the latter shortly afterwards by Miss
Maury. In both, the spectral lines are periodically photo-
graphed aa doublets, when the components of each pair, at
their " elongations " are travelling full speed ahead and aback
respectively, towards and away from the earth. The separa-
tion of the lines thus corresponds (allowance having been
made for the constant velocity of the system aa a whole) to
twice the rate of circulation, diminished, as we have ex-
plained, in proportion to the inclination of the path traversedr
Twice in the coutsb of each revolution, stars of the kind we
are now consideiing exhibit the phenomenon of doubled lines ;
at the intermediate epochs of conjunction, they give a single
spectmrn. By timing these alternations, a period of twenty
days has been deduced for ^ Ursfe^ one of four days for )3
AurigEe. Miss Maury's binary, accordingly ^ changes its
spectral aspect from day to day ; and the indicated relative
velocity of 150 miles a second shows it to possess at least five
times the massdvene^s of our sun.^
A magnificent system of this type, but in comparatively
slow circulation, is formed by Capella.* The light of a purely
aolar star, and of a companion somewhat less bright and some-
* Frost and Adftms, AHr^h. Jonm. vol. irriii. p. 383.
> Vogel, Silzungebfrichfc, BerLiD, Minih 10, 190*.
* Campbell, Lick Sulietin, No. 6 ; Attroph. Jovm. vol. z. p. UT ; Newa11«
JiMlhijf Notiat, V6t. Ix. p. il6.
190 THK SYSTEM OF THE STAKS
what leas maaaive, of the Prtx:yoa variety, are combined m
this object; and they mutually revolve in 104 days at th«
apparent or tuinimum rate of about seveoty luilea a Beconl
The parallax of Capella, though email, la assured ; it gives t
distauce of forty light-years, wheuoe we can infer that the joint
lustre of the components exceeds more than a hundredfold th^
splendour of the aun.
Gouplea coiiaisting of two bright membora are much
of detection than those of which one is obscure. Duplicated
rays in a Bteltar spectrum attract attention even on a crowded
plate exposed with an objective prism, iu a manner to secure
wholesale records ; but the oscillations of single lines reqaire
the aid of a slit and a comparison-spectrum to make them
evident. They evade notice unless the stars are separately
studied. Yet, despite observational difficulties, about 75 per
cent of the apectroaoopic binaries (to the number of nearly
130) known at the end of 1904 have sensibly obscure com-
pauious. The first noti-eclipsiug star recogniaed as double by
the mere swinging to and fro of solitary lines was Spiai
(a Virginis). Dr. Vogel thus determined in 1890 its revolu-
tion in four days round an attendant later shown to be very
feebly luminous. Both members of the stately visual pair,
Castor, on the other hand^ circulate swiftly round bodies giving
no sensible light. The quaternary system thus formed is of
unique interest. Dr. Curtis^' the discoverer of one of the
dark attendant stars (the other was found by Belopolsky in
1896), has determined for it — provisionally assuming tha
correctness of Doberck'a elements — a spectroscopic parallax of
O''*05, corresponding to a light-journey of 65 years, and
implying a total mass for the four constituent globes nearly
thirteen times that of the sun. But it seems to be very
unequally apportioned. One of the revolving pairs exerts thrice
the attractive power of its companion, while emittiug only half
as much light. The gravitational primary is the visual satellite,
and vice versd. Only through the association of telescopic with
spectroscopic measures, practicable by a rare exception for
Castor, can inferences regarding the mass of bright and dark
pairs become legitimate. Nothing definite can, under ordinaiy
circumstances, be affirmed oa the subject. For one com-
' Liek Bulletin, "So. 70.
SPECTROSCOPIC BINAEIES
m
ponent beiog iuvisible, the size of their relative orbit remains
absolutely undeterrained ; and the size of the relative orbit is
a datum esaeubial for computing the mass of the system, or
even a minimum value for the mass, which, in our ignorance
as to the be of the orbit, is the utmogt we could hope to
arrive at. The relative orbit, aa already explained, is the
Biim of the separate orbits; or, putting it otherwise^ the path
described by one &tar round a companion taken to be at rest.
Trom its span, in conjunction with the period, the noaas
of the pair la dcdncible. There is no means of learning it
without knowledge of these two elements. The masses of
bright and dark pairs can then^ aa a rule, only be guessed
at with the unwarranted help of arbitrary hypotheses. That
of Spica> for instance, has been estimated at 2*G times the
solar mass ; but the value has only the authority of a plausible
conjecture.
From the measured movements of stars with shining com-
panions, as already explained, the least passible amount of
matter present in each system may be learned. The orbit spectro-
scopically determined being the foreshortened representation
of the orbit actually traversed, is smaller in an unknown
degree ; and the mass of the moving bodies varies aa the cube
of the orbital radius. The error of mass- determinations hence
grows in a tripliciLte ratio to the eiTor of the linear dimensions
directly obtainable. Minimum values, nevertheless, are better
than none at all ; they fti a limit of great importance ; and
for one species of crypto-double stars they may almost count
as absolute values. These are eclipsing pairs in which both
eomponente are bright. Y Cygni is a favourable example.
The opposite movements in its system may be speetroscopically
elicited ; the size of the relative orbit will thereby be given ; and
since its plane is iixed by the occurrence of a twofold eclipse,
^he joint mass of the components can be ascertained without
ubious asaumptioaa. Several Algol -variables appear to be
Similarly constituted; but their investigation awaita the
leisure of overtasked spectrographers.
Few compound objects are more inviting to research than
stars variable in short periods, though not through eclipses.
Six have already been detected && spectroscopic binaries; and
the resolution of all may be regarded as de[)ending merely
m
THE SYSTEM OF THE STAIiS
upon time and facility. The extreme interest of the qucsti
connected with them is exempli^ed in ^ Oominonim^
radial velocity of which was found by Profefisor Campbell
b© subject to a double periodicity, due, he surmised, to
influonco. of a second dark satellite ; ^ yet the stable const]
tiou of n triple system on the indicated conditions seems
a hopelesa task. Again, * Pavonis varies from 3*8 Uj
5'2 magnitude iti a mean jjeriod of nine days, affected,
according to Mr. Roberts's observations,^ by an inequality
amounting to ten hours, comprised in a cycle of eight yeara
The duplicity of the star was ascertained by Dr. Palmer in
1904;^ and before long an answer may be furnished to the
critical incjuiry whether the disturbance of the light-period
is reflected, or perhaps originated, by a disturbance of the
gravitational period.
Nor IB it short-period variables alone which yield to the
motioU'test. The division of stars that fluctuate irregnlarlj",
or in long periods, is of not infrequent occurrence. Such ia
1} Geminoi'um, one of Burnlxam'a unequal pairs, raised to a
higher plane of complexity by the addition of CampbeL'a
spectroscopic attendant.*
A period of about forty days is partially conformed to by
the ebb and flow of luminosity in u Herculia, a helium-stAr
visible, even at its dimmest stages^ to the naked eye. Detected
aa binary by Mr. Adams* at the Yerkea Observatory, it revolve*
round a seemingly dark companion at a high speed, but in a
period which has still to be ascertained. The investigation
of the system constituted by e Aurigse is alflo incipient
Dr. Vogel's resolution of this object in 1902 into a bright
unequal pair, with a relative velocity in tlie line of sight of
nearly twenty-five miles a second, will be iu the minds of our
readers.^ Now « Aurigae ha.s, during the greater part of a
century, been remarked for slight phases of light-change held
to be quite capricious in their occurrence. Should Dr.
Ludendorff's regolarisation of them be verified by future
observations, their twenty-seven year period will rank as by
^ Astroph. Jounk, toL xiii, p. M.
^ Hd does Bot yilBtio implicit confideuco in them, Astr. Joum, No.
» Lick Bu-lirtin, No. flO. * Ibid. No. 20.
" Jttrapft. Joum. toL ztiL p. 261. * 3e« anU^ p. 10£.
SPECTEOSCOPIC BINARIES 193
/he longest that can be ascribed to &ny form of stellar
-change. And it will be of great importance to correlate
it, if possible, the star's period of orbital revolution.
3 is, perhaps, no object in the heavens of mote pregnant
est than this variable spectroscopic binary.
13
CHAPTKK XV
ITDUXPltE ETTABS
Tuz further r^olvability of a great nuBuy double stars iB
one of the most cuiioua resulta of modem improvenieDte in
the optical means of obBerring them. With every additiao
to the defiaiog power of teleeoopoB, the visible complezily
of stellar eji'atema has increased so rapidlj as to inspire a
Buspicion that simple binary combinations may be an excep-
tion rather than the rule. The frequency with which those
token to be such have yielded to disintegrating scrutiiiy
Buggeets at any rate some innate tendency, indicating that
the duplicity of etara is no accident of nebular condensa-
tion, but belongs essentially to the primitive design of
their organisation. Although we can never become fully
acquainted with all the detailed arrangemeuta of stellar
syBbemfi, we are then led to suppose them far more elaborate
and varied than appears at first eight E^h, we cannot
doabt> IB adapted by exquisite contrivances to its special end,
reflecting, in its untold harmonies of adjufibjuent, the Supreme
Wisdom from which they emanate.
The continuance of the proceas of optical dissociation, begun
by the splitting up of an apparently aimple star, sometimes
shows the primary, sometimea the eatellite, not unfrequently
both primary and satellite, to be very closely double. Ternary
ayatems are accordingly of two kinds. In one, the smaller
ebar conaiats of two in mutual circulation and concurrent
revolution round a single governing body ; in the other, an
intimately conjoined pair guides the movements of an un-
attended attendant. The planetary type of construction is
uncommon or unknown. No star has been ascertained to
MXTLTTPLE STAIIS
195
possess two or more companions circulating co-ordinately.
Groups poeeibly indicating such a disposition of parts exist,
but perspective may have a share in producing them. The
variable S Monooerotia, with its two client-stars, is an example.
Another is mentioned by Dr, See. Four extremely faint com-
panions, at distances between V &nd 39" from a si^th-
magnitude star in the Poop of Argo (Cord. Q. C. 10534),
have been detected by him and his predecessors. The group
is thus commented on by him : — " Quintuple ! Probably a
complicated physical system ; the only stellar system I know
of OGnstructed on a plan in any way analogous to that of the
planets/' ' There is, however, at present no proof that the
artaagemeut may not reaultj at least in part, from the chances
of perspective juxtaposition.
Among tlie most interesting triple stars of the double-
satellite description is the brilliantly coloured 7 Andromedffi-
The original components, of third and fifth magnitudes 10"
apart, remain in statu quo since they were seen by Father
Mayer in 1777, but their secular journey together over an
arc of 10" establishes the genuiuenpsa of their relationship.
In 1842 the sea-green companion wag found to be itself double.
With the 15 -inch Pulkowa refractor. Otto Struve caught
sight of a thin black line (representing probably a gap of
Home thousands of millions of miles), dividing it into two stars^
the fainter of about sixth magnitude, which within fifty-five
years completed a revolution in an orbit not much less eccentric
than that of y Virginia.^
A pair in some respects similar, but much fainter, is
attached at about the same appareut interval to the lustrous
white star Eigeh An excessively difficult object at the time
of its detection, it later became impossible. Its elongation,
suspected both by Burnham and Herbert Sadler in 1871,^ was
verified at Chicago and Mount Hamilton in 1378-79. Then,
for nearly twenty years, no sign of duplicity could be elicited
from it.* Change^ under the circumstances, seemed much
more probable than error ; and its rapid progress was indicated
by Professor Aitken'a reobservatlon of the sapphire attendant
* ^str. Jt»*rn. No, 431,
* W. J. Huasey, iVW. Lick Ohurvaiory, vol. v. p. 4&.
* A^r, Begisier, vol. itlu. p^ 16, * BumLom, Otn. Oat. p. 69,
OH
THE SYSTEM OF THE STABS
upon RigeU* s» pslpoUy doaUe in 1898. Xevenh«ka,
^fUr two yeuB, (he enttve satellite wu ftg«m undiaoeniibk'
The riddte of ita exifllanioe maj be finally aoJved by the tid d
a «pBctro|^niphic appflffstus of gteat light-collecting power.
A ternaiy groap, ooim^iaatidiiiig to these two in plan hm
gioatly enlarged in ai^ular scale^ oooiinsto of a 4*5 magnitiMh
fftar^ deeignabed bj FUmsteed 40, by Bayer o* Eridani, wiifc ■
faint and iar-away double satellite already referred to,* all
thtiee diaoovered by Herachel in 1783. The aflBooiation of the
pair with the large star at bo gr^t an interval as 92* would b»
improbable^ were it not certified by itieir poeseesioQ in oommtn
of an exceptioaally swift proper motiotv Aa advance during
the laat century over a spaoe nearly equal to a quarter of the
raoonV diameter has modified their relations only by a trifling
approach to their primary of the depeodeat &tars, due perhaps
to slow circulation round it in an orbit presented edgewise
to our flight
They have, in the meantime, almoet fini&hed a circuit of
one another, and will have completely finiahed it within about
160 years from the date of their detection.' And since their
distance from the earth has be«n measured, the real size of
their orbit and their joint mass are also known. We find then
that the average interval between them is thirty-eight tim«
that separatitig the earth from the sua. &o that (their path
being only moderately eccentric) they never approach aa near
to each other aa Keptune does to our oeotral orb, which they
together surpass 1"6 timee in gravitative power. But in their
place, from which light reaches U6 in twenty years, the stm
would shine as a fourth-magnitude star, while they combine
into one of only ninth magnitude. Their feeble luminosity
thua once more forces itself upon our attention, and compels
US to reflect upon the possibility of whole aystems existing in un-
impaired mechanical perfection, but wrapped in perennial dart*
neea. For what purpose eiisting, who can tell ? The flight
of our thoughti9 is short and the ultimate aims of the Maker
are remote. Attempts to compass them are foredoomed to
failure.
' Pttp. Attr. December 189&, p. 585.
' Liek BulUtin, N«. II, " See ante, p.
* Bttmliiim, Monthly AbCieu, vol, Uii. pi. 478-
iMULTIVLE STARS
197
Double primaries occur as freely as double satellites \ and
'iheir comjnon centre of gravity presumably conatitutea the
focua of attraction for their remote attendants. Castor
Bplendidly illustrabes tliia plan of conatruction, carried out on a
Taat scale in its system, which includes five members; the
locid components, a far-off captive star borae in their train,
I'And the obscure adjacent masses disclosed only by their
ctroscopic eflects. Another specimen is e Equulei, one
Herschel's pairs, the larger member of which was again
ivided by Struve in 1835. The feat had become possible
3ugh the progress of orbital motion, the continuance of
ioh has since rendered it easy. Signs of circulation in
7'5 magnitude star at 11"^ are scarcely, if at all,
eptible. Yet it is an undoubted satellite of the close
iple.
The movements of the third star (of T"! magnitude) in
lie ternary combination f Scorpii, seem to progress in an
pposite direction from that of the close double star which
controls them at an apparent distance of 7" ; but their nature
and method are etill imperfectly developed. The primary in
this system consists of two fifth-magnitude stars, formerly just
eeparable with a gootl 4-inch telescope, but now only 0'*'7
ajort. The orbit assigned to them by Dr. See ^ approximates^
in an unusual degree, to a circle, and ia traver&ed in 104 years,
Their spectrum is of the Sirian type. The eighth-magnitude
companion of e Hydrte has described, since its discovery by
Struve in 1825, an are of over 40", at a distance of 3". Its
blue tint ia charmingly set off by the warm yellow of the chief
star, divided by Schiaparelli in 1888 into a difficult pair re-
volving (by Professor Aitken'a elements) in leas than sixteen
yeara PoMibly, the process of resolution has not reached its
term; for Dr, Curtis measured, on 1900, fluctuations in the
radial velocity of the leading component. They more probably,
however, depend upon its revolution in the visual orbit,* Un-
doubted spectroscopic binaries nevertheless frequently occupy
analogous positions. Besides the systems of £* Ursae Majoris,
and If Geminorum, those of f Ura^, ^ Scorpii, and tc Pegasi
are thus composed. As a wide pair, k Pegasi was noted by
' FlMUDarion, Catalogw, p. 139. » SltlUxr Syjfem*, p. 178.
' LiciBulUtin, Noa. 4, U.
Ida
THE SYSTEM OF THE STARS
Herschel in 1786, The queatlott is still open whether hb
eleventh-magnitude companion has any physical cotmection
with the nuclear group. This consists of a fairly equal piur.
recognised by Borahom in 1880/ and found to revolve in
11 '4 years; together with an unseen companion to one of
them, detected by Campbell in 1900, and completing ite
circaits in about six days,*
The relations of tlie stars compounded in ^ Scorpii are no
less remarkable. Two, of respectively third and sixth magni-
tndes^ were first observed by Herechel in 1779; the third,
discovered by Burnham a century later, makes with the
primary an extraordinarily difficult, unequal pair at 0''"96.'
A fourth has been Bpectrographically measured by Mr. Adama'
It is a lustrous object with a helium spectrum, and revolves
at high speed in a period estimated at 6** 2l\^ No visible
relative movements have yet been perceived in the ^tem of
y3 Scoipiij which nevertheless asserts its organic unity by the
harmony of its advance througli apace.
One of the moat curiously interesting of all the stellar
systemfl known to us is ternary from an optical, quaternary
from a physical point of view. It is composed of one
obscure and three bright members, all in comparatively rapid
mutual circulatiou. The division of f Cancxi, by Tobias
Mayer in 1756, into a fiftli and a sixth magnitude star about
5-J-" asunder was tlie preliminary to Herschel's further ajujlysia.
" If I do not see extremely ill this morning," he wrote ou
November 21, 1781, "the krg© star consists of two,"* Thifi
was the earliest example of the decomposition of a double into
a triple star. The next distinct view of these close objecte
(called for convenience A and B, the remoter star C) was ob-
tained by Sir James South at Passy in 1825, but Struve's 9-inch
Fraunhofer showed them easily, and they have never since been
lost eight of. Eeohaervation at once rendered patent their
swift movement of revolution. Before the close of 1840 they
had, by resuming the positions in which they were originally
* Gemral CaUiiosuet p. 231.
' AairopJi. Jmi-m. toI, lii. p. 267-
* Monthly Noiiees, vol. xL p. 100 ; Geiierat Catalogve, p. 14S.
* Aatroph, Jvum. vol. xiriii. p. 69.
" Lowgll ObKrvaiiirti Bulletin, No. 1.
* Croasley, Kandbaok, p. 247.
MTTITTPLE STARS
199
observed, authoiitratively declared their period to be not far
from sixty years. And their orbit lies iu a plane bo nearly
square to the line of sight, that foreshorten ing takes little
effect upon it, and occultations are hence imposaible. Although
the maximuia inteiTal between the stare stsarcely e^cceeds one
second, and the nLinimum interval ia no more than 0''^'2, they
never doM up beyond the dividing powers of firgt-clas^
instruments.
But the orbital movements of the couple A B make only
port of a complex scheme of displacements. " This atar /' Sir
John Herschel remarked in 1826, "presents the hitherto
unique eonabination of three individuals, forming, if not a
Bystem connected by the agency of attractive forces, at least
one in which all the parts are in a state of relative motion." ^
He added that, if really ternary, its perturbations must
present ^' one of the most intricate problems in physical astron-
omy " ; and Professor Newciomb holds it probable that the
laws of motion in such combinations must, in general, be
" too eompUcat^d to admit of profitable mBtberoatical investi-
gation." "
The star C apparently retrogrades round A B at an
average rate of half a degree a year, indicating (if maintained
with approximate uniformity) revolution in a period of 600
or 700 years. But this average rate is subject to very
remarkable irregularities. The path traced out in the sky,
far from being a smooth curve, is looped into a series of
epicycles, in traversing which the star alternately quickens and
slackens, or even altogether desieta from its advance, while
increasing or diminishing, by proportionate amounta, its
distance from the centre of motion. This anomalous
behaviour, detected by M. Flammarion in 1873,* was both
detected and interpreted by Otto Struve in 1874.* The
vagaries of the third component of ^ Cancri proved, from his
investigation, to be very far from unmethodical. The accelera-
tions which they included were shown to be perfectly com-
penaated by retardations, and to be accompanied unfailingly
by expansions outward of the parts of the track where they
^ PhiL Trana. toL exvi, p. 32G.
» The Stars, p. 181. = Catalopif, p. 49.
* Cojfiptu Stndus, t. Ixzij. p. U63,
200
THE SYSTEM OF THE STAHS
OGCurred, while contructiona iuw&rd attended slackened m<xv^
ments. An explanation too was hazarded^ the Bafastantiftl
truth of whicli was attested by M. Seeliger's eluborftte Kaearcliee.^
It seems then that the atar G is merely a satellite to «
dark body round which it describes, in 17^ ye&is, a Utile
ellipBe with a mean radius of one-fifth of a eecond. Together
this singular pair circuits, or, more probably, is cinsuited bjr
A B, the iuviaible disturbing body being the moBt tnas&ive <d
the system- If this be the case, it is also^ of oouree^ the moet
nearly alaticiiAry, and should be regarded as the centre roond
which the lucent trio revolve — an arrangement hinting to as
that the collocation in the same orb, familiar to us in cIm
solar domain, of the functions of rule and light-givingj mijt
on Qccaaions, be dispensed with. An anti-Copemican system,
at any rate, appears to be to some extent exemplified bf
^ Oancri Here a ooolj dark globe^ clothed possibly with the
vegetation appropriate to those strange climes, and plentifully
stocked, it may be, with living things, ia waited on, for the
supply of their needs, by three vagrant suns, the motions of
which it controls, while maintaining the dignity of its own
comparative rest, or rather of its lesser degree of movement
For the preponderance of this unseen body cannot approach
that of a sun over its planets ; hence its central position ia by
no means imdisturbed. We must not forget, meantime, that
its existence is to some extent hypothetical. Mr. Bumham
thought it an evanescent creation of accumulated micro-
metrical errors;^ and Professor Frost in 1904 failed to elicit
any spectroscopic evidence of the eighteen - year period
ascribed to the third star.* The close pair (according to
Pickering's calculation) possesses nine times the solar emissive
power relatively to maaa ; and all the three visible components
show spectra of Sirian quality. Their real differences of
magnitude, too, Heem to be slight, although at times
exaggerated by relative variability. The entire group is
^ SiUungalrricht'T^ Wiem Bd. Ixxiiii. Abth^ 2, p. 1016; £fcnk9eKriJtm,
Munich, Bd. ZTii. Abth. I, 1SS9; Barzcr, Attr. Naeh. No. 2764; ObstrviHory,
vol. sii. p, 116,
* MoiUhly NoticM, April 1691, November 1B92 ; Aatr, arid AelTV^hyna^ toL
lil. p. a72 ; SeeligGr, ibid. voL xiii. p. 802 ; A$tr, Naeh. No. 31fl& ; ^zungsb.
Bt^ytf. Akad. Bd. xxiT, H«a. ill. 1S94.
* AMtroph. Jvurn. vol xix. p. aSG.
MULTIPLE STABS
201
irted through Bpace at the rate of IS"" a century^ but
distance from the earth ia unknowru
A quadruple system of remarkable type ia formed
f Ursffi Majoria with three variously related bodiee.
iden its spectroBCopic and telescopic attendants, the one aa
;e aa the other is sedate in its revolutions, it clauns the
escort, on it& indefinite journey onward, of the fifth-magnitude
star Alcor» the two making the combination popularly
designated the *' Horee and Bider." Since the interval
between them is of 11' 30", they can easily be dietinguiBhed
with the naked eye ; neverthelesa Alcor, totally overlooked by
the GreekSj was regarded sis a test-object for keen eyesight by
the Arabs. Its gradual brightening is thus strongly sug-
gested.^ The probability that Mizar and Aloor mutually
revolve ia strong, but not overwhelming ; their connection
nUffht be otherwise explained. If they do, their annus magnus
must be of enormous, to our ideas of interminable length.
Heal quaternary stars are often self-discriminating ; their
arrangement into two adjacent couples asserts physical con-
nection more strongly than any possible distribution of three
stars can do. And in effect, several perspective groups of a
single star with a genuine pair, such as S Equulei, 35 Pegasi,
7 Tauri, and ^ Delphini, are visibly in course of being dis-
solved by proper motion, while no " double-double " combina-
tion has yet given signs of breaking up.
A representative specimen of the latter class offers itself
in c Lyrse, a atar of the fourth magnitude, a little to the
north-east of Vega. Exceptionally keen eyes show it as
double, and one of the brilliaDt surprises provided by the
heavens for Sir WiUiam Herschel was that of finding each
component further diviaibk. The discovery, though beautiful
and interesting, was easy ; all the four stars can be seen with
a good 3-inch telescope. The "preceding" pair, or that
which crosses the meridian first, is distinguished a^ e^ the
" following " pair as f^ Lyr^ ; and Flamsteed attached the
numbers 4 and 5 to them respectively. The former consists
of a fifth and a sixth magnitude star 3" asunder; the con-
stituent stars of €^ are nearly equal (5*3 and 5*5 magnitudes),
and are set a little closer together (at ^"■45). Their revolu-
* FlunnmrioGL, Caialogat, f, 75.
THE SYSTEM OF THE STAItS
tiona, too, appear to be performed about twice as ijuicklf tf
those of the neighbouring couple. From the shifticig of th(
relative aituatioua since 1779 by more thaa half a rigi
aiiglo, their period maj he estimated at about 800
while that of c^ Lyrse is likely to exceed on© thousand,
practicabilitj of computing either orbit is still remote.
The small common proper motion (9" a century) of
t^ght coupler affords poaitive evidence of their unioa Into
va^b system. At their unmf^osured, perhaps immeasanUs
dxatance, the gap between them of 3J' may well stand ia
a ch^m costing light itaelf Home months to bridge ; yet the
atreas of their mutual gravity reaches across it, compelluiii;
their circulation in orbits bo spacious that a sirtgle round d
them must occupy an era of no insignificant duration^ even in
the life of a star. The four star* of e Lyrje give a spectrum of
the firat type, combined, in the leading couple, with a decided
cast of yellow. But thig is often the case with double stars.
" A miniature of e Lyrse " ^ is offered to our regards in
tf SeorpiL This is perhaps the most beautiful quadrapls
group in the heavens, from the narrow limits within which
the brilliant objects composing it are crowded. As a widi
doable it was noticed by C. Mayer in 1776 ; after seven^
years the smaller star was divided by Mitchel at Cincinnati,
and the larger one of fourth magnitude yielded similarly, iii
1874, to the insistence of Burnham. Both pairs share with
several neighbouring stars a slow drift through space.^ They
are 41" opart, and have as yet developed no systemic
movements.'
The sixth -magnitude star 86 Virginia may be said to
consist of a double primary with a double satellite at 27".
Full acquaintance with the group was made through Burnham'a
amdyais of one of Struve's " rejected " pairs. Its internal
relations will need time to develop/ A quaternary combina-
tion of p^uliar interest was detected by Mr. Innes in 1897.*
It consists of two close pairs, k Toucaui and Lacaille 353,
separated by the wide interval of 5' 20*^; yet, notwithstanding
^ FUmmftrioH, Caealoffve, p, 96.
* Iqdsa, Re/erenc£ Catahgue, ■p. 157 \.
* Bamhfttn, ffer*. Cat. p. 149, * Ibid. p. 128.
* MimihJy Notica, toL LriL p. 456 ; Re/. Cat. p. 10 a.
MULTIPLE STARS
203
th« antecedent improbability of their connection, it is emphatic-
ally asserted by the unanimity of their rapid rate of travel
across the sphere.
Eighteen "double-double" star-groups — one (% 2435)
with a span of no more than 15" — wete enumerated by Bum-
bum in 1882/ and three have, since been added by Hough
and Innea.* They perhaps exist more numerously than we
have as yet any idea o£
A " double-treble " star, so-called by Herschel, has been
the subject of numerous succeaaive discoveries. With the
slightest optical assistance tr Orionis, a star of 3*7 iniignitude,
just beneath the middle star in the belt of Orion, separates
into two wide and unequal components, each of which was,
October 7, 1779, perceived by Herschel to be triple.' As
usual in such cases the process of resolution was continued,
and the assemblage was described by Barlow as " double-
quadruple, with two very tine starB between the sets/**
These last, however, are not unlikely to be mere optical
associates. To this intricate group Burnham added a further
element of complexity. At Lick, in the autumn of 1888, he
found its chief member to be formed of a fourth and a sixth
magnitude star, a quarter of a second apart, and yielding, after
ten years, signs of mutual circulation.^ The disclosure, like
some others, raised a question as to the point where stellar
subdivision can really be said to cease, That it is not where
visual limitations interfere with our recognition of it was
emphatically reasserted in 1904 by Professors Frost and
Adams's spectroscopic discovery that the primary of Burnham's
pair is intimately, though invisibly coupled with an obscure,
tuafisive body.
The essentia! character of tr Orionis is that of being made up
of two diatinct, yet evidently connected knots of stars^ and the
same knot (S 762) *" contains all the four brightest componeata
These ditfer, and perhaps vary in colour, and their influence
may be assumed to predominate in this remarkable system.
* Obaenxitofy, vol. iv. p. 176.
' Astr, Nach. No, 377a ; AF^tUhly Noiicts, vol. Itu, p, *W.
■ PAH. frniM. Tol. liiii. p, 124.
• Smjtti, Ci/cte o/Otl Ob;eci9,vd. 1881^ p. IBS.
* AHr. Naeh. No. 2875 j Oeti. Gat. p. 68.
* Strar6> Mens. Mier&ai. pp. 149^ 24fi.
THE SYSTEM OF THE STABS
The multiple star 45 Ijeporis ia organised on apbnla
definite tbao thftt governing tb« stin>cture of tr Ononis. I
visible to the naked eye> it ooosista of four principal and
puboTvlinate members, ooccessirelj diaeovetBd t^ Sir
Herachel aud Burnham.^ One of the st^iBy of e^tb
ttide, stands ou t through its ruddy colour firom its
coinpaiiioii&' The entire group of nine objects covob
extent of 125".
The nebular relations of double and multiple 9tais
noticed with surprifie by Sir John Herachel at the outset of
career.' Although admitting without hesitation their ph
character, he was without the means of establishing it
made available^ aud coold enpport his conviction only b^
utter improbability of such collocations as he pointed out
fortmtou£i Thus, a close, minute stellar couple is planted
the exact csentre of a faint round nebula in Leo (New Gen.
Cat, 3230); and the same kind of coincidence recurs twice
in the southern constellation Dorado (K.G.C. 1732, 1961
Two pairs in Sagittarius, each set in the midat of a nel
(N.G.C. 6589, 6590) may from their contiguity be
pected to constitute one system; and two ninth- tnagnitude
Btara at 15", marking very nearly the foci of an elliptical
nebula in the same region (N.G.Q 6595), are certainly not
accidentally projected upon it. " One of the most curioui
objects in the heavens " (according to Sir John Kerschel),* is ft
trio of stars arranged in a minute equilateral triangle, relieved
upon a shield of milky light (K.G.C. 1931) j and its
siogularity was enhanced by the duplication, under Biimh&m's
gaze in 1891, of one member of the combination.^ By the
same obaorver, again^ an eighth -magnitude star riglib at the
heart of a round nebula in Monoceros (N.G.C. 2182) was
divided, also in 1391, into a delicate pair,'^ the remeasurement
of which after twelve years, by Professor Aitken, gave evidence
of slow circulation. Of circulatioDj we remember with surprisa,
conducted in a nebulous medium, and therefore presumabl
t
' Burnbam, Mtmnri H. Attr. Sec. toI. xUt. p. 238 ; Attr. Nach. No, 204S ;
i^MTvatory, voL iv- p, 177 ; Otn, Cat. p. 68,
^ O. Kfiottr OhatTWitiir^f^ T&L iv. pp. 1S4, 212.
* Mijrufirt B. Afir. Soe, vol. vL p. 7&. * /Net toL uL pi &4,
' ffm, OtU. p. 66. • Ibid. p. 7&.
MULTIPLE STARS
205
ipeded. But if eo, the syatena coiJd not be a pennanent
and a temporary star should result from its collapse.
difficulty is intensified by the consideration of many
slUl more noteworthy instances of the asaociatiDQ of
ipoedte stars with nebulae. The whole framework of the
\t nebulous structure in the sword of Orion seems to rest
the stellar group designated 0, or rather 0^ Oriouia ; for
is a second & not far off. itself a wide double star ; and
two together form, to the eye, one diffuse oKject, singly
logued by Ptolemyj Tycho Bralie, and Hevelius. But it ia
itb 0^ exclusively that we are at present concerned.
On the very slightest teleacopic persuasion, it allows itself
be eeea as quadruple. The four atara into which it divides
severaUy of fifth, sixth, seventh, and eighth magnitudes,
greatest interval between any two of them not exceeding
None of them is in visible subordination to any other ;
By stand, it might be said, on an equal footing, at the four
lers of a rudely quadrilateral figure, or " trapezium.*' They
itain their places, too, botli absolute and relative, with
rigidity. After two and a half centuries of observa-
1, no shifting of them can be detected. They are hence
bIj to be at a prodigious distance from the earth.
The rule that such groups seem more crowded as they are
tt«r seen, has not b«en infringed here. A fifth star of the
renth magnitude was added to the company by Struvcj
|ovember 11, 1826, and a sixth, still fainter, by Sir John
erschel, February 13, 1830. Both of these, though closely
Ijaoent, each to one of the larger stars, share their apparent
immobility.^ Variability in light has often been ascribed, and
as often denied to them. Burnham'a experience is against it;
yet the curious fact that Itobert Hooke saw the fifth star in
16G4 with a non-achromatic three and a half iuch tele^ope,'
is strongly indicative of temporary brightening; and M,
^omas SolfL was convinced that the sixth star was shining
itU unusual lustre when he observed it, after an interval of
months, on Kovembcr 10. 1901.^ Individual and
' Burubam's meiLBurea seem decUive oa tUis [K>iiit. Sea Iftrmoirs R. Astr
Soc, voU. xlir. p[x 203, 2S7 ; xIviL p. ^14 ; ifonXhiy H'otiut, vol. xlix. p. 2U7
I*ubt. Lick Obttrwttory, vol. ». p. 46-
' Jiieroyrapfita, p. ^2. ■ AstT. AbtfA. No. a7SL
206
THE SYSTEM OF THE STARS
atmoapherk conditioua are, however, largely conoemed in such
perauasiotis ; when they conspire favourably, it is weU asoor-
tained that all six of the trapedum-etars con be made out
with achiomatics or reflectois three to four inches id apeitme.^
Hooke^B observation can scarcely theu be said to demonstnte
change.
Further members of this group have, at varioiis times,
been half-seen, balf-Burmisod j but their existence, alwavs
problematical, has been disproved through the application of
the Lick thirty-eix inch^ for the three new stars perceived
feom Mount Hamilton by Alvan G-. Clark and Barnard could
certainly not have been detected vath any less powerful
instrument. Two of them lie within the trapezium ; th«
third, a double star of extraordinaiy minuteness and difficultr,
Bunard
• F
X
AlnoCUrk
a .
* B
Pio. ST.— fitan of Ibe TnpfKiaiii.
just outside it* Their positions are shown on the accom-
panyiug diagram (Fig, 27) where G and H represent two of
the recently discovered stara, the third, as an imperfectly
determined object, being provisionally marked with a cross.
The fact that the leading star in the trapezium has
proved to be a spectroscopic binary is not the lees astonishing
becauae of its congruity with much that had previously been
learned. Sir William and Lady Huggina recorded in 1897'
the ^XAt eigiLB of its dupUcity ; they were assured and defined
by the Yerkes measures in 1904.* Ita nature is moreover
shared, and attested through a far larger variation of radial
^ Webb^ GaI, Olgtcts. p. Sfl7.
* Burnham. MoTtthty yoiices, vol. ilix. p, 352 ; ji3fr. Nadu No, 2930.
' Atiroph. Joum. vol. vi p. 322.
* Frost uid Adima, Udd, toI. xtx. p. 153.
MTJLTTPLE STAES
207
ed, by ^ OriomB^ which crof^ses the meridian six seconde
itter than the septuple object bo the westv Half a degree to
south lies t Ononis, a triple star immersed in an ouLlyitig
ikred of the Sword-handle formation. Here again visual has
an followed up by spectroscopic resolution. The diffuse
rk lines in the prismatic ligbt of t Ononis oscillate to an
ttent indicating to and fro velocities of 60 kilometres (37^
liles) a second. And by siraikr tokens^ the nebulous stars S
[onocerotis, 5V Cygni, and <r Scorpii are known to be swiftly
Bulating couples. The investigation of Hystems so singularly
cumstanced will doubtless serve to elucidate the relations of
je glimmeriog fields of apace to maasea of matter traversing
lem. Should they appe-ar to slip through unopposed, our
ieas ae to the essential properties of material substance will
ive to be considerably modified.
In one other great nebula besides the Orion structure a
'multiple star seems dominant. The nuclear group in the
thM nebula (N.G.C. 6514) consists of a close quartette
covering an angular extent of only 19', with two extremely
faint additional stars discovered by Professors I^ngley and
Holden. Complete apparent fixity characterises the arrange-
ment
The frequent association of compound stars with nebulje
is no mere isolated fact. For they pass by insensible degrees
into star-chistera, the nebulous affinities of which have been,
ja many case^, established with the aid of photography. The
conjecture is even plausible that the formation of a multiple
stajr in a great nebula represents the initial stage of the
development from it of a crowded cluatre, minor nebulae giving
rifle to leaser groups ; and if objects of the kind have not yet,
BO to Speak, been turned out of the workshop, it is no wonder
that fragments of their raw material still cling round them.
Compositeness of structure may thus measure primitiveness of
condition^ illustrating, though to us dimly, the sequence of
Divinely decreed chatigos by which cosmiejil order is gradually
more and more fully disengaging itself from the " loud mis-
of chaos.
&TAB8 joined tc^tber ia sjntems peremptoriljr aaaerC m conuaon
origia. Tbeir companioiiBbip U not due to ch&nceL Bodies
moving independently in space may circuit one anoth^ !□
a hj^rboUe orbit ; but the event ahould be noiqnjei They
cun never meet again. Permanent capture is pnurtioUly out
of the questioiL The mterveatioa of a third body would be
Inquired to bring it about, and the tbiid body should be
critically situated, and of enormous toslsr to produce th€
neeowaTy amount of retardation. The poflaibility of a ctmaaH
aplffoftcb having led to an indissoluble unioti is indeed too
remote to be worth counting. Multiple etais, we naay rest
asBured, were such potentially from the first.
Yet the manner of their origin remained long ao im-
penetrable myBterj% Clearly, it belonged to the regular otder
of fiidoreal arrangements ; and quite aa clearly^ it difiEered
toto cotlo from the aeries of operationa by which the planetary
Hystem had come into existence. Nor could any reasoa for
the divergenoc be BBsigDed until Dr. See published, in 1893]
hia researchea on the part played by tidal friction in moulding
the relations of double stars. Baaed on Professor Darwin's
memorable inquiries into the antique history of the earth and
moon, they followed a line essentially original. No attempt
had previously been made to trace the consequences in Blellar
systems of a mode of action known to have been powerfully
effective within the narrow procincts of the lunar sphere.
Yet, since it gains efdcacy as the ratio between the masses
submitted to it approximates to equality, it should reach a
maximuiD of influence in modifying the relations of co-
209
THE EYOLTTTION OF MULTIPLE STABS 20t
ite bodies such as double stars. Tidal friction is, in
See*e words, " a neccBsary adjunct oi" gravitation wherever
oystems of Ouid bodies exist Id a state of relative motioD ;
it ie a physical agency aa universal as gravitation itself,
operating more or less powerfully in all the syBtema of the
universe." ^
The key to the enigma of double-star development was
given by the high eccentricities of their orbita. Two bodies
levolving very close together are not only pushed asunder by
tidal reaction, but are forced to retreat along trocka that
become elongated aa they widen. The process is terminable
after an indefinite lapse of time ; and is even theoretically
reveTBible, though to an almost evanescent degree. What we
jttflt now have to do with, however, are the dii'ect work-
imge of a cause, aatiefactorily shown to be adequate to the
effects assigned to it. If this be so, telescopic star-pairs set
forth on their careers as spectroscopic binaries ; while spectro-
scopic binaries must, through the mfluence of tidal friction in
widening their paths, be steadily growing into visual couples.
One class ia complementary to the other, and Dr, See's
hypothesis obtains fresh confirmation from each additional
discovery of a star with variable radial motioru
Moreover, these excessively close systema are strongly
marked by signs of progressive change. Some appear to be
still inchoate. The eventual stars are intimated by certain
phenomena of their light-changes to be perhaps as yet
undivided. Connected, it ia thought^ by a surviving ligament,
they revolve as a dumb-bell might, pivoted on its neck, and
aptly iUustrate the " apioidal " forma dealt with in the
formuhe of Poincar'i find Darwin. From the rupture of a
spinning " dumb-bell/' then, to stately binaries in secular
revolution, a virtually unbroken series of instances can be
traced ; and that the advance is really a development, is a
fairly irresistible conclusion. A set of specimens presenting
gradual modifications of a given type proclaims of itself a
transforming agency ; and double stars exhibit, not only all
the linked instances that could be expected, but the requisite
agency for producing them ready at hand in the grinding and
modelling power of ttdal friction.
* ^Jtn afui A$lTOpfij/ties, rgl. xiL p. 290.
14
210
THE SYSTEM OF THE STARS
I
The theory of double-star evolution through its exoep-
bional otficuuy in embryonic stellar sy^temB is thus, at &a
eight, strongly reooumiendud. It must be true to some
extent Bub it has limitations and quali^cations which
should not l)e overlooked. The dynamical and pbyaol
histories of double stars are iiitimateiy counect^ Theit
relative masaes and densities, their epectr&l congruities or
divergencies, their colour and brigbtne^, are 80 many itemi
of evidence as to the course of their companionship, and ihi
destiny awaiting them. Comparative mt^uiriea are indeed
especially difficult for objects in many cases barely eepoiable
in the aky, yet they have been set on foot ; and the few ficti
BO far collGcted are valuable, both in themselves, and sa a&
earnest of a fuller harvest. Meantime, they seem to warmnt
one or two provisional generalisations. The first is, that
contrasted pairs of yellow and blue tints are formed each of a
solar and Sirian star, the lesser component showing the morf
primitive spectrum. Since, however, their revolutions are (^
inordinate elowneeSj their mass- relations cannot be apportioned
It is only permissible to say that if satellite-statB resemble in
constitution solitary stars of similar light - quality, theii
brilliancy must exceed the proportion of their mass. Their
gravitative disparity should, in this case, largely outmeasure
their visible inequality.
An opposite rule seems to apply where the secondary star
is of a roseate or purplish hue. It is founded, indeed, upon
only two ascertained instances ; yet they do not appear to be
eioeptionaL The companion of 70 Ophincbi, while of less
than one-fourth the brightness of its primary, quadruples its
mass. Admitting it to be of the same density, it gives eleven
times less light per square mile of photospheric aurfaca And
for the analogous pair, i} Cassiopeiae, the ratio is ten to one.
The lesser luminary ehinea with one-tenth the areal brilliancy
of the primary, equal densities being again assumed. Un-
fortunately, the rays of these heavy satellites have not been
separately analysed ; so that, in the few case^ where spectial
distinctions are on record, nothing is knon-n aa to relative
maira; and where relative masses have been determined,
differences in light -quality are undiscriminated. An ex-
ception is furnished by a Centauri, the components of which
THE EVOLUTION OF MULTIPLE STAES 211
ftre thoroughly individualised. But they ehow no hetero-
geneity of colour or apectrum. One is a deeper yellow than
the other, simply because its ab&orption is stronger than,
though fiimiJai: to that of its comrade. Binary systeme
undoubtedly offer the most promising field for investigating
the stagea of stellar development. Their relative antiquity,
to begin with, can be roughly estimated ; for there is good
leasou to suppose the closest and swiftest pairs to be in
general the most primitive. Further, the compouents of
each are necessarily of the same age. Whatever spectral
differences they present cannot then be set down to the
exclusive account of tima They are either aboriginal, or
have supervened as the residt of innate diversities. Thus,
bodies unequal in mass are unlikely to develop at the same
rate. The long'accepted opinion was that it should be slow
in proportion to the quantity of matter contained in each
globe. Sir William and Lady Huggins, however^ suggested
in 189Y doubts on this point^ They indicated the probability
that a high gravitational constant might hasten the transition
from a Sirian to a solar spectrum ; and the phenomena of
double etara seem expreaaly adapted to serve as a criterion
I whether this is so or not. A deciaive condition could be drawn
I from a comparison of the masses of such a chramatlc pair as
^^3<50tis ; but the possibility of instituting it ie in the dim future.
^H Something, on the other hand^ may be learned from the great
spectroscopic binary Capella concerning the influence of massive-
nesa upon spectral history. If the plane of its revolutions passes
through the earth, the attractive power residing in the system
is more than twice that of the sun ; and this minimum esti-
mate should be increased eight-fold to correspond with an
orbital inclination of 60" to the line of sight. Now the star
is enormously brilliant. It has a measured par»Iliix, and at
its diatance, our sun would appear 102 times fainter. Assuming
the components of the binary to be equal globes^ of solar
density aud intrinsic lustre, each should posseas the mass of
363 suns. Their mutual attraction, in other words, should
exceed 726 times the gravitational pull exerted on the planets.
Keverthfeless, the highest value that can plausibly be assigned
their joint mass ia twenty times that of the sun. The
^ Astropk^ Jovm. toL tI. p. 320.
212
THE SYSTEM OF THE STAKS
tMBModous diflcrepancy thus mftde apparent obliges u i»
BOppooe that Capella, while iipectroeoopioaUj alinost « t«plin
of the Bvn, is an orb far leas oondenaed and more lanmioaa.
It then eridentljr became inveeted at a much earber st«ge
of oooling, with a reversing lajrer Bimilarly oompoaed hi tfait
producing the Fraonhofer lines. Further experience most
decide whether giant sons of thia type are inyariablr mon
C«]iuoQJs than their light would le&d us to expect, or wbeUk9
Capella is in this respect peculiar. Its example seircs «t
leaflt to give an idea of the modes of evolutioDAiy iuqoiij
rendered feasible by the study of bdnaiy syBtexna.
Inequality between mass and light is pushed to the iM
extreme in the obecore, though etrangly attractive attendaztha
of many lustrously white stars. A large numbex of sucb
ineongriious couples have been discovered spectaxtgraphicaUr,
and the enigma they present; finds no ready solution. Clearly,
diApaiate loss of energy by radiation will not reasonably ei-
plain the contrast of their present state. Rather, some
profound diversity of constitution mnst be supposed to have
brought it about The brilliancy of stellar photosphere
essentially depends upon the activity of interior circulator?
process^. These are perhaps, in abnormally dark globes, pre-
maturely retarded or arrested. But the bow ? and why ? evade
divinatory efforts*
Ftom dwelling on the origin of binary stars, our thoughts
insensibly range beyoud them to larger combiDations. Be-
volving couples very often form only part of an extended
system- Is it conceivable that such varied aggregations were
fashioned throughout by the same kind of influence ? Waa
tidal friction the factotum in all their developmental changes I
To affirm it would be periloua There is no warrant for
ascribing an iron consistency to creative methods. In the
planetary system, at any rate, they seem to have been cod-
siderably varied. Professor Darwin has virtually demonstrated
that lunar-terrestrial relations lay apart. No other member
of the solar family could have originated by fission, as the
moon presimiably did, or raised a tidal wave of overruling
magnitude ou the etill plastic surface of its primary. Hence,
uniformity in the processes of cosmogony need not be taken
for granted "We may^ for example, reasonably admit that the
THE EVOLUTION OF MULTIPLE STAKS 213
close pair in 2^ Vt^x Majorifi divided at clo6€ qimrters Bimilarly
to the earth and moon, without extending the inference to the
telescopic compaDion of the same star ; still leaa to Alcor» its
distant feUow- passenger through space. Each case should be
ooDsidered on its merits, without prepossession in favour of
hannoniaing the results. Indeed^ the long series of operations
traced out hj Dr. See is scarcely capable of being duplicated.
Throagh over-rapid apiumug, a fluid globe may split asunder
ooce ; but a repetition of the event is virtually precluded by
the very consequences of the first disruption. For the new-
born satellite exerts, by the drag of the tidal wave it raises
on its primary, a powerful retardative influence on ita rotation ;
the speed of which inmost unlikely to reach a second time the
pitch needed for instability ; and the satellite itself is uuder
the same prohibition. Multiple stars, then, cannot^ so far aa
we are able to judge, have been formed by succesflive sub-
diviaiouB of one parent mass. In stellar systems, as in the
solar system, many degrees of relationahip are diatinguiahable.
Groups in loose mutual connection may have originated con-
temporaneously in different sections of the same nebula.
Binaries of co-ordinate rank are doubtless frequently included
in a single complex mechanism. This species of remote kin-
Bhip is forcibly suggested by the movements of f Scorpii, one
of the few triple stars, all the members of which are in visible
revolution. Tet not in the same sense. The close pair
circulates directly, the third, more distant companion (as
already stated), in a retrograde direction. The wide
divergence thus probably indicated of the two orbital planes
betokens unmistakably a remarkable dissimilarity in the
eonditions under which the near and the remote satellites
respectively took their origin. A more intimate acquaintance
with such systems will perhaps show the case of f Scorpii to
be typical j it is assuredly most significant. Again, the
six stars forming the Orion trapezium are, beyond cavil, a
physical group, in immediate genetic connection ; yet it would
be extravagant to suppose one the parent of the others. Only
the dark body circulating contiguously to the brightest of the
aextett can be regarded as ita proper ofispring ; the rest claim
an independent footing. Ws can conceive them as having
condensed from distinct knots in one vast nebulous structure
214
THE SYSTEM OF THE STA£S
imfmmed with & dowly wheeling iiiimiMnit, We euiaol
flotto dy e thflB as thiowmaff one After Mindier hy oae evifi^
rotatiBg ^^eh&. The sne Biglit be sid of ibe qnednqfc
fljitem ff Ljia» and of meaj mat.
The BOfe •tfeeDtirely coaoie prooesies m etodied, tte
Bkon Tmrioee tiwj e^ypeftr. 7hii§» oometo vma be cleeziy ra
to bare ongtnftted dilfeiciitlj from planete^ aad sonte pUnHs
diflezaiUf from others; while our o>wn aaleUte Btrndt Mk
e line for itsell The large ooafWDanceB of the volar sjnlai
snlwist amid divenctj of detail, attesting etroog indiTidiialitifli
of history and statua. A^d vocb diTersitj' has its foUec* SDvpi
among the etare. It la much if we ean eatch glimpees of I
partial truth in meditating on their evolutioQal order; the
profundities of its meaning, and the intiicauaeB dt ila roois i>
tbe pa£t, and lamificaticins into the futme baffle our scniti-
niaing efforts.
CHAPTER XVU
THE PLEIADES
Tbom multiple fitats the transition is ewsj to star -clusters.
These eeem to embody completely the idea contained in germ
in the former class of objects. They are collections, often on
the grandest scale, of sunlike bodies small and large, united
in origin and history, acted upon by identical forces, tending
towards closely related ends. The manner and meaBure of
their aggregation^ however, vary widely, and with them the
cogency of the evidence as to their organic oneness. There
are innumerable cases in which it absolutely excludes doubt ;
there are some in which it is rather persuasive than con-
vincing. It i& not then always easy to distinguish between
a casual " sprinkle *' of etaifi and a genuine cluster, Kor can
the movement-test, by which so many physical have been
discriminated from optical double - stars, be here applied.
Internal difiplacements of a circulatory character have not
yet become apparent in any cluster, and there Ib only one
with an ascertained common pioper motion,
Thia ia the inunemdrial group of the Pleiades, famoue in
legend, and instructive, above all others, to exact inquirers —
the meeting* plaee in the skies of mythology and science.
The vivid and picturesque aspect of these stars riveted, from
the earliest ages, the attention of mankind ; a peculiar
sacredness attached to them, and their concern with human
destinies was believed to be intimate and direct Out of
the dim reveries about them of untutored races, issued their
association with the seven beneficent sky-spirits of the Vedaa
and the Zendavesta/ and the location among them of the
' BuDaen, Die PUiade% und dtr TkUrkreiM **, 4S4.
216
THE SYSTEM OF THE STABS
centre of the universe and the abode of the Ddty, o(
the tradition ia etill preserved b^ the Berbers imd
With November, the " Plfidad- month," many pmnitive
began their jear ; ' on the day of the midaigbt-cuL
of the Pleiadea, 17th Xovember, no petition was
in rain to the ancient kinga of Persia ; ' and the samt.' ^t^:
gave the signal at Bosirifi for the commencement of the im\
of Isis, and regulated leae immediately the celebration m\
nected with the fifty-tvro year cycle of the Mexicans. Samp]
AuBtralian tribes to this day dauf^ Id boaour of the " Seval
Stars," because " they are very good to the black felloin.* [
The Abiponea of Paraguay regard them with pride as tlicir |
aneeators,* Elsewhere^ the origin of fire and the knowledge of 1
rico-culture are tiaoed to them. They are the " hoeing-stan"
of South Africa,* take the place of a farming-calendar to tha
Solomon Islanders, and their last visible rising after sunael
ia, or has been celebrated with rejoicings all over the southen
hemisphere, as betokening the " wakiug-up time" to agricultural
activity.
To the Greeks of Hesiod'a age their " heliacal rising " (the
first visible before sunrise) announced, each May, the opening
of the fieasou for navigation ; and their name thus came lo
be interpreted (from plein, to sail), the " sailing-staTS." But
this etymology was doubtless — like the derivation of "elf"
and " goblin " from Chalf and GkibelUne — an afterthought ;
and it may be confidently maintained that the word '" Pleiades,"
bearing like its Arabic and Hebrew equivalents, the essential
signification of a '*cluBter/' came from the Greek pleiones,
many, or pleids, full,* It was represented in Latin by
"Vergiliai" (from ver, gpring), a designation possibly com-
memorative of the ancient coincidence of the atats with the
vernal equinox. They were, moreover, ehoseu about the same
epoch — say 2700 B.C. — by the Hindus to mark the first lunar
' Hs-Hburtosi J^efure, roL xxt, pp. 100, 317 ; V»ii SAndibk, L'A^nnomit,
t iv. p. 3S7.
* HAliburtoOj Ftativai of the Dtad, p. 46.
' Ihid. p. 13.
* Lubbock, Ori^n 0/ CivHisation^ p. 316, 4tli ed,
' .1. HamnioDd Tooke, in «D ioteresting p&per read in Jutuaiy 1SB9 before
tbs S. African PliUosophical Society.
* iffliwr*, Yol. III?, p. 608.
THE pleiahes
217
aion, called " Krittika," general of the celestial armies ; ^
long occupied the same post in Ohaldea under the title
inrayya," the crowd.*
The similarity of the traditions respecting the swarm of
tial " fireflies "
Quie septem did Bex tamea eese soIent,
1^8 suTpriaing as their universality. That they " were seven
now are six," ia asserted by almost all the nations of the
If from Japan to Nigritia, and variants of the classical
of the ** lost Pleiad *' are still repeated by sahle legend*
Dugers in Vi<itom and Western Australia, by "head-hunters"
L Borneo, by fetish-worshippers amid the mangrove-swamps of
Gold Coast An impression thus widely diffused must
Ither have spread from a common source or originated in an
?ioUB fact, and it is at least possible that the veiled face of
seventh Atlantid nmy t^ify a real loss of light in a pre-
atorically conspicuous star. Some members of the collection
at preaent, there is little doubt, slightly or slowly variable,"
id progressive tendencies of the kind are in more than one
suggested to he present. Thus Alcyone, the chief of the
[liUeotioD, now of the third magnitude, and just twice aa bright
the brightest of its companions, was either not oue of the
JUT Pleiades observed by Pfcolemy, or was then much fainter
it has been from Tycho Brahe'a time to our own. So at
least Francis Baily concluded from a careful examination of
the records/ and he knew better than most men how large
an allowance has to be made for ancient inaccuracy. Al
Sflfij boo, the competent reviser of Ptolemy's observations,
expressly states that the Alexandrian quartette appeared to
him, in the tenth century, the most lustrous among the
Pleiades,* Yet none of them can be identi6ed with the
pTQBent imid^i. A literal explanation of the old legend may
' R. H. AUen, Star I^ames arid IfitiT Meaniiigi, p. 39S.
■ Wab«r, iTuiiKhe Shtdien, Bd. x. ii. 21£.
* C. Wolf, Amtaleg dt I'Obaermtoirre fie Farit, t. xU. ii. p. 28 ; Lindemnnn.
M^moira dt fJcad., 9t. P^tw^bourg, t. XKcii, vii. S«r. No. S, p. 29 ; Vogel,
Pottdam Jte^ort., ISPO.
* Jitia&irs H, Aatr. Soe* vol. ilii. p. 0.
* Sofajellerap, Ik$eriptiofi dta ttaiUt, p. 132; Flaminarioii, Lta SU/iUs,
3M.
21S
THB SYSTBlf OF THE STABS
heooe be feasible, and ProfwBor Pickering's voggestod iderit-
ficfttion of PleioDe with tfae waanag A tlanrtd htm mnA ti
reoommend it* Tba dmpbj bf this star of a guet
Bpectram resembling that of P Cfgni ooimifeiiaiioes the tvw
that, like P Cygni^ it formerlf abatie with teznpoiaij a
intermittent briUiancj. It is now of 5'4 magnitude, or jati
twice aa bright as it wa^ hj Azgeknder's estiutate, fifty
/ears aga
The fire stars ordinanlj Tttible bftrirtm Alcji^ie (flee
Plate L Frontispiece) are Sectn and Atlas^ each fluctiiating
slightlj abore and below 3*8 magnitude; Maia« now of the
fourth, or one magiutnde fainter than Akyone ; Merope and
Taygeta, the inferioT? of Maia b^ respectively a quarter and
a half magnitude. Celaeuo, the seTeath or concealed Btar,
gLveB only about one^third the light of Tajgeta,
Yet it ean he eeen with many otheTB> under faTOur*
able circumfitances. Maestlio, the tutor of Kepler, perceiTcd
fourteen, and toapped eleven Pleiadea previousl)^ to the inven^
ticm of the telescope ; Carringtoii and Denning ootmted
fofirteen,' Misa Airy marked the places of twelve with the
naked eye.' The faintest of these fell but little short of the
sixth, and there are tweatj-tbree Pleiades down to the seventh
m^nitude,^ each of which (with perhaps one or two exceptioiis]
might be separately visible in a transparent sky or &om an
elevated station. But their crowded condition makes thia im-
possible, and givee rise rather to the efifect described by
Ka^wini in the thirteenth century, of " six bright stara with
a number of dusky ones between.'' ^
With the use and increase of telescopic powers, the popu-
louflneaa of the cluster has been amazingly increased. An
object-glass scarcely exceeding two inches diameter showed
Robert Hooke in 1664 seventy-eight Pleiades,* and Miehell*8
conjecture, in 17&7, that there might be more than a thousand
of them,' has been superabundantly verified by the results of
modem labours. Over an area about Alcyone me&surii^
Webb. Ctl (Hgteif, p. SM.
* Attr. JVacA. No. 2934.
" Monlhly Noti^tt ToL xxiii. p. 17B.
* Harvard Annala, rol, xir^ pt, iu p. S98 ; cf. HuUer Hud Kemrf, Aatr,
Naeh. Xo. 9Afl7. " Ideler. Sltmnamoi, p. 147.
■ Miero(fraphia, p, 241, t PhU. Tran*. ToL IviL p, 9&S
THE PLEIADES
219
15' X 90' M, Wolf catalogued, at the Patis Obeervatory in
176, 625 Btara to the fourteenth magnitude; on the MM.
^s aensitive ptatea, in 1885^ 1421 made their appearance
amaller space, and the number was brought up to 23 2d
"by exposures of four hours in November and December 1887.
The faintest objects thus registered were probably of about the
sixteenth photometric magoitude.
How many of them really belong to the group, and how
ay are referred to it by perspective, can be determined with
!ie help of time and patience. As regards some of the better
lown stars, the process of discrimination haa already begun.
Beseera meaaurementa of the places, relative to Alcyone,
of 52 Pleiades,^ executed with the Konigaberg heliometer
during the twelve years from 1829 to 1841, furnished a
starting-point for inveetigatioDS of their internal movements.
The upshot of the first effective comparisons was to exhibit
these as null. From a coUodion-print of the cluster taken by
Eutherfurd of New York in 1865, Dr. Gould redetermined
nearly nil Bessel'a stars with such accuracy as to make it
certain that no appreciable interstitial shiftinga had occurred
in the course of a quarter of a century ; * and his conclumon
was, through additional photographic comparisons of ten of
the same stars, extended by Professor Jacoby to the year
1900,^
Now this seeming rigidity implied a great deal. For the
point of origin of the measures in question is not immovably
fixed in the sky. The chief Atlantid has a secular proper
motion (according to Newcomb) of 6", the possession of which
in common by the whole stellar band virtually demonstrated
their effectual union. Where one among many objects is
ascertained to be moving, relative fixity can only mean that
all drift together^ and so the unique phenomenon was brought
to light of the transport in block across the sphere of some
scores or hundreds of congregated suns. Even if the whole of
this apparent displacement should prove to be as it were
rejected from the sokr advance, its significance of physical
kinship among the objects affected by it would be nowise
impaired. For an identical parallactic shift would equally
' AUt. J^ach. Ko. 430. ' Observatory, vol. il p» Ifl.
■ AttfopK Joum. ToL xitt. p. 66.
220
THE SYSTEM OF THE STABS
' Bsffioe to locate tbem in Ibe sune region of sp«oe note
imtnediate inGueooe of their confitrainicg mutaal grsTitj.
The BRlAbliahment of a genenl uQaaimitj of moveraeU
among the Pleiades waa the first Bt«p towards inveetigatii^
their retationa; the next waa to seek evidence of ii j i il iiiM ri r
change. This haa still to be found ; its highlj reooiidifie
nature has been rendered tinmistakable hj the laboois of
Wolf/ Pritchard* and ElJdn.' Bisplaoemanta within the
duster, though necessarilj in progresa, are bar^y naMxaL
Sometbiug, however, haa been done towards its aimljBi% M
the result of Dr. EUdn's work at Yale College in 1884-85.
Leaving nothing to be deeired in the way of skill and care,
it was the more Btnctly comparable with Beasel's from having
been executed, like his^ with a heliometer, one of about seren
inches aperture, completed in 1832 by the Messrs. Bepsoild
of Hamburg. Sixty-nine stars, down to 92 m^nitude, wan
included in the survey, only one of Bessel's being omitted,
while seventeen were added from the Bonn Dorchmusterung
The close agreement, on the whole, between the places detei^
mined, after an interval of forty- five years, at Konigaberg
and Yale, lent importance to some minute discrepancies
the most considerable of which intimated the probability that
eix of the objects on Bessel's list were only apparent members
of the cluster/ They should probably be regarded as peendtK
Pleiadee, intruders into a company from which they will
eventually be expelled through the cumulative effects of in-
compatible movementsL Exempt from the influence of the
current bearing Alcyone and its true associates slowly towards
the south -south -east, they remain almost absolutely stationary,
and are accordingly in course of being left behind. Recent
counts by Pickering* and Stratonofif^ make it &irly certain
that the majority of the small stars within the area of the
Pleiades will be left behind with them. The ground for this
1 AnnaUa de VOhKrvaioint t, xit, u, ; Comptes J^outut, t IxxxL p, 6,
' MtjTtthty Natiai, toL aOiv. p. 857-
rran*. Yrds CoUege Obtfrvaforif, Tol. L pt. L IS87. Pt viil contwns
reialta ofn SBcoud triaiigul&tiou by M. F. Smith id lfiOO-2.
Dr. Klkin expresaed this tIqw with iwuBicierable reMm u ngardi roar of
the sis. stATB, Cf. hi» reviBMl oocduaLotifl, Traiu. Yah ColL Obtfrvatory, Tol L
pt. vii. p. 3G6, ]»34,
' Harvard Circular, No. 17. ' Attr. Nath. Nff. 34il.
THE PLEIADES
221
;ce is that they ore leas densely strewn than the multi-
.0U8 stare in the adjacent sky. The true glomerahiU
is then formed of brighter objects, the number of which,
"tlioiigh still unknown, can be ascertained after a moderate
lapse of time by renewed photographic comparisona
The proper motion of Alcyone reverses, with approximate
accuracy, the direction of the aun'a progress through space.
It may hence be regarded as parallactic, that is, transferred
by perspective from our own. If this be so, the distance
between Alcyone and the earth can be calculated, given the
direction and velocity of the sun's translation. Now we know
that the sun is travelling towards a point in the conBtellation
Lyra at the rate of about twelve miles a second. On this
showing, the Pleiades are so remote that their light takes 190
years to reach us (parallax = "'01 7). Nor is the estimate
likely to be materially diminished,
Our own sun, thus far away, would shrink to a star
of 8' 6 magnitude. There can be little doubt, in fact, that it
is surpaased in brilliancy by fifty to sixty of the Pleiadeg.
And it must be, in some cases, very greatly surpassed ; by
Alcyone 170, byElectra 83, by Maia about 70 times. Sinus
itself takes a subordinate rank when compared with the five
I most brilliant members of a group, the real magnificence of
l^^hich we can thus in some degree apprehend.
^H The scale of its construction is no less imposing. No
^judgment can of course be formed as to the interval of space
' B¶ting any two of the stars belonging to it. All of them
are seen projected indiscriminately upon the sajne plane,
without regard to the directions in which they lie one from
the other* The line joining Maiaj for instance, with Alcyone,
may be foreshortened to any extent, or not at all. No
criterion is at hand which we can apply. Of the dimensiona,
however, of the cluster as a whole, some notion can be
gathered- For its shape — irrespectively of some outlying
streams of small stars — ^may be taken to be rudely globular ;
and since a circle described from Alcyone as a centre with a
radius of 48', includes all the princix>al stars, sixty of Klkin's
sixty-nine, fifty-two of Bessel's fifty-three falling within it,
the apparent diameter of the denser part of the aggregation
cannot differ much from 96'. But the proportion of the
THE SYSTEH OP THE STABS
radioB to the disUnoe of a ^LcA» is known from eleme&ti
trigoDOOBfttrf , and hoe ooaes oofc (in roand nombere) m i
to wTOufcx-ooe; ao tfant tfaa bodin ntnated doae to iia snrfHt
•M serentj-one times neuer to Uieir c^stzal lamioaiy U«
tlifiir oen^sl IimiiiiuT' la to as. If thej revolve round it, ii
IB at &XI interval exceeding fifteen billion miles, costing lig^
not far from three joaia (o cnaaa; and the period of their
ciTciilation m&j well be reckoned by millions of yearn Upc«
these dependent otba, Alcyone shines with sixty timee the
loBtre of S'liiua in terresCrial ^es ] yet the presence of 130,000
Alcyonea would only juat compensate for the withdrawal d
even such a diminished sun aa brightens the firmament of
Neptune. From staia moi« centrally placed, the chief of the
closter doubtleas appears a Teritable aun^ although it may not
be to all the primary light-giver. An assemblage like the
Pleiades distributed round our sun would extend eompaetlf
three -quarters of the way to a Centauri, its feelers and
appendages indefinitely farther. Hence there would be ample
room in it for secondary ayatems and particular associations of
luminoua bodies. And, in point of fact, the actual dusttf
contains several of Bumham's close double stare, one certainly,*
all presumably in mutual revolution, to say nothing of the
doubtful companion of Atlas which, distinctly visible only
onisd to Struve in 1827, gave nevertheless some sign of itB
preeence during an occultation by the moon, January 6j
1876.*
The discovery of Maia as a spectroscopic binary suggests
an indefinite range of hidden complexities in the mechanism
of the cluster. It ensued in the course of a research on the
radial velocities of the six leading Pleiades, carried out by
Mr. Walter Adams with the Bruce spectrograph of the Yerkes
Observatory in 1903-4.* The diffuseneaa of the spectral lines
in these stars impaired the precision of most of the determina-
tions; but Maia offered more facilities than its companions;
and the variation of its speed to the extent of about eighteen
miles a second seems indisputable. The period of its re-
volutions baa atill to be assigned. The other five stars all
proved to be receding from the sun at rates corresponding
1 AUt. JtfoM. No. 8047. * Ibi<L No. 2074,
■ AsiropK. Jqw%. toI lix. p. 336.
THE PLEIADES
233
■ly well witb the 8un*B celerity of withdrawal from them.
^That ifl to say, no evidence of individual motion (unless
3K)B8ibly in the case of Taygeta) was elicited from them.
Spectroecopic measures are then no moi^ immediately hopeful
"iban micrometrical measures ^ for obtaining a clue to the
djruamicHl condition of this marvellouis star-group,
A iSpectrum of helium type characterises itB genuine
members. A simultaneous spcctrographic impreseion obtained
by Professor Pickering from close upon forty of tlieBe etars,
January 26, 1886, demonstrated the nearly identical quality of
their light, and fumifihed " strong confirmation of their common
origin." ^ Only in two cases, a stronger " K line " recorded
itaelf than auch light ordinarily includes, and the divergence
was, in one of the two, both accentuated and explained by
diversity of motion. The star in question {a Pleiad um) haa
been already signalised as an incipient fugitive from the group
to which it never truly appertained.
The stars of the Pleiades, while shining with so poignant
a lustre as to make the sky-ground they are relieved upoa
show to the eye as blacker than elsewhere, are in reality
wrapped and entangled in an immense cosmical cloud. Some
indications to this effect caught by optical means have been
autographically amplified to so surprising an extent that the
discovery of the nebulous condition of the Pleiades ranks among
the most important achievements of celeatial photography.
The " Merope nebula " was compared by M. Tempel to a
,ia of breath upon a mirror. Discovered by him at Venice,
October 19, 1859, it envelops and stretches back in comeCary
shape from the star to which it is attached, covering a space
oi about ^5' by ^O'.* But this large size only makes its
perception more difficult, by impairing the effect of contrast
with the surrounding sky. High magnifying powers (which
e imply narrow fields of view)^ render it on this account com-
pletely inviaible, and a haze so slight as to permit the observa-
tion of stars of thirteenth or fourteenth magnitude sufhces
I I Ellcin, Trans. YaU CoUtgt Obweraiiory, toL L p. 101.
* ittmoin Amer. Atad. voL xi. [\ 21D ; Soirvard AnmaU^ vol. zzti. pt ii.
p. 3d2, whore the apcctrk pf Diiuty^one membein of tha group vo BpeoilieaUy
Noarded
« A^r. Jfaeh. No. 13W ; MonlMv Noiiu$, toI. zL p. 622.
, the
^^i
THE SYSTEM OF THE STARS
to oblit«tate it. This evasiveness auggeeted varubtHtj; If.
Tempers contrary opinion has been fullr justifietL
The idea was entertained both by Goldschmidt^ aai
"Wolft thftt the filmy veil flung round Merope was but a fag-
ment of a larger whole ; and as time went on, gUmpees ven
snatched of imsty ahreds and patches in cotiuectioa with otbff
members of the gmup. Alcyone appealed to Searle at Harrari
College, November 21, 1875, surrounded by whitish hght;*
the effusion about Merope, eyidently to Schiaparelli in lS7h?
and to Maxwell Hall in 1880, reached Electra and eTm
Celaono ; * while a leniarkable view afforded to the late Dt
Common by his three-foot retlector, February 3, 1880,* rf
three feebly luminous blotches between Merope and Alcyooft,
prompted his comment that " there ia a great deal yet to be
settled as to the extent and number of the nebulf& in thii
duBter.'*
Its import, however, became apparent only when
photography was brought to bear upon the subject. ITm
first nebula discovered by the new method was a small BpiraJ
appendage to the star Mala, which printed itself on plates
exposed by the MM. Henry, each during three honra, io
December 1885." Only the accumulating faculty of the
" chemical retina " co»ild have revealed the presence of aa
object BO excessively faint in a telescopic sense ; but what fe
known to exist is, by that alone, rendered more than half
visible, and the Maia nebula was accordingly discerned.
February 5, 1886, with the FuDcowa thirty-inch refractor,
then newly erected, and later with smaller iuBtruinents.^
Besides the Maia vortex, the Paris photographs depicted
a series of nebulous bars on either side of Merope, and a
curious streak extending like a finger-post from Electra towards
Alcyone. But all these were mere samples of what lay
behind. Impressions of the Pleiiides secured by Dr. Roberts
with his twenty-inch retlector in October and December, 1886,
showed the whole western side of the group to be involved in
^ Lf> Mtmdtt, t. lit. p. B29. ^ Harvard Annah, vol. xiii. p. 71.
" Attf, Nadt, No. 2045,
* Mtmthiy ^'oficet, toI, xU. p. 515. * Tbid. vol. iL p. 37«.
* Similarly recorded a month earlier at Harrard Oolkfef it vm takon for a
Saw in the D£gaciv«.
T Attr. Jfaeh, Noa, 2719. 3726. 2730.
THE PLEIADES
22S
Doe vast nebulous formation.^ " Streamers und fleecy iBasaes "
of coBiuical fog seem, in these aatomsbrng pictures, almost to
fill thi3 gpaeeB between the stars, as clouds choke a mountain
valley. The chief pointB of its couceutratiou are Alcyone,
Idierope^ and Maia ; but it includes as well Celseuo and Tay-
geta> atid is traceable southward from Asterope over an arc of
1' 10'. These photographs, in fine, as Mr- Wesley wrote,
•• not only prove beyond a doubt the existence of the much-
disputed Merope nebula, but they also combine and harmoniee
itt a very satisfactory manner the apparently irreconcilable
drawings." ^
The matter was not allowed to rest here. Early iu
1888 the MM- Henry succeeded in giving to several plates
eacposures of four hours, with results identical in each case, and
very eurioua Their nature can be estimated from our frontis-
|Kiece, which reproduces the final chart of the Pleiades prepared
by the MM. Henry. The greater part of the constetlation
is shown in it as veiled in nebulous matter of mot^t unequal
dsnsity. In some places it lies in heavy folds and wreaths,
in others it barely qualifies tho darkness of the sky. The
details of its distribution come out with remarkable clearness,
and are evidently to a large extent preecrihed by the relative
Bituatiou of the stars. Their lines of junction are frequently
marked by nebulous rays, establishing perhaps between them
relations of an unknown nature ; and masses of nebula, in
niuxkerous instances^ seem as if pulled out of shape and
drawn into festoons by the attractions of neighbouring stars.
But the strangest exempUlication of this filamentous tendency
ifl in a fine, thread-liko process, 3" or 4" wide, but 35' to 40'
long, issuing in an easterly direction from the edge of the
uebula about Maia, and stringing together " like beads on a
rosary " * seven stars met in its advance. Two similar rectilinear
nebuhe run parallel to the first, and a fourtli was photographed
by M. Stratonoff iu 189G.''
Wliethcr these luminous highways are due to material
condensations, or merely indicate tracks of electrical excite-
' JfoivfA/y Jfotiert, voL ikii. p. 24,
* Jount. Liv. Astr. Soc^ voL v. p. 160.
* Motiohex, Comptes Jiewiug, t. cvL p. 013 : H. C. Wilton, AHr* and Attirs-
iricf, Tol. xiil [J. 192.
* Attr. HmK. No. SSS«.
X$
22fl THE SYSTEM OF THE STABS
meDt, Uiej &re equall^r coimiiumcAtiye upaa one point Tbi
oozmection by their meaas of stars into zows virteoUy dt
monfltiabes tbeir real aligcuneDt, and thtiB oooakknib^
strengthens the presampdon that the linear mxnagaimt
preT&lect in dusters is no optical iltaoon^ but depeoda Vfm
intrinsic conditions, the outcome of univerBal laws..
The wonder of this aggregatioQ of stan and ixebol^ h
bGen enhanced hy Professor Bami&rd'e diacoTeries. In l89U.*
he detected visually a bright round object, like a comet with-
out appondagea, in Buch close ptoximitj to Merope aa to foca
with it probubly a nond^ript binary combiaattcm;, T^
three years later,^ two exposures with the WiUArd lena broo^
into view a «et of curving streaks iBsoing from the cbisltf
as a whole, and enfolding it exteriorly in far-reaching diiD
nebulosity. Ita genetic history can hence be judged to b«
Btill at an aarly atage ; yet the unity marking it is already
singularly diversified. Many orders of stars are there gatjiei«d
together iato what might be called a micdatuTe sidereal sjrstem,
the largest of such " surpassing gtory " aa to dim by comparisoo
the splendour of Siriua and Vega. The " act of order " in tins
** peopled kingdom " is not easy to divine ; we eao only stt
that the mutual relations of its denizens must be highly
intricate. Within the wide framework of the association
room is found for subordinate groupings of various obaradfcen
and degrees of closeness, from stars far apart, but drifting
in company, to pairs aa unmistakably united by contiguity as
two nuts within the same shell. Thus, the polity governing
the entire system of the Pleiades would seem to be of the
federative kind. Nor can we be yet sure that its boDd^
while evidently so loose as to give lutshackled play to looal
liberties, are nevertheless sufficiently strong to restrain tlie
slow worktugs of disruptive tendencies.
1 A9lT, JVocft. No. SOI 8. * /M, No. S353.
CHAPTER XVin
STAK CLUSTERS
CSbuT five hundred clufiters are at present tolentbly well
mown to astronomers, and a large number besides, their
ibaracter rendered ambiguous by distance, are probably in-
Inded among botb " resolvable " and " unresolved " nebulee.
Inch aggregations may be broadly divided into " irregular "
iiid "globular" clufiterB. Although, as might have been
ixpected, the line of demarcation between the two claaaea
a by no means eharply drawn, each has its own marked
»eculiaritie&
Irregular clusters are ftamed on no very obvious plan ;
bey are not centrally condensed, they are of all shapes, and
heir leading stars rarely occupy critical positions. The stare
n them are collected together, to a superficial glance, much
iter the fashion of a flock of birds. Alcyoue, it is true,
leems of primary dignity among the Pleiades, and the Pleiades
n&y be regarded as typical of irregular clustei's; yet the
lominance, even here^ of a central star may be more apparent
han real
The arrangement of stain in clusters h, nevertheless, far
rom being unmethodical, even though the method discernible
Q it be not of the sort that might have been anticipated.
'.% seems inconsistent with movements in closed curves,
ind suggests rather the description of hyperbolic orbits,
ifet its true nature must obviously be greatly obscured to
►ur perception by the annulmentj through perspective, of
■he third dimension of space, whereby independent group-
ngB, projected indiBcriminately side by aide, are rendered
jarely if at all recognisable. That they should, under these
%2B
THE SYSTEM OF THE STABS
circamstanoeA, stand out to Anj extent is mora sorprais;
than that thej should aometimee be inextrjcabljr e&UngIri
with sprinkled etais belonging to the fore- or haefcgranl
The nebidous ImlHng together of a septupie aet in the FUld*
aaaureB oa, nevertheless, that Btar^^alineatioiis are o«>i illcwT
Nearly oil observers have been ixupreaaed wntt tU
streaming and reticulatied character of many stnllar m»a.
blagea. Thus where the feet of the Twins <U]
Way, an object is enconnlered so "nrnrvelix.^.'-.j ^ww».-_
with a Urge telescope^ that "^ no one coold see it for Lb« fij<c
time/' Mr. Lassell declared, "without an excIamatioB.* A
field 19' in diameter " is perfectly fuU of briUijuit atan sa-
nanally equal in magnitade and distribution over the v^U
area. Nothing but a sight of the object itself can cor
idea of its exquisite beauty/'^ Admiral Sm}'th dcscj;.-^ ■
aa " a goi^ecma field of etaia &om the ninth to the sixteenlti
magnitudes, but vrith the centre of the maas leas xich Uud
the reet. From the small stars being inclined to fonn cunes
of three or four, and often with a large one at the rcvot of th'
curve, it somewhat tieminds one of the burning of a ekj-
rocket." * A photograph of this duster ' by Professor Bamar>],
teproduoed in Plate XL, Fig. 1, leaves very little doubt of its
intimate galactic affinities. The sinuous linens of etArs i
compose it/ although more dosGly entangled than the
catenary arrangements on the leas crowded parts of the
can scarcely be organically distinct from them.
Yet the radiated aspect of stellar throngs lends them a
quaai-individuality. Tbe singular looped conformation \*i£ib)o
in the " gold-dust " duster in Auriga (M 3 7) attracted the atten-
tion both of d'Arr«st and Lord Eoese ; * about one bundretJ
connected stars in Ophiuchus (N.G.C, 6494) "run in lines anJ
arches";* a superb assemblage in Cassiopeia (N.G.C 77S9;
was deecribed by Lord Roaae as formed of jagged branches with
' Monthly Noiicta, voL xir. p. 7A>
* Cycle, p. IftS (Cbunbera's ed.).
' U 3fi = N.0.C. 2163. NcibuUe ud closters tli»aghoat thk toIcbic
■n dutingnished bf Ucuier's welMfQOwn oambera, irbeD uooog Uie 10^
epumflratod bj him^ atherwiae by 7>rejeT'£ in the Kne Ofnerai Caimtsgm'.
* 3*cchi, jftti deir Aeead. Font. t. rii. p. 72.
* Tm«. li. Irish Acad, to], ii. p, 51.
* PML Tranf, vol cinii. p. 460.
^
^
STAR CLUSTEBS
irk holee between, and by Dr. Roberts, from hia photographs,
^s exhibiting curved and wreathed patterns in stars.' The
constituents of a large group near the Poop of Argo (N.G.C.
2667) struck the elder HerBchel by their arrangement "chiefly in
rows/' illustrative, to his mind, of the mechanical complexities
of such eystemg. Each row, he observed, while posseraing its
own centre of attraction, will at the same time attract all the
others; nay, "there must be somewhere in all the rows to-
gether the seat of a preponderating cluBtering power which
will act upon all the stars in the neighbourhood."* Specula-
tions, indeed, upon the dynamical relatione of " stars in rows "
are still prematui'e, nor are they likely, for some time to come,
to be accounted aa " of the order of the day/' But the con-
tinual recurrence in the heavens of this mode of stellar aggre-
gation cannot fail, to suggest the development of plans of
systemic dissolution and recomposition on a grand scale, and
involving the play of, by us, unimaginable forces.
The more attentively clusters are studied, the more intri-
cate their construction appeara That which challenged
HerscheFs notice is not singular in lEtimating a Icjigue of
several co-ordinate groups. There is rarely evidence in the
conformation of irregular clusters of their being governed
from a single focus of attraction,; there are irequent indica-
tions of the eimultam^Dus ascendancy of several. A cluster in
Sagittarius (K.G.C, 6451) is distinctly bifid It was re-
marked by Sir John Herschel at Feldhausen as " divided by a
broad, vacant, straight band";° and his figure shows the
separation as absolutely complete, the sections,
Like cliffs which had been rent asunder,
facing each other with a chasm between.
A beautiful cluster in Sobieski's shield (M 11), first noted
by Kirch in 1681, seems to be extensively dislocated. Sir
John Herechel succeeded, by the use of high powers, in break-
ing it up " into five or six distinct groups with rifts or cracks
between them." * Father Seochi perceived in it a three-lobed
^ Cfiestial Fhoio'jTapht^ vol. i. p. 129,
2 Phil. Trans. toI. civ. p. 289.
' Cape Obiervaiiont, p. llO.
* F\ii, Trans, vol. oniii. p. 4fl2.
230 THE SYSTEM OF THE STABS
central vacuity;* and M* Fenet, who in 1895 m&pped from
Dr. Roborts's phatograpbe 395 of ita oompocenta, ' remufaii
their most likely progresaive sepftxation into aeven or ag^
difitinct aUotmeuta.
Plate XYI. shows M 11 in iba Milky Way kkc&tiaii u
photographed by Frofe-saor Barnard with the WillArd km
In hia opmion it ia *' hardly queetionabU " that the cloUtt
(here ueceaB&rily contracted into a simple cltimp) really octo at
nucleus to the vast atar-clouds * attached to it like volondoois
wings. But bow strangely related auch a nucleus must be to
such a, formation I
This " glorious object " (as Sir John Herachel called it) ow
just be made out with the naked eye on a perfet:tly cle«r
night. HaUey mentioned it in 1716 as " of itself but a small
obscure spot, but with a atar that ahiaes through it whii^
makes it the more luminous." * Some years lat6r, Deiliam
found it to be " not a nebulose, but a clui^ter of stars, somewhat
like that which ia in the MUky Way." ' A catalo^e of tw&
hundred of the components, prepared iu 1870 by M. Helmert,
of the Hamburg Observatory," provides material for the futur*
investigation of relative changes.
The presence in a cluster in Monooeroa (N'.CC. 2269) of
** a double seat of preponderating attractions," was observed by
Sir William Herschel ; ' and a throng of some two htmdied
stars in Cancer (M 67), discernible with an opera-glaas, falb
no less obviously into two divisiona.^ In a collection seen at
PaiBonatown to be riddled with absolutely dark '* lanes and
openings"* {N.G,C. 2548), the principle of local self-govern-
ment has evidently been already carried a long way. A
"reticulated mass of small stars" iu Cj-gnus (K.G.C. 6S1&)
was there described as " a most gorgeous cluster, /u// of Kolu";
and the drawing published by Lord Bosse depicts a winding
1 AUi deW Jccad. Pwt, U Tli. p. 75.
* £ul£. Soei&i Astr, de France, 1895, \\ 6fi.
' Aitrsph. /imm. vol. i. p. 11,
* Phil. Tr&M. vol. ixix. p. 3Q2.
■ Ihid, vol, jutviii, p. 72.
■ P^lieatimen der Hamhurgw Stemware, No. I, 1S74.
' Phil. Tranit. vol. civ. p. 208.
• Smjtb, Cffctf, p. 241 ; L. Fenet, L' Attronomie, t. vi. p. 145,
* Trant. R. DuHin. Soe. vol. ii. p. 6fl.
*.lltll.
Fk»tngi«|>l!i ipr ili'SRiw 1 1 \iw\ ailjiiTUt (ialftctic Cli^ini funiis, \ltai'jirti-cl. )
I
STAK CLUSTEKS
2S1
bbon of aters inclosiDg three blank circular spaces of sym-
letrically varying diameters.
Ainong the '* curioaitiea " of the heavens are to be reckoned
laaters within clusterBL Thus, a large loose collection in
emini {N,G.C. 2331) involves a neat group of "six or
5veQ stars close together, and well isolated ixom the rest." '
parallel instance is met with in N.G.C. 2194, situated where
le Milky Way passes between Gemini and Oriou ^ and within
|ha bright cluster M 67 in Cancer^ Dr. Roberta was struck
rith a knot of five stars of tenth to twelfth magnitudes,
■their photo -images touching. If they should be proved/*
le added, " to be physically connected, the revelation would
be astounding."'^
Star- groupings of singularly definite forma frequently
occur, A triangular swarm (N.G.G, 7836) presents itself
in Cetus; a rectangular area in Vulpecnla {N,G.C. 6802)
is densely strewn with fine star-dust. Clusters shaped like
half-open fans are tolerably numerous. One in Gemini, if
removed to a sufficient distance, would appear^ according to Sir
John Herschel, "as a fan-shaped nebula with a bright point
like a star at the vertex." Another specimen of an " acut-
angular" cluster 2' in length (N.G.C. 7510), is bounded by
" two principal linea of stars drawing to one." ^
In Cygnua is an oval annulus, 4' across (N.G.C, 7128),
of stars centrally surrounding a ruddy one of the ninth
magnitude^ A similar elliptical group, with a double substi-
tuted for the red star, is centrally placed in one of the two
great adjacent clusters in Peraeus (K.G.C. 869).* This
superb object, like the scarcely inferior assemblage (N.G.C.
884) it immediately precedes, was regarded by Herschel as
merely a protuberance of the Milky Way, and his intuition
was probably correct. The two togetlier form a telescopic
pageant such as, in the wildest flight of imagination,
Hipparchus could little have dreamed would one day be ■un-
rolled before the eyes of men out of the "cloudy spot" in the
Bword-handle of Perseus which he (it is said) was the first to
1 Trans. J?. liuhtiii Sag, p. 66.
^ CeUstial Phoiographs^ voL i. p. fl9.
* Phil, Trans, yo], csKiii. pp. 476, 603.
* J, HcrBcliel, Phil. Tram. yqI, cxiiii. p. 573.
» I »— ♦
^- X -
-r - ; r — -
• T \r- T
A
.k.V . A.V ...
.■..'. :r:-i V. ::;:■ • ::.: .::•::.:- :y Mr. H. C
Hi ].^72.' T:.-- :! -:.■■•. ^vi- :■ '^ liiu *'''.: ■
it 'Iw ill i'mI iJiov-;. .-.:.".-. '.•.'.■.lii :■►■ rif ox'.r
iKj'i'-r Ui*- < ij'-uiij'*. ii:- ■■-. th-y 1,'uly liii--.- u
'■I..iii;'f, -ill' •: H'-l -•■!.■ 1'- liiL'.i-'Urcl:;L-:its ^\
h.T-,iy t'j i/" iiiihul<-]y i"li.il']t.'.
' .Sr, rl,, OW-, ji. f;.'. - As*r. .
' /Ar St,.n\liiv<' i\ X I'crsei, p. S
* Moathhj Xnii-ys. v-l. 1. p. :jl;
^ '.V/^'c (itistrriitiotis, }>. 17. " Month? u Sot
STAB CLUSTERS
233
la the constellation Cancer may be seen, any fine night in
iter, a blot of dim light placed midway between two fourth-
agnitude stam The stars were called by the ancients the
Aselli, the interposed cloudlet representing to their
a " Manger," FroEsepe. Since its disappearance was
£oned a sure presage of itiin/ a good deal of popular
attention was paid to it, and its stellar constitution was one
of the earliest telescopic discoveries ; but only preliminary
steps have been taken towards its exact investigation. Of its
components^ thirty are measurable on Rutberfurd'a photo-
gmpbs, and 363 were mapped over an area of three square
degrees by C, Wolf some sixteen years later, eighty-two among
them being carefully determined as points of reference for their
fellows,^ Asaph Hall's catalogue for 1870 of 151 of these
stars has already been turned to account by Sch ur of
Gottingen for testing the relative fixity of 45 among their
number,^ previously (in 1858) measured by Winnecke with
the Bonn heliometer ; * but no assured results as regards
either their concerted, or their individual movements, have
yet been elicited. Most of the stars in Praesepe yield spectra
of the solar type."^
The particles of a drop of water are not in more obvious
mtitual dependence than the constituent stars of globular
clusters ; *' the most magnificent objects/' in the elder
Herschel's opinion, " that can be seen in the heavens " Were
there only one such collection, the probiibility of its separate
organisation might be reckoned " infinitely infinite," and one
hundred and eleven of them were enumerated by Sir John
Herscbel in 1864. It does not, however, foUow that the
systems thus constituted are of a permanent or stable
character ; their configuration, in fact, points to an opposite
conclusion. There may, of course, be an indefinite number of
arrangements by which the dynamical equilibrium of a " ball
of stars " could be secured ; there is only one which the
present resources of analysia enable us distinctly to conceive.
> AtBtOB, IHoaeineia, tt. 160-180, 265 ; Tbeophrastus, Ds S^Kis PluviaruTTi,
ed. EeiutttQi, p. 419.
= OoTtiptcs RfndKS, t. lOT. p. 333.
' Attr. Milth. der 06ltingenji^n Stemtcarte, 1S95.
• Jbui, Tb. ii. ; Naturt, toL lii, p. &1B,
' Fiokerlng, Harvard AT^-naltf vol. uyi. pt. iL p. 26i<
S34 THE SYSTEM OF THE STABS
Tbi» was adverted to, mAaj years aluce, by Sir John H(
Kqual revolviog maascs, uniformly distributed throughoot i'
ephezieat space, would be acted upon by a force Taijiug
diruUy as the distanoe from, the centre. The reason of Om
is easily seen ; for the further out a component of such a
system is located, the more matter there will be ioside, and tk
> leflB outside ite orbit. The strength of the oentral pull thm
j ffeaohes a maximum at the surface of the sphere, the velccity
by wliich it ia baUncefl growing in the same propomoa
Ellipses described under these conditions would all, acoord-
i ugly, have an identical period; whatever their eccentricilit*,
iu whatever planes they lay, iu whatever direction they were
traversed, each would remain invariable j and the harmony of
a system in which no perturbations could possibly arise, would
remain unbroken for ever, provided only that the size of the
circulating bodioa, and the range of their immediate and inteti^
attractions, were insignificant compared with the spatiui intei-
vals separating them.
But this state of nice adjustment la a mere theoretical
possibility. There is no likelihood that it has anywhere an
aotual existence; and the stipulationa, upon compliance with
which its realiaation strictly dependa, are certainly disregarded
in all the stellar groups with which we have any close
acquaintance. The components of theae are neither equal
nor equably distributed. Central compression^ ov^r and above
the merely apparent effect of the gradually increasing depth
of the star-strata presented to the eye, is markedly efifecUve
iu globular clusters. Professor Pickerings from careful photo-
graphic counts of the three typical specimens « Ceutauri, 47
Toucan i, and M 13 (in Hercules) deduced the rule that the
number of stars per square minute of are increases in arith-
luetical progression with approach to the middle point.* Real
crowding thus intensifies the " blaze," where the stars run
together, even with powerful telescopes, into an indiscriminate
silvery eflFulgence.
Sir John Herachel acknowledged his embarrassment in even
trying to imagine the *' conditions of conservation of such a
system aa that of ta Centauri or 47 Toucani without admitting
' OuUin^s of Astronomy, 9tli ed, p, €36,
* Harvard AnnaU, vol. xxri. pt. il p, 21&.
SXAB GLUSTEE3
235
pulaive forces on the one hand, or an interposed medium
the other, to keep the etara asunder." ^ Tims compacted
kto a whole, they might, he thought, instead of revolving
iividnally, be supposed to rotate in their corporate capacity
a single body. But the efltablishment in such aggrega-
Dns of a " statical equilibrium " by means of an " interposed
liam," ia assuredly chimerical. The hypothesia of their
station in one piece is countenanced by no circumstance
inected with them. It is decisively negatived by their
Tularitiea of figure. The shai-p contours of bodies whirl-
on an axis are nowhere to be found among these objects,
aeir streaming edges betmy a totally different mode of
misation.
Globular clusttira commonly present a radiated appearance
their esterior parts. They seem to throw abroad feelers
ito fipace. The great cluster in Hercules ia not singular
in the display of " hairy-looking, curvilinear " branches. That
in. Canes Venatici (M 3) has "i^ys running out on every side"
from a central mass, in which " several small dark holes were
disclosed by Lord Rosse's powerful reflectors;' showing pretty
plainly that the spiral tendency, visible in the outer regions,
penetrates, in reality to the very heart of the system. From
a well-known eloster in Aquarius (M 2), " streams of stars
branch out, taking the direction of tangents." * That in
OphiuchuB (M 12) ia provided with long straggling tentacles,
gf a "slightly spiral arrungement," according to the same
aathority. And a remarkable assemblage in Coma Berenices
(M 53) was described by Herschel and Baily as "a fine com-
pressed cluster with curved appendages like the short claws
of a crab running out from the main body." * The peculiarity
in question is the more significant that it is shared by many
undoubted nebula?,
We find it difficult to conceive the existence of " streama
of stars" that are notjlowin^; and accordingly the persistent
radial alignment of the components of clusters inevitably
gests the advance of change, whether in the direction of
1 Cape 0b*crmtiQn9, p. 139.
" Trans. It. Dub. Smi. vol. ii. p. J32.
' Ibid. p. 162.
*■ FhiL Tram. rol. cixiii. p. 4GB.
236
THK 3TSTEM OF THK STABS
€opoeate»tkio or td diflbvcn. Either the tide ai mtntiual i
Httuig iavmrd^and the * f Iwtf wring pows** (to ue & bvonisi
phnMB of Sir William BacadifllV) is ttSXl «^M*wfcg itadt to
collect atus from smrooiidii^ ii{»oe; or elae a ffintfifiyl
ini|witoft predomxaato^ bj niicb (lUl-grovn orts are diii«
from tfae Dfuaesj of ■obs in wbieb Uiey irei« leared, to Mek
tbesr 80pante fijitma^ and enter on an independent qmbk
6hBwbcire> Bat the qneoCaon «• to whether aepazatiit <r
a ggrr gtti-fMifirt tendeociai pietail in globular closteis in, for the
p ree c ot^ beyond the range of profitable di^cnasioEL All tbil
ean be eaid i« that, after Ihe lapee of aome oenturiea^ photo-
graphic maararenients 10^7 help towardfi deciding it.
An object viaoallj teaembling a blurred star below th<
fourth tnagnitttde, woa named hj Bajer u C«ntanii It neter
rUeb in theeo latitudes^ but Herschel^s great reflector rerreaied
it to Mm at the Cape aa a ** noble globular cluster^ beyood all
compahsoQ Che rtcheat and larg^t object of the kind in the
heaTen&" ' The stara coDtained in it are, strictly epeaJdng,
innumerable About 6400 have been enumerated from the
best photographic platea;^ but a residuum of mottled bax
indicates the reckoning to be far from exhaustive. Those
iudiTidoalised are nearly all brighter than the fonrteeatk,
fainter than 125 magnitude; and no less than 125 amotig
them have been found by Professor Bailey to flash and fade io
periods ranging from 475* to 6** 11". The diameter of this
stellar swarm is put at 40', but eome 1600 of its appatent
coufititueute are held to beloug to the general population of
the aky.
The lovelineaB of the cluBter 47 Toucaai near the Loooor
Magellanic Cloud was, to Herschers view, set off by a divemty
of colour betweeu an interior mass of ro&e'tiuted stars and
marginal strata of purely white ones.' But the effect was
doubtless eubjecLive ; it met with no later recognition ; and to
the present writer, in 1888, the fiheeny radiance of thifi
©xquiflite object appeared of uniform quality from centre to
circumference. A photograph of it, secured November I7j
Oapt ObMervations, p, 21,
) Aiir. avd Aair^h^ticMf tqL xii p- SH ; Sarvitrd Annalt, vol. nxviiL
' Cape ObaervationM, p. 18.
STAB CLUSTERS
23r
)02, aC the Royal Observatory, Cape of Good Hope, is,
jugh the kiudnesa of Sir David Gillj reproduced in Plate
[L, Fig. 2, Probably no other cluster exhibits an equal
ee of conipresaioD. Withia a sphere of 11' radius are
luded mgh upon 10,000 stars, of which 5019 have been
ly counted.* The blanknesa of the auirounding sky
idera 47 Toucani all the more obvious to unaided aight; it
indeed, for several nigbta after his arrival in Peru^
staken by Humboldt for a cornet-^ Only eight variables
ive been detected in it — a scanty gleaning compared with
rich harvests gathered in & Centauri, and in the starry
sberes M 5 and M 3, situated in Serpens and Canes Venatiei
ectively. The last-named collection shelters at least 132
ckering lights, being one in seven of its individualised
ttmponente. Those of several other elusterSj nevertheless, shine
ith remarkable stability ; and these eontraata seem unrelated
I diverBitiea of Btructure or quality In the groupa manifesting
lem.
The gradationa of lustre are, in many of these aggrega-
tions, distributed on a clear!y traceable plan. As a general,
if not an invariable rule, the smaller stars are gathered
together in the middle, while the bright ones interpenetrate
them in rows and branches. ThuSj of a magnificent cluster
in Sagittarius (M 22), known since 16G5, the central portion
accumulates the light of multitudes of excessively minute,
and is freely sprinkled over with larger stars. Sir John
Herachel remarked of a cluster in the southern constellation
of the Altar (N.G.C. 6752) : " The stars are of two magnitudes ;
the larger run out in lines like crooked radii, the smaller are
maBsed together in and around the middle."" A similar
arrangement was noted by Webb * in the Canes Venatiei and
Coma Berenices clusters (M 3, M 63), aa well as in the
imposing collection in Serpens above referred to, the more
condensed part of which (compared by Sir John Herachel to a
snowball) seems as if " projected on a loose, irregular ground
of stars." s
* Bailey, Edrvard Annaht rol. xixriii. p. 349.
' Cosmos (Otti'strana.), vol. iii. p. 193.
* C&pe ObserAktiiona, [}. lie.
* Student, vol. L p. IflO.
' PMl. TranM. vol. csuciii. p. 3£0,
i»9
TOR STSTDH OF THS STABS
ZrreguUhtitt of distiibatmt in
A Gm
highi J ffiigtitttKTi
At TummmowvL, in 1850.^ tins
" du-k Udm,* Mftwting fti a point cooaiAetmhkj remofvd fm
tii«i ceiatret wen peiueired to mterropt the briHiaai^ of tbs
globe of 8Un in Heieaki (M 13> They wen aftenrai
noogniaed bj Bnffhun and Wdib, and reoorded tbaoaadva
with emphaAA i& a pbotogr^h taken by Dr. Soberts in 18 ST.
Globular da«t«n in Ophttichixii (M 12^ ia PegaooB (M U),'
and ia Caoee Venatici (M 3), appear to be sinailari/ toBneUeiL
PreooDceiv«d ideas as to the awcfaanism of oelfiotial spbem
are ntteiix ooofoiuidod bf pheDomena not eaaOr recoDdUhk
with the proaecuUcHi erif any otderly schente of cimdatefj
movement. The aeeniix^ rifts, bowe^'cr, are not afaaolutilf
vacant. A slndy of the cluster in Hcrcnlefl (M 13} Vt
Mr. H, K* Palmer,' &om plates ezpoeed with the Croesky
reflector, brought oat the aingoJar fact that its cozopodtttt
fall generally into two orders, the distiibuUAii of which ■
radicaUy dlBTeiieiit. The faint stats, or those below
miigoitude, are scattered with fair uniformiCy throng]
spherical epoce ; thoee brighter obey a streaming
and the gaps between their ramifications show ae dark
Tha Bame exphmatioti is doubtless valid in all siioilar
BiffereDcee of distance are alooe adequate to account
the variety of texture observable in globular clusteraL
in Aqoahiis^ for instance, likened by Sir John Heivcbel to
heap of golden sand/' might very well be the domewhat
grained Hereulea group withdrawn as fer again into
At a still further stage of remoteness, the appear&noe
presumably be reached of a stellar throng in the Dolpl
(N.G.C. 6934), which, with low powers, might pass for a
planetary nebula, but under stronger optical ootDpuIaion
assumes the granulated aspect of a true cluster. And many
more, their genuine nature rendered impenetrable by exceeeive
distance, are possibly reduced to the featureless semblance of
" irresolvable ** nebulse.
But there are real, as well as apparent diversities in these
objects. Although smaller and mote compact clusteia must,
* Pfiil. Trans, vol, cli. p. 732.
» Webb, Oil. of^t€tM, p. ara.
* AalToph. /ourm. tah i, p. 240,
riiul't^taplis of tSuiillierii riideieal Ulijctits.
fi«. 1. l>iiui*4£nM'l' -^1 Me-isJtT ^. Liki'M with tlu^ Bruce Titl*iin.Dpe liy H. I.
g. "^ PliifiogMiili nf 47 ToTicjinw, taken nt llit^ Mayai Ohw-rTatory, Cspe of
STAB CLUSTEKS
239
on the whole, be more remote than large, looaely-formed onea,
yet " this argument," Sir William Herachel remarked, " does
not extend so far aa to exclude a real difference which there
tmay be in different clusters, not only in the eize, but *lao in
the number and arrangement of the stare." There may be
Ifc globular clusters with coinponenta of the actual magnitude of
ll Sirius ; others, optically indistingulBhable from tbem^ may be
aggregated out of eelf-luminoufi bodies no larger than Mara^
or even than Ceree or Pallas. Our total inability to locate
them in Bpace leaves us without the means of judging. Nor
are we likely to be better provided in this respect for an
indefinite time to come. AU that can be done is to make a
supposition, and trace the coneequences. Let our example be
the great cluster in Hercules.
"This is but a little patch," Halley wrote in 1716, but it
shows iteelf to the naked eye when the sky is serene, and the
moon absent.^ Messier termed it "n^buleuse sans ^toiles";*
yet a " twinkling " indicative of ita stellar character may
l^e caught with a tele^ope four inches in aperture ; and a
powerful instrument resolves it to the core. Within the
precincts of Halley's " little patch," Sir William estimated
fourteen thousand stars to be " cribb'd^ cabined, and confined!"
The apparent diameter of this object, including moat of
the " scattered stars in streaky maasea and lines," ^ wliich form
a sort of "glory" round it, is 18'; that of its truly spherical
portion may be put at 14'. Now a globe subtending an angle
of 14' must have a real diameter y^^ of its distance from the
eye, which if we assume to be such as would correspond to a
parallax of -^^j of a second, we find that the cluster, outliers
apart, measurea 1^600^000 millions of miles across. Light, in
other words, occupies about ninety-seven days in traversing
it, while it needs siity-five years to journey thence hither.
Its components may be regarded, on an average^ as of 13'5
magnitude; and Mr. Palmer reckoaed at 5482 the number
distinctly printed on the Crossley plates.
If, then, 6500 atare be supposed uniformly distributed
through a sphere 1,600,000 million miled in diameter, an
^ FMl. Tra-ru, vol. iiii. p. 392.
* Conn, dea Timps, 1784, p. 233.
* Fhil, TroHM. toL oxxtu. p. 4fi8.
240
THE SYSTEM OF THE STARS
interval, roughlf^ of 61,000 millJOD» or more tbaa
five time» the dbtance of Keptune from the son^
each froia its ne&reBt uclgbboar.^ Upon a spectator ia
intermediate eituatton* six stars (beddeB crowds of gt^i
inferiority) would shine with about sixteen times the 1
that Sirius displays to uis. Yet since 625 milljoa st&n
thia brilliancy would be needed to supply the light we
from the sun, the general illumination of the cluster
greatly exceed the qualified darkness of a star-lit aight.
At its aurmised distance, oar 8un would appear as a
of 6'3 magnitude ; it would shine, that is to say, about 7'
times ss brightly as an average one of the grouped objectt
Each of these, otxordingly, emits ^-^ of the solar light; uA
if of the same luminosity relative to mass as the sun, it
exercises just j^^ of the solar attractive power. The tniSB
of the entire system of 5500 such bodies is aooordiog^
lees than one - third that of our sun. This may be
r^arded aa a minimum estimate. The probabilities are in
faTOur of the cluster being vuatly more remote than we haw
here assumed it to be ; hence composed of larger or brighwi
and presumahly more mussive individual bodies than reeoltt
from our calculation.
No insight has yet been obtained into the mode of fo;
tion of globular clusters. Their antecedent state re:
wholly obscui-e. True nebidosity appears to be absent fr^sm
them. All those examined by Professor Barnard with the
great Yerkes refractor proved throughout unmistakably stelLir.
The nebular relations of leas condensed groups are, on the
other hand, frequently very close ; and their photographic
study has amply justified the conjecture that the two dasflflB ,
of object form an UDbroken series — that clusters exist i^fl
every stage of development from nebulae, and that the advan^
cing condensation of many nebulae will eventuaEy transform
them into veritable clusters. Suggestions to this effect derived
from analogies of forra^^ are corroborated by numerous observa-
tions of the actual coexistence with grouped stars of nebulous
masses. The Pleiades is the palmary but not a solitary
^ Seo Mr. J. E. Gore's analAgoiu calculatioiui in Jown, Liv. Attr. Soc*
VoL V. p. 169 ; Studies in Astrvnomy^ p, SO (1(^04).
* Lockyar, Ptw:. R, Soeiety, toL xliv, p. 29.
STAR CLUSTEK>S
241
stance of a hybrid system. A bright cluster of the same
:ral character in Sagittarius (N.G.O. 6530) is obvioualy
mnected with a great nehida (M 8), in tlie meshes of which
it ^eems as if entangled. Yet tht^ two formations are not
Strictly c<;>ncentrie. The cluster followSj while it overlaps
the nebulii. Nor do the coamic llowules adhere 80 closely to
individual stare as in the Pleiadtra. Plat^j XII., Fig. 1, shows a
photograph of the combiuatioii taken ut Arequipa with the Bruce
telescope, June 11. 1896 ;' and a group of nebulous stars iu the
ittitiit-'diate neighbourhood was detected by Professor Barnard
on it plate exposed during four and a quarter hours, June
K. 1892.
A suggestive photograph of a "cloudy vortex"' in Mono-
,j^^'os (N.G.C, 2237-39) was taken by Dr. Roberts, Marah 5.
1899. Within a series of annular undulutious (so to c^ll
them) of nebulous matter covering a aky-space one degree
across, a straggling cluster is centrally situated. The associated
effect strongly recalls that of Nova Persei with its web of
glimmering whorls, and intimates possibly an analogous
genetic tie.
The gpectm of clusters while, in the main, continuous,
are probably not devoid of individual peculiarities. Sir
William Huggins was struck, in 1866, with the absence of
red rays from the analysed light of the great cluster in
Hercules, and perceived in it irregularities due either to bright
or dusky bands." They were construed in the latter sense by
Vogel in 1371,^ since when the inquiry has been unaccountably
neglected. With the powerful Lnstrmnenta of modern con-
struction, it might, nevertheless, be profitably extended by
spectrograph ic means to many globular assemblages; and the
leeults to be expected from it are a nne qud non for advancing
much further our imperfect acquaintance with them.
' Harvard Uircular, No. 15.
^ Mrii. Roberta, Journ. Brit. jtMtr. Art. vol. xii. p. Ill ; aae ftlsc Barnud,
Astr. ^ach. No. 2916, Jstr. and Aatrophj/ticf, vol. xili. pp. 173, 642.
* rhii. Trans, vol, clvi. p. 339.
,* Aatr. Nach. No. 1B64.
I6
with
fMfcoa ty gwiHiUKin^ hmbI Khe —C^crte of
ia tiw adovia flpivo^ HeMs wnv to be ibend in tk
«i tiagib CiMl brasfaai^ hwimTW ; ihej
eaMBltf7> •u^iuau, oamaam^ Taaeiii
Aieldiy mihf—il with rtai^ or liaded like tbe cpa i(
irhwia, diiplaTfld itwiiiianlw^ m weB m nebttloin diar^ ag^
ih— ill, triipglw^ panlMogniM^ twin and teiple rjjihf
One ndnlft^ Uioaght to nfWw the fMse ai an owl, sm
Mined Moovdingli'; aaother waggeatad a oah; * tiuzd a
■wan ; « fotxitb (tbe great Onon fomation) became known ■
the Flab Month nebula, trom it* toppcned UteieiB lo tbe
g^ing jaws of a marine moorter Fancy ranged nl Urge
UuDogb thia wide radn, attemptang to fiamiliariae itaetf
with the strange objects ooDtained in it by* finding for thoa
terreatrial aimtlitudeaL
Within the la«t few yean, however^ — indeed, it maj Ik
naid, Hioce the completion of the Roase reflector in 1845, —
iMbiUar ioquiiied have entered upon a new phase. A " glim-
Otfrmg of reaaon " haa begun to hover over what kmg appealed
a aoeoe of hopeless bewilderment;. With improved tel^oc^
mains above aU, with the aid of photographj— ^m^iurf hae
blOOBM iuere&»iiigly manifeat among all n1«iffp^f of nebulie.
^tmcture, not of a finiflhed kind, bat indicating with great
212
^
THE FORMS OF NEBULA
243
probobility the advance of formative processes on an enormous
scale, both as regards space and time. Masses that seemed
all but asDorphous when imperfectly seen, ehow to a keener
scrutiny nodes aad nuclei of condeDsafcion ; curbing lines of
light, telling of the presence of movement and force, furrow
theoi ; they are perceived to be rifted as if by a colossal
thunderbol t, or riddled as if by a portentous cannonade.
Simple milky eflusions prove to be far less common than had
been supposed, and exceeaive comple^ty of constitution is
already a rec<»gnisable characteristic of most nebula>.
It is one which adds greatly to the interest of their study.
For a5 the curious details of thi?ir organisation are laid bare
by the intricate inequalities of their light, the prospect grows
hopeful of gaining some insight into the nature of the systems
formed by, or in preparation from them. Optical discoveries,
while gradually acquiring phyai&il significance, are helping
to lay the foundation of a " nebular theory '* emanating from
augmented knowledge, and the discreetly adventurous thoughts
which it may be supposed to countenance.
Meanwhile, some mode of nebidar classification has to be
adopted for the guidance of our ideas ; and since their rapid
modification through fresh detections allows no arrangement
to be at present more than provisional, it will be best to
depart aa little as possible from that already in use. We
may, then, for descriptive purposes, divide nebulse into the
following eight classes, which, nevertheless, frequently over-
lap so widely as to be barely distinguishable : — ( 1 ) Nebulous
stars; (2) Planetary nebuliE ; (3) Annular nebulee; (4) Comet-
ai-y nebulffi; (5) Spiral nebuhe; (6) Double nebula; (7)
Elliptical nebulae; (8) Irregular nebulaa.
In the course of one of his " reviews of the heavens," Sir
William Herschel discovered a star in Taurus " perfectly in
the centre " of a " faintly luminous atmosphere" about 3' in
diameter.^ The consideration of thig object (N.G.C. 1514)
and of some others like it, led him in 1791 to the memorable
concluaion ttiat there exista in space " a shining fluid of a
nature totally unknown to us." Nothing, indeed^ could be
chiartir than that " the nebulosity about the star was not of
a starry nature/' and there is just as little doubt that it is
' rhif. Tram. toI. Ixni. pp. 71, S2.
Roberti't pbtai is 1889;' end Pt u J U M y i r BartiArd's phol»-
gmphic explontuaw hȴe jielded munemos exampln of a
nmiUr nature aoiuetuMe tifmbtH into multiple gro^
Anmig ^ir John HeracbeTa aoathem dtnoTeries wms * dtfi.
dlATply'^tLned doitt:^ star stntoonded by a bright laminoos
** fttmoiiphere " 2*10 extent * (N.G.C. 536") : one of Bumltam's
close pMis lA in atow revolutioa, as already mentioned, at the
b«arl of the nebula N.G.C 2182 ; while nebulous spoctroooo|nc
binArieii, despite their upjtarentlj lucongmoua cimuastancM,
are b^iiiiUDg to take luuk auiong the ordinary products itf
the Mdereal world.
A " nebiilouB star " proper foroi8 the centre of an ill-
defined aureola ; but nebulous adjuncts to stars exist in em;
variety' of branches and cberelureav wiaps and whorlo, In^
dtAd the sequence is so eonttnuou« between bright stars with
filmy appendages, and pronounoed nebutie involving minute
stars, that it is often difficult to say vrbether the stelltf
or the nebular character predominates. Thus, "planetary"
nebulfir haTe^ witli mre exceptions, stellar nuclei; they can be
discriminated, however, from nebulous stars, finat, by their
protlnrninanlly gaaeooH i^ctra, next> by the definite terminatioo
of their disn:n.
It ifl then no wonder if, among Herschel's nebulous stars,
one wiiH found not strictly entitled to bear that name, Thia
nooduKript objtrl C^*G-^'^ 2392) is situated in Gemini, and
' Tram. Ji. Dub. Soe. v&i. ii, p. 40.
• Sidertat MesMetigrr, vol, it, ji, ^8.
' Uvnthly yoticet, vol ilix. |». 363.
* Qt)nt ObKTvations, pp. 23, 10/,,
THE FORMS OF NEBULA
245
that it abruck him as somBthing ucusual luaj be inferred from
his designating it "one of the most remarkable pUenonema I
Ke ever seen." * With the Parsoiistown reflector it presented
most " astonishing " appearance. Herachera ** equally
used nebulosity" was replaced by Eieverul bright and dark
rings, various in breadth, and perhaps spiral in their arrange-
ment.^ The diameter of the combination is about 45"» and
donbta about ito nature were set at reat by the dictum of the
spectroBCope. D'Arrest" found its light to be concentrated in
the green ray of uebidiuni (wave-length 5007) — the central
star or nucleus a^^erting its superior t-xjudensution by the dis-
play of a faint continuous radtauL^e. It ift then essentially a
nebula, and generally paBses for one of the annular, or
perforated kind. A truly nebuloua star of a reddish colour,
make8 with it (not^ we may Burmiae, fortuitoualyj, an open
pair at 105''.*
A nebula in Afjuila fX.G.C, 6781) presents analogies
to HiTscliclft burred star in Gemini. -T. Herschel con-
sidered it to be of planetary nature ; but the RoBse reflector
showed a sudden diminution of brightness towards the
middle,^ and lUmard unhesitatingly pronounces for its
annularity.^
Planetary nebuLe were first distinctively adverted to by
Sir William Hersehel Their classification caused him a good
deal of perplexity. " We can hardly suppose them " he re-
marki'd at starting, '- to be nebulae ; their light is so uniform
ae well aa vivid, the diameters so small and weU-defin<idj as
to make it almost improbable they should belong to that
Bpecies of bodies." After he had weighed and found wanting
the hypotheses of their being actual planets belonging to
distant suns, or distended starsj or comets near aphelion, he,
nevertheless, (it last decided — rightly, as usual — in favour of
their nebulous nature/
^P Hit. Trana. toL btutL p. 81.
'^ Trana. B. Dub. Soc. rol. ii. p. &0 ; ue also H. C. Key, Monthty Nctitts,
vol. xxviii. p. ]&1.
' Atir. Nach. l^o. \^%h ; Abhandlunfjeii, LuLpsi^, Bd. ili. p. 521.
■* lAieellj, Menwira R. Aeir, Soe. vol. IXXTJ. pp. 42, Q\,
'■ Tram. Ji. Dub. Soc. vol. ii. p. 50; Fkil. Trtmt. 1801, p. 752.
* Monthly Noiit<s, voL Ix. p. 250.
I? Phil. Trtrnt. vol. Ixxt. p. MS.
THB SYSTEM OF THE STABS
Tifij of them vere kmemn wben PidDehBg tifgin
lag" in 1881, for "ttmn with reouxkablft np&gUm*;^ tad,
vrithiin a few yeai% npwanU of tweotj more were identiiiei
throng the qtuiUtf of their light aloDe, bj him and Dr.
CopeUzMi Tbe«e are. ])ow«Ter, devoid of the oooagitBooA dis
which waa the ori^nal had^ of their das ; thef are eithtt
very smalls or very remote pUnetariea ; and are oftca &
LLDf^ubihcd as " aIoUat nehal^e."
A true " plaaeUiry " aapect haa not, indeed, in an^ oMt
8unriTe<l the acrqtiiiy of modem obserrere. What had weemA
equably iUummated discs arc broken up hj the poweriiil tefe-
■copea now iu use, into brighter und darker portiocw, &
tributed in evident rebitiou to some unknown conflict of forott
Some of these discs include atrongly-tuarked nuclei ; others i
iprinkliDg of minute stars ; oondeasation towards a spheixtl
mir&oe givefl to muny the uspei-t of a ring-shaped encloeon;
few (if any) ure clean at the t'dges.
Not li few are seemiii|^lj multiplex. Two or three super-
polled djsoa are traceable in them, hinting at a morphotogicdl
history Bimilur to that of disturbed comets.
^fl^^^ Thus a small oval planetary (N,(_i,C. 6572) in
^^^Hl Ophiuchus wa£ resolved by Vogel with the great
^^^H I Vir-nrtti Ti^fractot in 1883,^ into three strata of
L v|f . ii^'i'iilosity ilifiposed as in Fig. 28, representi^.
y no doul.it, flUL-tesaive apherical imd elliji^pidfll
- - ' ujivtilupi'B uT lUminishiiif^ luminous power,
""mWJ 01^; An abJLHit CN.G.C. G210) with an "intense'
N.b,.iMV«ff.i). i^j^^, ^.^j^^j^ j.^^-j,^ ^p^ ^^ ^j^g distance aU round;'
ttiid huzy *4t tho odges,^ was i>eTCeived by Vogel as triple^ A
faint oval husk (ao to speak) seemed to enclose a vivid keruel.
aud that agtiin to include a stellar nucleus. This nebula is
aituated iu the constellation Hei'cules ; and one of a simi
oharocter in EridanuB (N.G.C. 1535), waa described at Pi
aonstown as preseutiny a grauular. Nile-water blue disc 18
(MT088, including a atelkr nucleua, and encircled with a faiui
atmosphere** Mr. Lixssell noted the combined eflect
* Obtervatory, voI». iv. p. 81» r. |.. SB-I ; MotUhlif iVotiett, ToL xIt. p. 91.
* Potsdam PukHeatimm, No. H, p. M.
' 2Va)t3. li. Dub. See, vol. ii, p. J60,
* /Wrf. p. 41.
THE FORMS OF NEBULA
247
Jextraordiuary and beautiful" ^ Such " nebulous nebulae " (to
row Dr. Swift's phrii^)'^ are among the most enigmatical
' celestial objects.
or special interest ttmoDg planetary nebulse is one lying
lite close to the pole af the eeliptiic, near the star tn DracouL*
r.G.C. 6543). Its longer diameter (for it is slightly
Uptical) measures about 30"; it is of a blue colour, and
iowe a white star of eleventh magnitude giving a perfectly
itinuons spectrum exactly in the middle of a diac from
rhich a purely gaseous one ia derived. Sir William Huggina'a
fit experiment in the analysis of nebular light wae in fact
tied upoti the planetary in Draco, which has in varioua way&
en used aa a test object- Attempts to determine its parallax
ere vainly made by d'Arreat, Briinnow, and Bredichim* For
aper motion, too, it was tested by d' Arrest in 1S72, with a
lilarly negative reatUt. During the eighty -two years*
iterval since a careful observation by Lalande in 1790^ the
ebula had remained to all appearance completely stationary'.
lut this fixedness was really to some extent communicative
regards its •minintum distance from the earth. D'Aireat
iowed that unless this exceed a light-journey of forty-seven
yeatB, the nebula must have become sensibly displaced in the
course of eighty-two years by the simple perspective effect of
the sun's advance at the rate of five miles a second.* Now the
solar velocity assuredly does not fall short of twelve miles a
second, while the term of the nebula's seeming immobility
has become protracted from 82 to 115 years. The estimate
of its distance needs, on both these gi-ounde, to be augmented ;
and we find, accordingly^ that its light can only reach oui-
eyes after an interval of nearly 160 yeara,^ if then ', for it may
spend a much longer time on the road. The real size of the
^^lobe it emanatea from must be vast iu proportion to such
^H ^ Memtriri R. A^r. Soc. VoL xnvi p. 40.
^B ' Aitr, Nash. No. 3474.
^^B ^ Brdniiow abtamod fbr H iv. 37 a notnlTu.! parallax^ bat Brediohin, from
^^p&arly douMe thi.- number of obserTatiom, derived n negatW4 citie implying thi^
nel>u]a to l>e more rffinotei iliao the tt^ntb-nrngnitudi? star with wbii::b it was
ciJiQpu-ed. AttT, Nach. No, 'i9l€ (OudetuADs) ; Kn'j. Mec, rd. xliii p, 604
(H. Sadler;.
• AaiT. Koch. No. 1885.
' CerrwapoaJtDg to a pAtalUi of O""*)^.
t '^ // I ^ **•** - *"•■
^^^^_^ II y y shape iBdic«t«d w«s t»
^^^^^^ ^fe^^^^^ phatoEBBoii taken at Jtoad*
■ ^^ iB 18»9.* A -bnga, H'
pUiKUrr'* in Sigitta (S.G.C 6905X with a ck«elf U$adr
abt Atf at each mdt,* was eMUj wa ul y wl i&fco a ■yiit ky
M. Antoniadi, with the great Parifl dderosUtt.' His drawrag,
rcproducetJ in Fig. 30* shows the object under a form sjiuilar
to that prcHeuted by the " Great Whirlpool *' nebula uDtO
* Hi/fitKly JifolWt, vol. xlviii. p. sa$ : PuhL A. 8. il vol i p. 36.
• Dii»JiitidrB«, B^il AmIt. Feb, 1900,
' KMler, Putfl, Liek ObMrvatory^ vol. ilL p. 213.
* JCneiciedget vol- iiiii. p. SSO-
THE FORMS OF NEBULiE
249
compelling power of the Rosse reflector was brought to
*T 00 it.
Tlieae are nut iaolattid exiiuipliiB. A consklerable number
' planetary nebulce, as we have Jilready partly seen, Tnaniiest
:)th Hunulir Miid spinil t<?iulBi)cieB, In some a marginal
brightemng gives, with sufficient light-concentration, the eftect
of a ring ; in others, curvilinear effecta of chiaroacuro betray
incipient spirality of conforniRtion. Since they partake of the
nature of all tbe three species, their classification is to a great
extent arbitrary. Five of Herachel's planetaries assumed, in
fact, at Pargonstown a ring-shape.' One of these (N,G.C\
^438). remarkably situated within the eluater M 46 in Argo,
observed not alone to be pierced with a nearly central
n^vity, but to contain two, perhaps three atars, towards one
of which the exterior nebulous ring wound spirally inward.*
A " bole " too diaclosed itself in a planetary in Andromeda
(N.G.C. 7662) observed by Lassell ae biannalar, "a ring
within a ring," To Father Secchi, it had, with liigh powers^
the effect of a " magnificent horseshoe of scintillating points," ■
the glitter of which was alao evident to Vogel.^ It is. never-
theless, like all the memlH^rs of its clasa^ of a purely gaftcous
constitution. The "biannular" planetary is either hazy or
" fringed *' at the edgea, of a bluish colour, and measures
32" by 28",^ An etfuaion from its south-eastern extremity
was pliotc^'uphed by Deslandrea.*
The blue, or greenish tinge distinguishing, to some extent,
all gaaeoufi nebulee, is especially conspicuous in a planetarj^
(N.G.Q. 3918), discovered by Sir John Heischei in the
Centaur, and described as very like Uranus, only half as large
again, its "colour a l>eautiful riuh blue, between Prussian and
verditer green."' And a " sky-ldue likenesa of Saturn"
replaced, in Mr. Lnasell'a reflector, a round, faintly luet^nt
object (N.G.C, 7009) observed by Herschel in 1782 near
the star u Aquarii. With higher powers, the diec became a
26" by 16", hazy within and without; and the whole
* FMl Trails, vol. cil. p, 507, - TbitL p, 5ia.
■ AtCT. Naeh. No. 1018 ; i*s ^oilts, t ii. p. 14.
* Faitditm Fi^litatitmen, No. U, p. 37.
* LaaHQLt, JfemmMjS. Atir. JSm. voL xixtL ]i. 51.
" BtUl. Aalr. FbU, 1«00,
' Ca^ ObstTvalioM, p. 100,
260
THE SYSTEM OF THE STARS
<^
Fto. Bl,— Anriii! ..- ■■!■','.
I Aqusrlii^
interior assumed, under Vogel'a examtcatioa, a corioos team*
shaped atructiirc.' Profo«s8or Holden remarked an uneipeCUd
point of likeness between ihm nebula and the one in Aiidi«-
med& (K.G.C. 7662)^ in the possession by both of a
interior oval ring, singularly vrarped and twisted out of tbe
central plane ; the pei^ulmrtty associating them alaa with
th« helical planetary in Draco. The atue, or handle-Hh
appendages producing in the object near p Aquarii its
resemblance to Saturn with half-opened rings, are a unique
feature among nebula;. First represented bj I^rd Koa£«, thej
were resolved hy I^rofeafior Holden * into distinct luminotf
niaeaes, just tmcrsihly connected witli the main body(8ee Fig.31).
The analogy with sateIUte-«ten
ia tenkptiiig, but may l>e am-
leading. The frequent attend-^
ance of small stars upon nebulc
both planetfiry aad annular long
ago attracted the attention of
Sir John HeracheL' One such
group (N.G.C. S618) struck him as exactly like a planet
and pair of moons, and stan; in slow ti-ausit across a uebuk
of which they are the dependents, may often appear projCNAed
upon it. But not the slightest evidence of movement in theef
ancillary stare has yet been detected.
The typical annular nebula (M 57) was detected by
Darquier of Toulouse in 177^, between and 7 Lyrae. It
confliats of an oval bright ring, 80^' by 60", the interior uf
which is filled with a dim nebulous haxe like " gauze stretched
over a hoop/'* Hardiugj already in 1797, perceived inv^-
larities in the illumtiiation of the ring ; ^ and vivid patches
emphasise the extremities of the minor axis. Minima of
light, on the contrary, terminate the major axia ; the nebula,
as photographed at Her<?ny, September 1, 1886, taking some-
what the shape of a pair of parentheses set a. little apart,
^ but with spiral links between."^ With the Roase
' Potsdam Publicalionen, No. 14, p. 37.
' 3f(nUhiy ^atieet, vol. xlviii. p. ^91. ' Phit. TVafu. tdI. cxxiiL p. 500.
* Sir J. Her»t^lkQj'8 Outlines of J ftr, {>, 644, Sth I'd.
"[alcii'H, Monthly Nolieta, vol. irxvi, p. 64,
• VonGotliwd, Aatt. Naeh. Nft. 274».
THE FORMS OF KEBULiE
251
reflector, filaments of u^bulositj were seen streamiug outward
from the edges ; ^ and the realitj of these singular appendages
was, after fifty-three years, photographically attested with the
Croasley reflector.^
A central star, discerned in thie nebula by von Hahu at
emplin, towards the close of the eighteenth century, was
tnissed by him in 1800,* and has often since evaded the
scrutiny of better provided observera. It appeared on the
Her^ny and Liverpool photographs,* but notwithstanding its
intense actinic quality, left no trace on plates exposed at PaiiB.
T*r. Max Wolf's recent photographs lend aome countenance
to the explanation of these anomalieH by genuine variability.''
This insignificant light-speck appears to be the very punetum
stdieTis of the aurrouuding nebulone orguniam. Professor
Schaeberle's photographs, taken in 1903 with a reflector of
extraordinarily short focus, display it as the origin of a pair
of oppositely issuing branches which, coiling in a clockwise
direction, produce by their amalgamation the effect of a conj-
plex ring,* MopeovePj the ring is now seen to be the nucleus
of a larger formation, 15' in diameter, which embraces in its
dim folds a email nebula, also a " two-branched, left-handed
spiral" discovered by Professor Barnard in 189S. These
surpriaiug results, although needing full verification, are re-
commended to acceptance by the unity they impart to facts
previously disjointed and fragmentary.
A nebula in Cygnus (N.G.C 6894) might be called a
i-eduued copy of that in Lyra, It measures 47" by 41", the
interior vacuity^ which is partially tilled with faint light, 20"-
A conspicuous star is included within it.' An object of the
some kind in Scorpio (N.G.C. 6337) was described by Sir-
John Herschel as " a beautiful delicate ring of a faint ghost-
like appearance, about 40" in diameter."** Two stars, or
nebulouB uode^, are placed in it exactly opposite to each
' PAt'it. Trans. vo\. cirxiv. p, 322.
* Kaoler, Ailroph. JonTti. vol. x, |j. 196-
* Asir. Jahrbue/t, 1802, p. 10.
* Vou Oothftrd, AtCr. A'adt. No. 27fi4 ; 3pitAl«r, ibid. No. 2&00.
B A*lr. iVacft. No. ZaU.
'^ A%(r. Jottrn, NiK<i. &39, 5^7.
' Lord Roue, TraTu. R. Irish Auttl; vol, ii. p, 156.
* Caps ObUFvaiitfns, p. 114.
oUier, aad the whole aspect of the nebiila suggests
remoteness.^
Four ring-nebalm, two in the northern, two in the 9ont
hemisphere, were known to the Herachels ; and^ as we
Been, many 80-caU«d " plimeturiee " show iLunular, as aaM
uebuls ahow spitftl proclivities, Bitigs, in some ins
visibly curve inward towards a nucleus, giving rise to U*
variety which we have designated " eometary " nebuUe. Thiit
a ninth - magnitude star with nebulosity attached (N.O.C
1999) appeared with the Kosse reflector like "a comet ooiM
into a ring " * and was photographed, precisely tindar the ame
aspect, by Dr. Common in 1883.' The triple star, 4. Onmk,
leas than a degree distant, is enveloped in a nebula of au-
logoufl form, which ih also less definitely shown bj tiie
appeudnge nf the star Maia in the Pleiadea. Sir John
Herscbel's *' falcated " nebula ar^ of the same kind. Os#
such in Argo, 10' in extent (N.G.C, 3199) displayed to bio
H " semi'luiiar shape/' dilfu»e ouUide, but with a sharp izmar
edge.* Another (N.G.C. 346) occurs far to the south in
Hydrua "A complete telescopic comet, a praiect miniatuR
of HalleyV''' was encountered in Eridanue (N.G.C. I325'i.
and star-like coudenaatious, with brush, or fan-like appor-
tenances, are not iuifre([uently entered on bis lists. A pair
of amnll nebiihe pliotographed by Wolf and Barnard near Ibe
bright Btar y Oassiopei^e * are singularly perfect examples of
rectilinear cometaries. They imitate precisely half -opened
fans ; the emanation from the star at the vertex has had do
curvature impressed upon it ; it spreads from a point withooi
enfolding it; the rotational twist seema absent.
The discovery of spiral nebulse was beyond question the
moat important result of tlie construction of the great Parsons-
town reflector. Its significance is continually enhanced as ths
wide prevalence of convoluted forms among this whole class
of sidereal objects is rendered more fully apparent by the
increasing advance of esplomtion.
The Whirlpool nebiihi in Canes Venatici (M 51) presents,
^ li&BBell, MsrrunT» Ji. AHr. Sot, toI. xxivi p. 47.
TVonj. R, Duh. S&c, vol. ii. p. 50. * ObMervaiorit, vol. xii p^ 84.
* Cape Obtervations, gjp. '20, 94. ° Ibid, p. &l,
" Aitr. Jfaek. Nm. 3214, 3317 ; Aar. and Astroph, toI. xiii. p. 1S2.
THE FORMS OF NEBULA
263
M^ a gi"cat telescope, a truly amiLzing appearance. Two
slei separately oiitnlogued by t^ir John Herschel ai*e then
to ha conntjcted by an exterior faint sweep Irotii an
^tter system of ivreathiug nebulous banda. These, too, show
cloeities and angularities/ in obv^ious mutual relations, as
the knots, instead of aimply forming upon the spires, bad
entiined, or at least deflected their course, A still clearer
awledge of their arrangement was gained tiirough a photo-
iph taken by Dr. Koberta with four hours' exposure. April
1889.- The nebula displayed itself, no longer simply
led like a watt'; h -spring, hut aa composed of a pair of curving
issuing fi'Dm oppoaite extremities of an oval central body.
Pne of these loses itaelf in a vague effusion, as a comet's tail
iee out into darkness ; the other attains the secondary nucleus,
id there terminates. The spiral character of this great vortex
perhaps rendered exceptionally conHjiicuouB by its being
ore favom-ably placed than moat others for our inspection.
Te seem to get nearly a bird's-eye view of it, and are thus
labled to take in the design of its construction at a glance,
spectrum is continuous.
An object in Virgo 3' acroas (M 99) is a right-handed
Its branches turn the opposite way from those of
51. Their tendency to form ncMie.s and angles was strik*
ziy ahown in a piiotograph obtained in two hours, by M.
Dn Gothard, April 12, 1888.* A dift'uae nebulous masa in
Priauyuluiu (M 33) Just discernible to the naked eye, appeared
rith the Boese rejector in the guise of a " large spiral, full of
iota."* Since it measures 62' by 35', ita real si^e must
prodigious, and its structural dt^tails are of correspond-
ag intricacy.'* Fundamentally, however, the nebula, like
other known members of itM class, doubtless consists of a
"Bucleua and two winding branGln?s, the complex ramiHcations
of which are of what may be culled incidental origin. A
photograph of it, taken by Dr. Max Wolf, Septemljer 26, 1902,
is, with his kind permission, exhibited in Plate XIII., Fig, 2.
Curved furrows of light and shade, conuentrically c^spoaed,
' VogffI, Puhlicationen, No. 14, p, 32.
|[gg*1, AitT. Naeh. No. 2864. * fhit. Trans, vol. i-li. |i. 711.
* KobtrlB, CifMstvU PhotoyraphJ^ vol. ii. ji, 8&.
THE FORMS OF NEBULA
25&
Gt85,^ makes probably the closest pair known; and a
k^ifl reproduction, with greatly widened gpatial intervalu,
^tiar syatems like that of y Aadi'omedBe, occurs in a triple
^Xxla in Virgo, conaiatiiig of a bright round nebula attended,
distance of 5', by an extremely faint one which is itself
t>\e* (N.G.C, 5813-14). ^Viiother compound object of a
ig character was noticed by Sir John HerscheP in Canes
atici (N.G.C. 4631), where an enormously long ray of
kolosity has a round, dimly luminous companion, a tenth-
^^itude star placed between i*er\Hng perhaps as a centre of
taction for both. In other cases, the syateiuic association
individual stars and nebuke seems tolerably obvious. Merope
the Pleiades, as we have seen, claims the attendance of a
ay satellite ; and Dr. Swift observed at Echo Mountain an
irently quadruple star to be really composed of two pairs,
apart, each condsting of a star and nebula.
A very close double nebula in Gemini (N.G.C 2371-72)
also an intervening star symmetrically located in the line
their centres.* Cirrus -like atreaks of nebulosity
tially encircle the two objects. Duplicity is, in other
9, still less clearly defined. Thus, a pair of nebulie near
Leonis (N.G.C. 3226-27) are together enclosed in a faint
linous envelope, the effect recalling that of the celebrated
'Dumb-bell*' nebula in Vulpecula (M 27).'^ which ia only
eived to be eseentially single wlien the " neck " uniting
vo conspicuous hazy masses is brought into view with a
ttwerfnl telescope. Sir John Hei-scbel first observed the
Uptical outline of the entire to be rounded out by faint
iminosity, and thus saw it in its true aspect as a large,
iversified oval disc^ measuring about o' by S'. It might
adeed be called a magnified planetary nebula not devoid
annular inciinations. The eventuality that by the
reaa of the central contraction and marginal spreading
indicated by its present hour-glass shape, the chief part
its maaa may become di£[\ised into a ring^ is strongly
' Sid, Mfta. vol. iv, p. 39.
* O'Arrwftt, Astr. Nuch. No. 1360. • Phit. Trans, rol. oxxul p. 43) .
* IamwU, Memoirt Ji. Attr, Soc vol. xxUL p. 02 ; Lotd Uo«a0, Phil. 2'ran*.
dI. 0x1. p. &n.
* D'Arre&t, AbkoTtdlti^ngtnt Leipzig, 1857, p. 335.
256 THE SYSTEM OF THE STARS
auggeeted by the au^ilog}' of the bright Sipot« at either end of
the minor axia of the ring-nebula in Lyra, A planetary in
the southern hemisphere (N.G.C 1365) appears, in Etict, tu
have already reached a more advanced stage on the eame roaii.
and Beveral '* miniatures " of thu " Dumb-bell " art* included
among that clas8 (if objects. Oue especially in Cygnu*^
(N.G.C. 6905). depicted by Vog/dH with the Viemis 27-iDch,
eaaily givefi an impression of actual duplicity,^ and showed mI
Pareonstown as a " beautiful little spiral." It has a centni
star and four " satellitea." Its visual spectrum, like that of
the Dumb-bell nebula, ia approximately monochromatic The
leading nebular my at 5007 concentrates nearly the whole of
its light.
A photograph of the Dumb-bell nebula, taken by Dr.
RoberUf with an exposure of three hours, October 3. 1888,
mtiinates pretty clearly the advance towards conapleteuees of
the oval bright border of the disc,^ as well aa its superpoeition
upou a fainter, more elliptical one, visible as a kind of effiuam
at the extremities of its longest diameter. Vogel's drawing*
likewise »u|^6ts, though after a different fashion, the presence
of two ellipses, one partially concealed behind the other ; and
there hence Beems reason to think that this singidtir fonuatioD
partakes in more ways than one of the compound character
evident in many planetary nebuhe. Nor is it pt-rhaps isolated
in space. On I'rofeaaor Sc^haeberle'e plates it appeared as the
bright central part of u right-handed vortex ; coamical relations
Ijeing thus ascribed to it no leas extensive than those claimed,
on eimilar evidence, for the spiral Ring in Lyra.
' PrtbliaitutncH, FoUidflhi, "So. 14, p- 36.
^ K&lioui-diii, Cvmptet Jitndw, t- imwi. p. ^SO, oommentod ou the aiulog;
belweaQ Ibc Dumb'beU apd the Lyre bebulK reodared muitfeat by the Moadoa
j'hotoifriiphH.
' Publieatianm, No. 11, p. 8S.
CHAPTER XX
THE GR£AT NEBDL£
elliptical and irregular classes of nebulae are illustrated
euch splendid examples, that an entire volume rather than
' fiiugle chapter might well be devoted to their consideration.
One member especially of each towers above the rest, like
Ajax among the Argive host, and the two are so different
that it is not eaay to award the palm of superiority to either.
Needless to say that we allude to the objects in Andromeda
and Orion, the types respectively of the elliptical and irregular
plans of nebular tonatruction.
The former (M 31) ifi the only genuine nebula which
could easily be detected, without previous knowledge of its
existence, with the unaided eye, and it ia the only one, acicord-
ingly, which was discovered in pre- telescopic times. AX Sflfi
was familiar with the " little cloud " near the most northern
of the three stars in the girdle of Andromeda ; ^ and its place
wae marked on a star- map brought £rom Holland to Paris
ty De Thou, and believed to date from the tenth century,*
Simon Mariua, who was the first to turn a telescope upon it,
December 15, IG 12, called it "stellam quandam admirandte
figurte," and compared its dull and pallid mys to those of a
candle shining by night through a semi-transparent piece of
horn. Yet this strange phenomenon was only rescued from
neglect by Boulliaud, whoae attention was directed to it by
the passage of the comet of 1664 across that part of the eky.
So surprising did the disregard of it by Hipparchus, Tycho,
^ Scl^jellBrap, Ikterij^ion de» ^oitgs, p. 120.
* Lfl Oantil, M^nvirti tU VAcad, 1769, p. 469.
367
t1
258
THE SYSTEM OF THE STASS
ftDd Bayer then appear to hita that hd coDclitded it to nry
in light, a hypotbeau which derives no support from reoetii
obserTAtioiifl,
With powerful light-conceDtratiou this " most magniiceDi
object'* {ia Sir John Herachel'a phrase) asaamee Twt pi»-
portiona They were extexided by G. F. Bond, nsiDg thi
15-ixicb refractor of Harvard College, to cover an area d
4" X 3(^ and be probably did not reach their absolute limits.
Two adjacent nebule^ one (M 52) described by Le GeDtil to
1749, the other (N.G.C
205) by Caroline Hencbd
in 1783, "undoubtedly fifl
within their oompasB.' '
The light of this nebolt
ifl " of the most perfectly
milky, absolutely irreaolf-
able kind" * It does nat
collect into " floccules>" and
producer none of the sdntil-
latiDg effect giving to maor
guaeoua nebulsB a dt^usive
appearance of reeolvabilit^.
From the circumference
towards the centre, hov-
ever, it gradually brightens^ then abruptly condenses to »
small nucleus, of indistinct outline under high magnifyifig
powers, and possibly (like the nuclei of many comets) granu-
lated, but asauredly not stellar.
Thia progressive brightening inward ahows, nevertheles,
interruptiouB. On September 14. 1847, Bond discerned two
long dark rifta running nearly parallel to one another, and to
the axis of the nebula.' Their detection was a consequence of
the widened area of luminosity perceptible with hia inatrumentr
the inner rift having been taken, until then, for its boundary in
that direction. The outlines of Bond's drawing are given in
the accompanying diagram by Mr. Wasley (Fig. 32), in which
the " rifta " are marked A and £. G represents Le Gentil's
* Bond, UcTruiira Amsr. Acad. vol. iii. p. 83.
' J. HenKhel, Mtmoirs £u A tit. Soc. vaL il. p. 4M,
' Mtuwirs AmtTv Aead, vol. iii p. 80,
L
THE GREAT NEBULA
259
\
¥?■
..D Miss Herechel's attendant nebula, E an exoeptionally lucent
^ region crowded {it has Binoe been found) with hoata of minute
Altera.'
^B Tbeae enigmatical appearances at last assumed an intelli-
gible form ill a photograph
taken by Dr. EobertSj October
1» 1888.* The view given by
this magnificent picture of
the Andromeda nebula aa a
BymmetncaJ, though still
inchoate Btnicture^ ploughed
up by tremendouBj yet not
undisciplined forces, working
harmoniously towards the
fulfilment of some majestic
design of the Master Builder
of the universe, is of a
stature to modify profoundly
CUT notions as to how such
designs obtain their definitive
embodiment. An impression
obtained three months later
with four houre' exposure
was carefully studied by Mr.
Wesley ; and hia tracing of the lin^ of conformation brought
out on the sensitive plate is copied in Fig. 33,
Bond's " canals " are now seen prolonged and curved into
two vast rings (AA and BB), which prove, on attentive con-
sideration, to be dusky intervala separating the succeseive
epirea of a single great stream of nebulous matter, winding
outward from near the primary to reach the secondary nucleus
(M 32). The similarity of the relations between the two
nuclei here, and in the " whirlpool " nebula in Canea Venatvci,
can scarcely escape notice. Thousands of stars are scattered
over and around the Andromeda nebula; the situation of
which in a prolongation of the Milky Way perhaps sufficiently
explains their profusion. A beautiful photograph of it taken by
Dr. Max WoK, August 18, 1901, with the 16-inch Bruce lens,
Flo. 33. — Splnl Stmcian of thfl Qre^t Andro-
meda NebuU {Knotelw^, yoL slU p. 16),
^ lUnyard,
wUdgty vol. xii, p. 7fl.
to], xlix. pp. €C, 130*
2d0 THE SYSTEM OF THE STABS
is ahovm in PUte XIII., Fig. 1 ; and serenU striJoAg pkiur*^
of tlie same taAfveUouiS object have been obtained br lb
Ritchey with a two-foot redector of bis own oonsUtacUoii
Near the ceotre on the oti^noiU aegHtir^, he tolla vb} " sh&H'k
detmed narrow rifts and d&rk holes " ard ditftinguiduble, tft
truces of which evade direct telooccypic observrntioa. Thai
peculiar eSeota of chiaroBcuro are probablj indicatiTe tri
tumultuary local movements, but attempts to ttxplaia tbem m
detail must loug reuiain futile.
Opinioias are divided as to the cooBtitution of the Andxt)-
meda nebula. Sir Norman Lockyer inferred it to be meteomc.
comparing its state to that of " a comet vrithin a tnoDth ol
perihelion." ^ Dr. Scheiner, on the other hand, r^ards it
as virtually a cluster of sun-like stara* A ^)ec£rographic
impression, wrung from it by meaoa of an exposoz^ of
Y^ hours with a short-focus reflector in January 1899, flaemed
to him a faint replica of the solar apectrum, marlnd br
the familiar dusky ruliuga, but by no bright lineei Y«t
Sir William and Lady Huggine hnve more tb&n ODce,
observing the same spectrum visually, caught tmequivocil
traces of the admixture in it of emissive with absocptire
elements.*
The real shape of the formation must be that of a disc.
oval or inund^ but with a spheroidal mass both at the origin
and extremity of the nebulous spires. Their convolutions, if
actually circular, must lie in a plane inclined about 25* to the
line of sight ;^ but we can only estimate their extent in space
by making a precarious assumption as to their remotenesR
Taking the distance of the nebula, for instance, to be of
sixty-five light years, that already attributed, for illustrative
purposes, to the cluster in Hercules, we find its radius to
measure 162,000 times the radius of the earth's orbit; so that
the frontier of this glimmering realm, as determined by Bond,
is much more than half as remote from its centre as the
nearest fixed star (a Centauri) is from ourselves I In travelling
from end to end of it, light spends nearly six years ; and if it
» Attroph. Jmtmatf foL iit. [i, 228,
* Obaervaiory, vol. lii. p. fla. ' Aatr. Naeh, No. 3M9.
* AUas o/StettaT SptdTa, p. 135.
° Scheiner, Photographu d€r Ghaivnw, p. S32.
THE GKEAT NEBUUE
261
obliquely towards uSj then onr view of the further margin
ly be of an earlier date than our view of the hither margin
a coaple of years or more. Extensive changes within the
ehula might then manifest themselves to us successively,
Ithough they had really occurred simultaneously ; while, con-
ely, the coincidence in time of widespread variations would
^ue a position of the nebula nearly square to the line of
sight. That it is Btill in the pla&tic 8t&ge there can be little
doubt; and the outbreak of the "new star*' of 1885 haa
shown that the action of the powers engaged in ruoulding it to
ite predestined shape may occasionally be attended by a cata-
strophic liberation of energy.
Two adjacent nebulae in Leo, both enrolled by Messier,
have finally quitted the ambiguous position long occupied by
them. They are elliptical spirals, analogues of the colossal
structure in Andromeda. Photographed by von Gothard in
1888, the one (M 65) showed a bright centre with four
appendages resembling the sails of a windmill ; the other
(M 66), a complex arrangement of envelopes partially sur-
rounding a nucleus, somewhat like the paraboloidal veils flung
round the head of a comet near perihelioiu These, howeverj
were incomplete views. On Dr. Koberts'a plates/ Loth objects
took shape as ovoid formations composed of closely winding
luminous coils, "thick inlaid," in the case of M 66, the chief
of the pair, with nebulotis condensations.
Sir John Herschel frequently noticed an approach to
&nnularity in the members of this class of nebulce, and added
the remarkable comment that " as the condensation increases
towards the middle the eUiptieity of the strata diminiahea" '
This, if verified, would imply their ovalness to be not a purely
visual effect ; and the inference that the appearance of elonga-
tion corresponds to its reality is supported by such critical
circumstances as the situation of a pair of stars either at the
fod of a nebulous ellipse (N,G.C, 6595), or at the extremities
of its major axis (N.G.C 6648),
The longitudinal clefts often visible in ray-shaped nebulas
corroborate this opinion. For otherwise, why should they rim
lengthwise rather than in any other direction ? If the bodies
' Cdeatial Phoio^aphSt vol. ii, p. 76.
* Cape Obtervalwnt, p, 22,
262 THE SYSTEM OF THE STABS
t\mj cbarocieriae were, in &ct, cticakr diaca, none o^ tbii?
pbjsical featoroB ooold hAve anj relation to the appeiaacE
they happen to a»ume bj projection. Such « nktaoa m
eixtremely conapicuoua in an elliptical nebaU, ia tlks
Centaur (K.G.C. 5123), divided along ite entiro lengUt br
" a perfectly de&nit^ atruigfat cat, 40" broad.** A dafioBe
nebulous streak runs between, and parallel to the habia.
which are shaipl/ bounded on the aides facing each other, bot
hazj on thoee averted. " The internal edges of thin tst
problematic objeet," Sir John Herschel remarked, ** hftw -
gleaming light like the moonlight touching (hd ootliBe la &
tinutspaiencj." ^ It is by no meaoa a solitary exampla A
long, narrow nebula in Leo (N.G.C. 3623) ia " split faalo two
parallel iaj&" * A black chasm, into which the nucleiB pto-
trades, eepatates a lucid from a faint atreak in Coma BerenieH*
(N.G.C. 4565); and a nebula in Andromeda (N.G.CL 891).
with " a chink in the middle and two stars," sappoeed bj Sir
John Herachel to be " a thin, flat ring, of enormous dimeiUMU;
seen very obliquely," and photographed under that aspect
by Dr. Boberta in 1891/ may really belong, as waa indicated
by the Farsonstown observations^ to the numerous cabegoi^
of cloven rayt. That their distinctive peculiarity dopenda
upon some general conatnictive principle cannot readily be
doubted, but we ehould vainly attempt to apecuIuLe upon ita
nature.
No descriptive formula is wide enough to include all the
capricious forms of "irr^ular" nebulae. In regarding tboe
singular structures, we seem to see surges and epray-flakea of
a nebuloujs ocean bewitched into sudden immobility ; or a rack
of tempest-driven clouds banging in the &ky, momentarily
awaiting the transforming violence of a fresh onset. Some-
times, continents of pale light are separated by narrow straits
of comparative darkness ; elsewhere, obscure spaces are hemmed
in by luminous inlets and channels. The "great looped
nebula" (30 Doradds)^ one of the inmates of the greater
Magellanic Cloud, resembles a atrip of cellular tissue. It
serves not to conceal, but to ornament in a wide, openwork
' Cape OfiiKraoiion*, pp. 20, 105.
Trant, R. DuK Soe, vol. ii. p. 9C. * Ihid, p. 118^
'* Celestial PhotoffrapA^ voL I p. 41.
1
1 -■
p
THE GREAT KEBUL^
263
ftttem the ekj behind it, and was described by Sir John
Herschel as ^' an aBsemblage of loops," the " complicated
windings" of which constitute it "one of the moet extra-
ordinary objeeta which the heavens present.'* ^ It gives,
nevertheless^ a dense photographic image, Plate XV. reproduces
an admirable picture obtained in two hours at the Royal
Observatory, Cape of Good Hope, in which claws and tentacles
of faintly lucent stuff are seen to be thrown abroad in all
directions from the main trunk, itself extensively riddled with
dark spaces.* From the Arequipa plates Professor Pickering
judged this object to be the core of a spiral," probably embracing
the whole contents of the Nubecula Major, and even to the eye
it appears as in some sort their kernel. The " looped nebula "
may then very well be the hub of ita own particular universe.
Its spectrum is gaaeoui*, but with an unusually strong inter-
mixture of continuous light.
The efficiency of the camera in disclosing the intricacies
of nebular structure is vividly exemplified in Plate XIV., which
exhibits, eelf-portiayed, one of the many celestial marvels
gathered together in the constellation Cygniis, The object
(N.G.C. 6992), though very imperfectly characterised to
visual observation, is marked in our picture (the original of
which was taken by Mr. W. E. WilBon of Daramona, October
7, 1899) by a surprising wealth of detaiL Its texture is
perceived to be throughout delicately filamentous/ the fila-
ments being, as it were, drawn out in the same general
direction ; and the bright patches composing the nebula
have besides, as Mr. Wilson noted, a parallel trend which
coincides with that of the separate nebulous threads, A con-
cordant play of forces is thus evidently brought to bear upon
the entire formation, which, measuring from end to end 80'
of arc,* must be of a vastness transcending imagination.
There is, beeides, some reason to believe it organically related
to an undulated nebular mass in its immediate neighbourhood
(N.G.C. 6990).*
1 Capg Oburvationtf p. 12.
' Oore, World* of Space, p* 208,
* ffaroard Amvsh, vol nri, p. 208,
' Sw fetao Ritcheyi Astroph^ Joum. tuI. zir, p, 22B.
" Roberta, C*I. Photifffrupha, vol, ii. p, 14&,
* H. C. WilBon, Fop. AmIt. Oct. 1002.
M4
THB SYSTEM OF THE STABS
But all other irreguUr nebubs oiikk into iiwigtufieutt
compared with that ahown by an opaxs-glsaB as ft ffliv«ij
patch round one of the atora in Orion's swonL Thii extzft-
ordioarj object (M 42) has been under eSecdTe obesntm
for 250 jeATi, and during the last cdghty haa baen aao»>
graphed^ mapped, me^ured, figured, and photographed with i
diligence worthy of its pre-eminence. Hence, fulare chai^
In it, ahould they take place, most be slight indeed to
- detection.
The multiple star Orionia might be called the foondAtii
etone of the edifice. All the lines of ite architeotore an
down with reference to it, iind the intimate physical
tioa of the stare with the gaaeous stulf surroundiug them,
been spectrographically demon at rated by Sir William
Lady Huggins^ and amply ratified by Professors Frost
Adams.
Surrounding the trapezium is the brightest part d
nehuUi called, from its ^t delineator, the " Hu;
region," Over this epace, shaped like a right-angled
the light 13 collected into " flocculent ma&aes" which, with
best aoeing, prove to be throughout of a " hairy "
The effect was compared by Sir John Herschel to
" breakiog-up of a mackerel-fiky, when the clouds of whiolLl
oonsista begin to assume a cirrous appearance," * and su,
to Mr, Laseell* " larg« masses of cotton -wool packed
behind another, the edges pulled out so as to be very film^
The " pea-green colour " of the whole object struck
forcibly, but is apparent to moat obserTers as little more
a greeuiah tinge.
Emanations (or what seem such) from the Huygeniau
core stretch away in wide curves to form the outlying porti
of the uebula* One great effluence runs out into a " proboi
attached to the upptT jaw of the nondescript creature liuiu<
in unearthly radiance, on the eky. Another, represeni
ing the lower jaw, bounds on the northern side the
of the distended fauces (the " Sinus M^nus "), and ia sub-
L sensibly connected — as if by a ahoal leading to an island —
I
Memoirs R Aitr, Soc, vol, ii. p. 4&1 ; 0, Stone, fu6(. Ltaiuier ^Corrnkk
Obrarvatori/t vgl, L ^t. 7, p. 274.
^ Ibid. voL xxiii. p. 64.
iVii Irivt^iilui" X^buJii ill I'v^iuih. I'lmto^rujilicil by W. K. W'Jhon, KJl S,
THE GREAT NEBULA
266
ith tha ''nebula minima" (M 43), a roonded mass vhieh
^appears as if just drawing together into a star.'* ^ Behind,
id between the two, misty efiTusions Bpread far afield;
olved by O. P. Bond into an intricate fabric of convoluted
ftnd branching filaments, the brighter region from which they
spring diapkying a similar, but more compact mode of aggre-
gation. "^ It IB now impoaeible/' he wrote after a particularly
fine view of the nebula, on February 26, 1861, "to see it in
any other aspect than as a maze of radiating, spiral-like
wreatlia of nebulosity, or filamentous tentacles, the centre of
the vortex being about the trapezium/' ^ And to Mr. Safford^
using the then recently constructed 18j-inch Clark equatoreal,
it appeared as " an assemblage of curved wispa of luminous
matter, which, branching outward from a common origin in
the bright massea in the vicinity of the trapezium, sweep
towaj^ a southerly direction, on either side of an axis passing
through the apex of the Regio Huygeuiaaa." '
The appLcation of photography to this amazing object
has not only supplied records of its actual condition in-
definitely more authentic than any producible by the human
hand, but has served to combine the peculiaritiea of its con-
formation into a strikitiigly suggestive whole. The outcome
can best be appreciated by reference to Fig. 34, exhibiting an
" index diagram " prepared by Messrs. Eanyard and "Wesley
from several negatives procui'ed by Dr. Roberta with varied
exposures. Two points are made perfectly clear by it. First,
that the whole fabric of the nebula is concave towards an
axis " passing through the trapezium in a north-easterly and
south-westerly direction."* Kext, that the effluences from the
trapezium liave a predominant tendency to assume ramified,
or tree-like forma. Thus the seemingly eruptive jet marked
with the letter b mimics the shape of a stone-pine, and bears
a less equivocal resemblance to the " stemmed " type of solar
prominencee, aa well as to certain arboreal structures visible
in some photographs of the solar corona. The latter analogy
ia rendered still more apparent by comparing the vast nebulous
out-growths, a and A, with the group of coronal rays repre-
^ J. Hdsehe], Metrtoirt B, Attt. See. vol. li. p. 49.'>.
' B^kTvard Annalt, vol. v, p, 168. * Ih%d. p. 159.
* Raujard, Knawttdyt^ vol. lii, p, 147.
THE SYSTEM OK THE STABS
asnted in Fig. 35. The aanie kind of atmctoreB seeBa, ii M
otsee. At ODce to spring npwafd ftad to carre i&wd. as if
nnder the iuduence of a two-fold actioo — oatwaid fen a
centre, and inward towards an axi& Tbia oi^ganic aboilint;
— Gmt detected by Ur. Banyard — btt t wat u i the OrioD aabok
and the lominoua appendages of the sun, is borne oat fef tk»
fesemblance to apon glan of their minute texture.
The limits of the greet " sword-handle ** nebula an obb*
Flo. St. — Index tHagnm to fltmetum photogmpbed la the Ortcm HcbalE
(gwioLHtffe, voL xlL p. 140).
tinually being pushed further back, and there ia no reason to
believe the process nearly terminated. On Mr, Kobert^fl
plates/ firet the " nebula minima " waa joined on to the main
body, then, with lengthened exposures, a cloudy mass to the
north (N.G.C. 19 77) was reduced to its true position of an
offset, by which the forma of the parent-body are pretty
closely counterfeited.'' But even the combined object is far
' MinUMtf ^^otica^ toL xliz, p. 290,
» Ratiywd, tec, c«. p. 1*8.
THE GREAT NEBULAE
26r
om representing the nebulous contents of this part of the sky.
Br an area of 150 square degrees, iri which it IB nearly
antral, twelve new nebulie were photographed at Harvard
ollege in the spring of 1888, and ludicatioog were obtained
it Sir William Herschel's surmise ' of the union into
le immense stratum many degrees in length of the " great "
gbula with othera lying north and south of it, might
be veriSed in the immediate future.^ It was soon after-
wards more than verified. On January 14, 1890, Profeeeor
W. H. Pickering exposed a plate during 6^ 22"" at the
■k
k
Fro. S5.— Qnrap of OqphuJ: &tniet(iT» (W. 11. WHler^ XiwvMgt, vtfL ili p. HT\
aummit of Mount Wilson, California, with a 2l-inch portrait-
lens. A singular diaclosure resulted,' A great " snake " of
diffuse nebulosity (aa Professor Wolf has since called it),
issuing from the trapezium, was perceived to enclose the whole
central part of the constellation with dim folds 15 degrees in
diameter. Cosmical vortines on this gigantesque scale are
beginning to appear leea rare phenomena than the strangeness of
their aspect and implications might have led us to anticipate.
They are discoverable only by means of short-focus photo-
graphy.
In the Orion nebula we perhaps see an undeveloped
1 Phil. Tratu, vol. Ixxii. p. 2111.
' Harvard Annais, Toi. inii. p. 117. ' Und, voL rxnL p. 36.
268
THE SYSTEM OF THE STAHS
diiBter on tb» model of tbe rieiade&. Nearly & tbooduul ttan
were catalogued b^ Bond Id the portion of it (3*36 aqiine
d^rees in area) examined by Liio. and las list provw to be &j
from exhaiutiva.^ Many of them ahoulJ, uideed, in Pcotoor
Hotdeik'a opinion,' be accounted rather aa nebular oondeoi^
tiona than as true stars ; but that they will eventoaily gra*
to he auch^ aa they slowly absorb the nebulona niaterial now
enahrouding them, is a justifiable coojectureL Tbe aame pn>-
oesa appears already far advanced in the PIeiades» with the
reault that the stellar now altogether predominate orer the
nebuhir element in the compound Bystem. It may not hai^
been always so. The balance inclined perhaps^ in tbe remote
past, as decisively the other way aa it now does in the Orion
nebula. Tbe variability of nearly a hundred of its in^njlved
stars ia an additional fealiii^ of resemblance to compieased
duatera. Noted in a few cases by Dr. fioberte in 1890/ it
was rendered astonishingly prominent in 1904, by Mis
Leavitt'a comparieona of records stored in the Harvard photo-
graphic archivea.^ The discovery gains added aigmficaaoe
from the fact that many, or moat of tbe twinkling crowd
thus brought into evidence belong to the cluster- 1}*^ of
variables.*
It iB not easy, Sir John Herschel tdla na, '^ for laognage
to convey a full impreasion of the beauty and sublimity of
the spectacle offered by the Argo nebula^ when viewed in a
sweep, ushered in as it is by so glorious and innumerahle a
procession of stars, to which it forms a sort of climax.'**
"Situated in one of thoee rich and brilliant ma&sea, a sue-
oeaaion of which, curiously contrasted with dark adjaoant
ipacea, constitute the Milky Way between Centaur and Argo'
its branches with their included racuitiea cover more than a
square degree, and are strewn by above twelve hundred stars
These, unlike the components of the trapeEimn-cluBter, show
no general tendency to vary in light The peculiarity from
which the Argo formation derives its current title of the
* Pftrkhurst Astrop\. Joum. toL ir. p, 130.
* fFiuhinyltni Observatioiu, 1S7S, App. 1, p, 2S1,
3 MiffUhly ^'^atuxs, yd]. 1. p. 818.
* Attr. Koch. No- 3fl50 ; Bartard Oirculara^ Nob. 78» 7», B«.
' J. S. HAgen, Jstroph, Jtmrn. vol. x\x. p. 3H4.
* Cape ObKfvaiiontt p. 88,
^iy^^-^ijj-
'_•■*"
I
Phntogrnjih of tlie Key-Hole Nebula.
Tiiki.>u Willi tlie Knicb 'Jl4-iuch Effractor at Antqttipft.
THE GREAT NEBTILiE
tej-hole " nebula, ia a large lemniscate-ehaped opening in
central and brightest part, the blackneau of which ia
Etlified only by the veiling of one corner by a strip of thin
Bbulous haze, Fonr stars are placed precisely at the edgea,
none perceptible to the eye within the vacuity; and the
famous variable rj Carinae. lies close to its eaatern border. Such
was the brilliancy of the etar In 18S8 that it ahnoBt obliterated
the " key-hole/' now, and previously to the outburst, the
individualising feature of what would otherwise seem a chaotic
sea of luminous biUowa. Duplication emphasises the meaniDg
with which it i& fraught. A second oval aperttue, completely
dark, hut for the faint sparkle of four minute stars, occurs in the
eouthera^ sparser part of the nebula. It might be compared
to the echo of a catch-phrase. Plate XVII. reproduces a photo-
graph of this nebula, taken by Professor Bailey at Arequipa,
June 1, 1896, with an exposure of four hours. The light
and shade being reversed, the most intensely actinic parta of
the portrayed objeet are printed black, while its vacuities are
left white. Thus, the "key-hole" appears as a crooked,
flhadowless aperture in the moat strongly himiuous section of
the inchoate structure, which is rendered in a manner bifid
by a vast dusky channel running from south-eaat to north-
west between two nebulous continents. The second " key-
bole/' which ia larger than the first, and has some similarity
to a kidney-bean, lies far to the south, in an outlying effusion.
A very peciJiiir gaseous nebula in Sobieski's Shield (M 17)
has revealed itself piecemeal. Messier, first of all, noticed, in
1764, a apindle-shaped, starlesa ray, about 6' in lengths Sir
William Herschel added an arch springing from its western
extremity, and the combined object became known as the
" Horseshoe" or " Omega" nebula, its form reaembhug that of
the Greek capital letter n, with the left-hand base-line turned
up obliquely,^ Again, it suggested a " Swan " to observers
whose instruments were inadequate to show the complete
arch, and Flammarion compared it to a smoke-drift, fantastic-
ally wreathed by the wind. In the cleai' aii* of the Cape, Sir
John Herschel detected a second very faint " horse-shoe/*
attached to the opposite end of Messier's streak from the first,*
1 J. Hom-hel, Phil. Tranf. vol. cJCiiiL p. Ml,
'* Cape ObMrvaiiftiti, p. 10.
Omega nebula^ obtained by Br. Roberta Id 1893. eahiUi
Meesier's my ha the axis of &n oval maas covering an ajM IS*
hy 12';* but the intimate secrBt of its orgaaiaatioa bn Mffl
to be penetrated It ia iudeed situated too Car to the nott
to be usefully inveetigated in these latitudes.
The " America " nebula is apparent oiilj to th« obttBial
retina. Some inditiAlioufl of ita existetice were caofht bj iIm
cider Her^bel ; but its virtual diaoovery wae mAde pbsle*
grapliically by Dr. Max Wolt On a plate exposed DmmIm
12, 1890, the vast object portrayed in Plat« XYITL etoagdiot
the Sret time into full view, and received ^ name deecriliEI9
of its striking resemblance in &hape to the contitient of Kott
America. Among the features attracting attetition oo ov
plate are a amall, intently black hole piercing the neck of
light that corresponds to the Isthmus of Panama, and
nebulous atar, like an island in the Atlantic Ooean off
coast of Kew Jersey. This is 57 Cygni, lately found to I
spectroacopic binary in ewift circulation round an ot
companion.' It yields a helium spectrum in con^spondeiM*
with its nebulous relation ships.
Ko logical distinction can be established between irreffo
nebuhe and those indefinite tracts of milky radiance
by the elder Herschel " diCfufled nebulosities." The total
of fifty-two separate tracts perceived to be thua phosphorescent
was estimated by him at 152 square degrees, and he added
the judicious remark that *' the abundance of nebulous matter
diBuasd through such an expansion of the heavens most
exceed all imagination."* The few visual observations subse-
quently made of these regions* intimate irregularities in their
illumination doubtless dependent upon the slow advance of
cosmic processes of large scope. Their investigation, bow-
ever, ia properly the task of the camera. Already, some of
Herschera " affected " regions have been proved, by the photo-
' Sidgrtat JfeJKujj*?, t*l. iv. p. 38. ■ C*i. Photagrapkt, voi i p. lOL
' Frost and AddiCDJ, Astrcph. Joum. toL xrii. p. 381.
* Phil Tritns, vol cL p, 277-
• Dreya^^ K J. S. Aatr. Oea. Jahrg. iiii p. 63 ; Littrowj SUrngntppm vmd
^ehelmaam, p. 29 ; T«inp«l. Attr, ^a^. No. 2C11.
THE GBEAT NEBULA 271
iphs of Barnard/ Boberts/ and Wolf,* to indade strongly
p-eloped nebulous formations ; the condition of the rest has
LL to be ascertained. Prolonged exposures with appropriate
truments will be needed to determine it satisfJEkctOTilj.
' JMroph. Joum. vol. xvii. p. 77.
• Monthly Natic$$, toL ixiiL pu 28. * Srid, ju 80S.
BpKCULAnotrs aa to an identity of uuture between nebnbl
u&id oometd are no novelty ; they pr^entod themsdvM, u
they could hardly fail to do, to the mind of Sir William
Herschel,^ and Sir Norman Lockyer sought to prorida Uieta
with an experimeDtal b&sb bj his researchce oa meteqrites in
1888-89.'' The results were scarcely encouraging. Indeed, UiC
two classes of bodies have epectroecopically little in commoc
Ko gaseous nebula gives a trace of the carbou-bandfi chancte^
ietic of comets; while the bright lines derived trom nebalft
are absent from moat comets certainly, from all probably.
Yet a physical analogy snbsiats, and is evidently charged with
meaning.
Both comets and nebulae consist of enormous volumes of
gaeeoufl material, controlled by nuclear condensationSt whether
of the same or of a different nature in the two genera we need
not now stop to inquira. Both, tht^re is the strongest reason
to believe, shine through the effects of electrical excitement
In both, thei-e ate manifest signs of the working of repulsive,
as well aa of attractive agencies.
A telescopic comet is indistinguishable except by it9
motion from the ordinary, centrally condensad, rotind nebola.
which is itself indistinguishable from an exceedingly remote
globular cluster. Superficial likenesses do not, it is true,
count for much ; one object may counterfeit another without
bearing any true relationship to it. What it ta really im-
portant to note is the structural resemblance of nebahe to
comets. The ports of a comet become differentiated exclusively
> I^il, Trwtf. roL oi. p. 306. * Tht MUmnilic B^pathaiM, p. 2S8.
373
J
PHE NATUBE AND GRANGES OF NEBULAE 273
Icander solar InSuence. Hence their symmetrieal arrangement.
^ms regards au axis paesing through the sun, is modified only
tbj the orbital displacement of the body to which thej belong,
l^nd from which they emanate. It is extremely curious to
tifind that, notwithstanding the absence of these conditions, the
features of certain nehulfe are impressed with a correaponJiDg,
"though different kind of polarity. Definitely directed outflows
(or what aeem to he such) are in them of frequent occurrence.
Prom many of these objects, aa from many comets, only a
' single stream of effueion is manifest ; and we then get " stars
' with tails," which might well pass for miniatures of the
' bearded travellers through oui^ constellations. Those effusions
ftre, in some cases, boxmded by straight lines ; they are fan-
' shaped ; in others, they are curved, often so strongly that the
! " brush " is bent into a " coil" Such difierencea may be
plausibly associated with the varied conditions of aiial
rotation in the star-like nucleus. Wbere there is none, the
isauing matter naturally proceeds straight outward ; its
corvature depends upon its being left continually further
I behind in the widening cirelea reached by it as it ascends
I from an advancing point of efflux.
It is easy to see that this process, if carried far enough,
will result in the production of a helicoidal nebula. Fully
developed spirals are, however, constructed oa a less simple
principle. Their convolutions are duplex. Two opposing
branches combine to form them. That these branches
represent intakes of matter from space is hardly a tenable
opinion. It has, in fact, been virtually abandoned owing to
its inconsistency alike with the design and the details of the
objects under consideration. The conviction is now dominant
that they originated through some kind of repulsive action.
Professor T. C Chamberlin regards them aa products of
catastrophic disruption. Each is the wreck of a sun-like body,
dispersed through the tidal influence of some similar orb to
which it made a fatally close approach,^ They illustrate,
accordingly, " the effects of explosive projection combined with
conourreut rotation." M. Deslandrea adverts to the corre-
spondence between the diametral wings of the solar corona
id the opposed arms of a spiral nebula, the ramifications of
1 Aitroph. Joum, voL xir. p. 31.
274
THE SYSTEM OF THE STABS
which he hold^ to 1^ explicable on Br6dikhine*B ihtotj
multiple comet&ry tails ; ^ wliile Mr. W. £. WUson w«ft stmdc
vrith the " coinetary taila, curved like plumfcs away fram iKe
central nuck'UB,'' attiichcd to the nodoaitiee beeCrewiog tq
photograph of the Whirlpool in the Honting Boga'
With very rare exceptions, xiel-iuli' are seen by na, nAt '
pUn, but in fxirapeetive. '' The only thing," Profeaeor
wrote in 1889,^ "we really know about the form of a
in general. Is that it is projected into a cert-Ain hIi
problem is to €nd the true curves in space, knonin^
projected curves." His efforts to solve this arduous problem I
actual trinls with helices of wire projected in all ima
varieties of poaition, mtt with a certain mc-asure of buc
The " type-cun'e " at which he fiually arrived, though
perhap** really conformed to in nature, served, at any
usefully to define ideaa regarding " the actual aituation of
different branehea of a nebula in space of three dimensiooSi.^
Kebulfe of the spiral and " brush " kinds, are not the
ones exhibiting cometary relation ships. A charact
feature of nebulous trains and " wings," exempli Bed liotb'
the Orion and Pleiades formations, is their va^e diffluioai
one aide, but sharp terminatii>n on the olher^ just as in
luminous vanes appended to the heads of cometa. The
tinned ejection of matter agaiiist a counter-current of force'
which it iH unceasingly driven backward, seems iudicatedj
both cas«s.
Planetary nebulae, too, imitate, in a fashion of their
the heads of comets under energe tic solar action. Their
nxultipla discs correspond most strikingly to th« multiple
envelopes of comets, and intimate a similar origin through
interior espansive or repulsive agencies. Only that in the
absence of the dh-ective power of the sun, tlie waves of «id*-
nation ^lead equally in uU directions, producing suoceflsive
approximately globular, instead of parabolic surfaoea. Und
tlie combined iuOuences of rotation and contractiou,
shells might be expected eventually to subside into rinc
* CompUf Jifiviffi*, Juno 23, 1902.
* Aftr. ReArarcKtuit lktr<imr»nn.,
• PublUtUiana Attr. Soc. of the Pa
* Roch«, itimniint tU t'Acad. dt4 StUtiut, W
' p. 2«.
(THE NATURE AOT5 CHANGES OF NEBULA 275
but it would be rash to affirm that annular nebulaj, in poiut
of fact, acquired in this way their present aspect
No visible sigus of movement have, up to this, been
ived from nebulae. In the ordinary sense they appear
absolutely etationary. Accurate observationH of them are,
indeed, comparatively recent; they go backj nevertheless, for
enough to juHtil'y the statement that not one among about
four hundred well-determined nebulae becomes progreaaively
displaced by so much aa one second of are yearly. The
nebula in the Pleiades ought perhaps to rank as exceptions to
thia general immobility, since we need no direct proof to
aesure us that they drift with the cluster of which they form
an integral part- The drift, to be sure, is slow ; but it is
aecnrely ascertained, and atforda grounds for the ijole estimate,
that is not mere guess-work, of the distance of a nebulous
syatem.^ The apparent indiffewnce of all other uebulie to
the perspective effects of the eun'a swift advance through
Space leaves little probability that any of tbem lie as near
to us as the nearer stars ; and the probability is raised aknost
to certainty by the apectroscopie discovery that many of thaiXL
ar« animated by rapid individual movements.
Thirteen planetary nebulffi measured by Profeasot Keeler
in 1890,* proved to have an average radial velocity of 17
miles a second. The swiftest among them is the helical
structure in Draco, which ahowa an advancing speed of
40 mile^ a second ; the " Saturn " planetiiry in Aquarius
oXbo approaches the aun, though somewhat more slowly ; while
a stellar nebula in Aquila (N.G.C. 6790) increases its distance
by 30 miles a second, or by ten times the earth's orbital
ladiufi in each year. As regards motion, then, no distinction
can be drawn between stars and this kind of nebulae. Tlie
■ irregular class has bL'cn investigated for spectral displacements
only in its leading representative ; and the concordant results
of several inquirers prove the Orion formation to be in course
of withdrawal from the earth at the rate of about 11 miles a
second.* But, since thia velocity must be largely, if not
wholly, an effect of the sun's translation through space, the
^ Se« ante, p. 106.
* Liek PnUifaHim9, vol iii, pp, 217, 228.
* Froit Aud Adama, Aitroph, Journ. vol. sii, p. 354,
S74I
THE SYSTEM OF THE STABS
Xflbaift mftjr in bet be «lroaet st rest in the sldlar
Indkabom of poanble marvow&tB wifchia it i
Dr. Vogel in 1902 Irom spectrogisiDB of its
1 ikntsd bf
HMft ptftS,'
and the doe will periiapa eretitqAll/ be followed op to ft definite
mne. But no ciebiila has jet been pfoved, by line of s^X
memmaim, to loUte oa an axis. Nor are double nebdc
pooeptibtj circnlAting. Tho ajsUmn tbey ptesiunably ood-
stKtnte rem&in ngidl/ fixed. The oontz&rf baa often been
MBerted ; jet revelations, alleged on the sfaength of inoxsci
obeervakiona, and brought to a rtaindiitili bj precise ooee,
nuut plaintj be diamiesed ae tUoaoiy ; " unlees," aa Dr. Ih^-^
wsjM,' " we are to believe tbat nebulas in the good old d^r^
moved about an tbey liked^ but bare boon on their good
behaviour dnoe 1861 and kept <)aiet'' The existence,
frequently obaerTed, of a oebulous connection between gnmped
objectiL intimates a atat« of things h&rdlj oompatihie iHlb
mntnal drcnUttou, The relations of theee imper&otlj
separated individuab ^re perhaps in ft state of tr&osition, likl
those of multiple comi^tarj masses, at times enclosed togetbs
like double nebulse^ in a dimlj Uimlnous aheath.
The idea of the accompauioient of pUnetarj nebuUe bj
satellites, was snggested to Sir John Herschel bj the Crequeut
and clc^e proximity to such objects of minute stars/ and be
recommended their careful micrometrical measurement as a
criterion of poeeible future changes But d' Arrest found thA
attendant stars just in the positions Herschel had assigned to
them/ and only one case of suspected displacement has sinee
attracted serious attention. Professor Barnard noticed a minute
discrepancy between his measures in IS 99 of a twelflti-
magnitude star closely following the ring nebula in Lyra
and those made by Burnham eight years previously.* He
inclined, nevertheless, to attribute the alteration (if real) to a
shifting of the point of reference rather than to movement in
the star* Now the point of reference having been the nebular
Qucleus, the verifioation of his surmifie would involve the
detection of proper motion in a class of objects heretofore
1 Sitiatit'jaberKhU, Beirlui. Marcb 13, 1903.
" Jfmifilif Kvtieet, vol. ilvii. p. 418. ' PAiL Tnmt. roL cxuU. p. BOO.
* Leif&ig Abhandiungtn, IM. iii. p, 30S.
" Mimthly Noiictt, vol. li. p. a<& ; cf. Lcrnvflmrorth, ibid, vol, bci. p. :25.
THE NATUEE AKD CHAISTGES OF NEBULA 277
imperturbftbly fixed. The lapse of a very few years will
render practicable the decision of this interesting question.
Variability in light is a quality of nebulie && sui'ely as of
etarSj although the cases are rare in which it can be eetablislied
with certainty. Nebulae are peculiarly seneitive to atmo-
spheric influences. Their finer detailsj always hovering on the
verge of viaibility^ are completely shrouded by the lightest
mist. Hence, even to the same eye, and with the same instru-
ment, the aspect of the same nebula often varies greatly from
night to night, and since personality is nowhere stronger than
in the perception of the delicate luminous gradations delineat-
ing to our aighfc the forms of nebulfe, a difference of observers
adds a further incalculable element of uncertaJBty. Rumours
of change then easily arise, hut are with difficulty sub-
stantiated.
Theystart.neverthelesSjfrom a presumption not unwarranted
by facts. The occLurence of luminous fluctuations in nebulae
has been proved by the complete extinction of one^ and the
fading to evanescence of a second in the same vicinity. On
October 11, 1852, Mr. Hind discovered, near the group of the
Hyades in Taurus, a small round nebula (N.G.C. 1555) with
slight central con den so lion. It was then very faint, but
brightened steadily until 1856, when d'Arrest ranked it as
belonging to the first, although verging towards the second
class of brilliancy.* His amazement then was extreme to
find on October Z, 1861, iU place apparently vacant! Some
glimmer of its light was indeed made out for a year or two
longer with the Pulkowa 15-inch refractor; but that too
waned, and the object remained invisible for above a
quarter of a century. Then, in 1890, it was just barely
descried by Professor Barnard with the SS-inch Lick telescope;
and even that Buperb instrument failed to show it in September
1895. In 1897 it was not to be eeeu on any terms; in 1898»
it barely stained the field of the 40-inch Yerkes refractor ;
but Professor Keeler managed in 1899 to secure impressions
of its somewhat complex fonn on long - exposed Crosaley
plates.^ The apparition^ so far as can be judged, was a
strictly temporary one* Hind's notice probably did not
^ Attr. NfKh. Noa. \m^, T689 ; Auwera, ihid. No. 1393.
' ProhitTTis in ABirophyticSi p. 52^ (Gierke),
f8 THE SYSTEM OF THE STABS
lag far behind its first perceptibility with modente insbKH
mentB,
A curious feature of the occunenoe was the sjmpathetk,
or at any rate simultaDeoos, decay in light of a bhiaII star-
since known as " T Tauri "' — placed almost in contact with tk
nebula. The atar, however, recovered in 1868 about the same
time that a second new nebnla (N.G.C. 1654) came into riev.
First discerned by O. Strave, it was observed by d'Arrest. wbo
was fully convinced of its novelty, and bis opinion was borne
out by its subsequent total disappearance,^
The ligbtr^jhanges of nebuhe do not offer the same diversity
as those of stars. Only two kinds of variability — those
producing respectively ephemeral appearances and capricious
brightening^ and fadings — axe represented among them. No
periodical nebulae have yet been shown to exist. Tlie influenceSv
of whatever nature^ bringing about the rhythmical pulsations
of stellar light» would seem to be absent from the nebular
kingdom. A distinotioD, however, peculiar to themselves, can
be established among Tariable nebulae. Their fluctuations
m^j be either general or partiaL They may aGTect the whole
of a moderately compact object, or certain sections of aa
extensive formation. Examples of both kinds^ and of all
degrees of authenticity, abound; but we will only mention a
very few, in which the reality of change seems scaroely
disputable.
One such is afforded by en elliptical nebula in Leo (N.G.Cl
3666), "very bright" when discovered by the elder Herscbd
ia 1734, but noted by hie son as abnormally faint for the
first class. Subsequently observed altemationa have made it
all but certain that the discrepancy indicated genuine change.'
A nebida in Cetus, too {N,G.C. 955), is evidently subject to
similar vicissitudea SchdnfeM in 1&61, and Vogel in 1865,
failed to see it, although it was, at sundry other epochs, easily
visible to the former observer, aa well as to d' Arrest and
Winnecke, and fully justified in 1887, I>r. Dreyer considered,
Herschel's ascription of it to the second order of brightness.'
' Dreyer, Mimairt Jt. A»ir, Soi. voL xlii. p. 211,
* Winnecke, Aatr. Hath. No. 2283 ; Dreyer, XemnTt M. AHf. Sae. roL klix.
p. 218.
■ Winnecki, Monthly Noiic£t, roL xnTiiL p, IM ; D«yWr toe. eit. p. 21S.
THE NATURE AND CHANGES OF NEBULAE 279
iham found it without difficulty in 1891, and attributes
"its occasional evasivenes8 to '' uafaYourable atmospheric con-
ditions."' Yet they aeem hardly adequate to explain the
marked anoinali&a of its record.
Intrinsic change indubitably affects a amall nebula
attached in fan-shape to the variable star R Coronae Australis.
Suspected by Schmidt in 1865, it has been rendered patent
by Mr, Innes's observations.* When further materials are
available it will be of ^n^at interest to determine the relations
in light-change of these diasimilar, though nasoeiated objenta,
Again^ one of a group of nebulce in Virgo, observed by
Schmidt at Athens in 1862 (N.G.C. 5655), could not be found
by d'Ar«st in 1855, two minute stars appearing as its loctim
tenentes? If, as seema probable, the identical object was
inserted by Hersehel, from an observation of December 28,
1785^ as No. 498 of hia second class, its re-emergence to view
may at any time he looked for, Tlie collection to which it
belongs^ were judged by d'Arrcat (no doubt tightly) to be the
brightest '* knots " of a wide - spreading nebulous structure
(M 49). The vai-iability of one of them approximates to
the local changes of irregular nebulae, exemplified with most
certainty in the virtual efFacement of the " swan *' eection of
the formation in Argo. Prominent in Sir John Herschera
drawing* it waa missed visually by Mr H. G. Russell in 1871,
and is very feebly represented in the best modern photographs.
A bare mottling of the lacuna to the south-east of the " key-
lole " in Plate XVIL now marks the place where the nebulous
Ffiwan " formerly paraded its radiant plumage.
No change so striking haa, within two centuries, occurred
in the Orion nebula. Its organiaation appears, on the whole,
to be wonderfully stable ; for certain alleged light- fluctuations
of a partial kind * have not been thoroughly substantia ted,^
Those believed to affect the Omega and Tritid nebulae, seem to
have resulted in a modification of what we may call caast-lineef
^ Lick Publicntions, vol. ii, p. 172.
* Annals Cape Ohtervaii>r\i, vol. ii. p. 134 B.
' D" Arrest, Attr. NacK No. 1620.
* 0, StruiTB, V, J, 3. Aitr, Qe§. Jnhrg. lii. p, 35 ; M^fanget Math. t. ii. p.
BO ; d'Arreat. Astr. NaeK. No. 1366 ; H<ilden, fVask. Obxrvaiiifnt, 1S7B,
kpp- i- PP- 12If 23^.
* O. 3tone, Publ. Lwandtr WCormick Olaerv. vol. i. Plate VII, p. 271.
280
THE SYSTEM OF THE STABS
here advancing^ there encroached upon hj the oea of daikfiMi
which eiuToundfl them. In the latter oliject, a smgalu
apparent alteration in t^e relatiTe places of the multiple star
and the nebulous n^assea involving it, i& perhaps dne to Ibifi
instability of outlines. Sir John Herschel ia 1827 and 1833
described the star as located " exactly in the central Tacuitjr "
of tJie nebula^ and just at the point of convergence of tbe
three rifts dividing it throughout.^ But a drawing made
by him at tbe Cape in August 1335 exhibits the star, no
longer aa central, but as adhering to the eaet^n tnaes of
nebulosity, A similar state of things waa noted hy IAmod
and Smith in 1839,^ and subaista so obviously at the pmenl
time, aa to render a mistake about it inconceivable. Th«
implied change, however, must have taken place abruptly,
between 1833 and 1S35, aJid then cea«ed ; so that proper
motion, either of the star or nebuU, had certainly nothing to
do with it,' There seems no alternative but to admit that
the frontier4iues between luminosity and obscurity were, at
the epoch in question, very considerably "rectiiied."
Speculation regarding the uature of white nebulae must
be left in abeyance until their spectra have been satisfactorily
investigated ; but there is a consensus of opinion that those
aho wing a discontinuous radiance are lum inous through
electrical excitement. The fact of their incoroj^rable tenuity
was established by Mr. Ranyard in 1892, on the ground of
their ineffectiveness in imparting motion to bodies in their
vicinity; and highly rarefied gases in Rpaoe cannot be hoi
Gaseous nebula ate, in fact, reasonably believed to be at a
temperature not much above absolute zero. They are not,
then, incandescent, but rather " luminescent " ; their light is
independent of thermal conditions. The phospliorescencie
produced in a Crookea's vacuum-tube exemplifies, according to
M. Dealandres, their mode of illuminatioa.'* Cathode-rays
emanating from central condensations set their materials aglow.
M. Arrhenius, on the other hand, derives from exterior
^ Mtmoirt &. Aatr, Soc vol. iii. p. 43 ; Phil, Trans, vol. cxxiiL p. 400 ;
Hold^u, A7n«r, Jaurn. of Sf:ii:ncij vol. »iv, ji. 434 (1377).
* Tram. Apier. Phil. Sac vol. vij. p. 175.
' Dreyor, Manthly Notices, toI. xlvii. p. 419,
*■ Comptet Hfiidui, Ma; 20, Judb 23, 1002.
J
THE NATURE AJSD CHANGES OF NEBULA 281
acies the light -stimulus acting upon them. There are
ay indications, he tells us/ that space is pervaded Ly
itively charged particles expelled with enonnons velocity
the stars. These being absorbed by nebulse, occasion
ctxical discharges through the gaseous volumes composing
lem, their frigid condition notwithstanding; and Professor
Dewar's experiments assure us that excessive cold is no bar
to light-emiseioa. Moreover, none that is truly continuous
seems to be included in nebular radiations. Wliat passed
for such baa been analysed by Mr. Palmer into ranges of
faint, superposed bright lines,^ Associated stars, however,
yield genuine etellai- spectra, and have perhaps taken an
active part in the weaving of the textures they begem. The
unmistakable analogy, at any rate, between solar-coronal and
cometary forma on the one side, and nebular forms on the
other, indicates for all a kindred origin in the play of
opposing forces, generated by certain foci of condensation, one
of which is our sun, while the others can be safely designated
only as nuclear points. Where there is only one such nucleus,
the enveloping gases assume a simple globular or oval shape ;
where there are many, the result is exceedingly complex.
Irregular nebul£e are thus most likely potential star-clusters ;
they consist of a stellar framework, draped with nebulous
folds, spirals, and festoons, disposed along lines of force laid
down by the rival or concurrent energies of the compact
masses which it is permissible to regard as inchoate suns.
* Zthrbudi dtr Kosmischen Ph^aik, Bd. i. p. -la.
' Lick BulUtin, No. 35. loeq^UiOlitiea of the kind were long ago ftunpected
by Sir WilliAiEL and I^y HuggiiUL
THS DI3TA>'CE3 OF THS STASS
Ths most arduous among the problems of BieQu' artroDOiDf
was, filnguUrlj enough, the first to be attacked. Tt
attacked, indeed, before the possibiiiiy was eren remofeely di»-
cemed that Htollor astroDomjr might come to be regarded as i
Bubfitantive branch of science^ In the hope, not af penetntiag
the mocratable oecjeta oi the remote sphere of the fixed staz^
but of solving doubts about the motion of the earth, Copemiea^
Tycho, and Galileo led the way in the long series of experi-
ments on the appisrent displacements of tJie stars reBottiiig
from oar own annual travelluig round the son. Tlie interest
of the question whetlier such displaceinents existed or not, was
for them of a wholly '* parochial" kind; it lay in the test
they afforded as to the reality of the terrestrial reYolutioii&
Should the stars be found to shift ever so little by the effect of
perspective, then the heliocentric theory could no longer be
gainsaid ; if. on the contrary, they ignored sublunary ciroling^
the " pill " (as Kepler termed it) to be swallowed by Coper-
nicaos was Indeed a huge one. For the distances to which
the &xed stars had^ in that case, to be relegated, seemed in
those times monstrous and incredible; and monstrous and
incredible they would appear still, were we not fortsed by
iirecuaable evidence to believe in them.
Throughout the history of these inquiries, at least in its
earlier part, it may be taken almost as an axiom that the
largeat ostensible parallaxes were obtained by the worst
means. With each successive improvement in methods and
instruments, as the limits of possible error shrank, the dis-
placements apparently measured dwindled, and the stars
282
THE DISTANCES OF THE STARS
283
ae less accessible to attempted determinations. DuriDg
Bme tliree centuries, the ill-success of an aatronomer in thie
atter wa3 a measure of bis akiil and judgment. Eesulta
bbtaiaed with euapicious facility by inexpert obBervere utterly
raded the guarded scrutiny of such men as Tycho Brahe,
S'tadley, and Pond. Flamsteed, indeed, just at the close of
le seventeenth century, detected in the pole-star annual
itioaa which were certainly Twt illusory. Yet here too
leie was a caveat. Theory and fact did not correspond.
Let ua conBider for a moment what must be the viaual
Beets upon very distant objects of the comprehensive and
nceasing rounds of the planet upon which we are borne aa
%toTs. Unmistakably, to begin with, we see them in
dififerent directions at different times of year. In Jiinuary and
July, in March and September, and bo on, we are at opposite
ends of baae-lines 186 millions of miles in length. The stars
then must be continually thrown, now a little to one side, now
to the other, of the true, or " mean " places which they would
severally occupy if viewed from the immobile sun. In other
words, each describes round its mean place in a period of a year,
a small apparent orbit, which is nothing else than the orbit of
the earth projected in miniature on the sky. For stars flituated
in the ecHptic^ — -that is, in the plane of the earth's motion^
thifl orbit contracts into a right line, along which the star merely
swings to and fro ; for stars near the pole of the ecliptic, the per-
spective orbit is sensibly a circle ; while intermediate latitudes
afford all degrees of foreshortening. Every star — unless those
few lying close to the pole of the ecliptic^haa thus its epochs
of maximum parallax, six months apart^ when it seems to stand
alternately at opposite extremities of the major aits of the par-
allactic ellipse, and it is then that measures of its apparent
displacements can be most advantageously made. These
opportune seasons occur when the earth's longitude falls short
of, or exceeds by ninety degrees the longitude of the star. They
are accordingly different for stars with different longitudes.
The precise /orm of displacement due to the earth's revolu-
tion round the sun is thus strictly calculable for each individual
star ; the am4}'unt alone cannot be predicted, but must be obtained
by observation ; and from tliia amount the distance of the star
is deduced, Por each pamltactic orbit is a perfect model, both
284
THE SYSTEM OF THE STABS
in slukpe and nxes, of the e&rth's orbit as it would be nen froal
the iter, abridgiaeiit of compasB (down ta oontnotiOB into «
vbtttal point) ooKreaponding to a more and more profonnd i»'
mermon of the point of survey in the abywoB of apaeo.
'Hve patalUx of a star is then the dlfferenea b e ftw em
pofiitiooe aa seen horn either side, and from the centre of tte
earth's orbit. U is, in short, the angle subtended, at tbe
diAtaoce of tl^iat particnlar star, by the mean interral banran
earth and sou. Kow we can tell in a moment how &r off i
spectator most be to eee a line ninetj-three millions of
in length diminished to the angular dimension of, let u»
one second. He must be 206,265 x 93 millions of mila
distant But no star has yet been foond so n^r to as as tiu
Tliat is to say, the shift of no known star amounts to as mneh
aa the width of a sixpence held up at Charing Croes to
spectator at Stanhope Gate or at Millbank.
We are now in a position to understand why it was
Flatnsteed'a obeervatioDB of the ap]>arent diaplacetnenta
Polaris could not, when critically examined, be set down to
the account of parallar. The Btar seemed indeed to deecdbt*
regularly each year, a little ellipse of exactly the right tlu^
and as to ite sii^, there waa no d priori reason why the pole-
star should not hare a parallax of upwards of twenty seoonda
But there waa one irreconcilable discrepancy. The displaoe-
menta noted occorred at wrong times. Had they been of t
jiamlkctic nature, the position of the star in its minttte
fictitious orbit should have been invariably ninety d^reea in
advance of what it actually was. They were not then due to
parallax ; but obtained their proper explanation from Bradley's
discovery of the aberration of light in 1729.
During the ensuing century and a quarter, the only valid
results obtained in thia direction consisted in demonstrations,
renewed and enforced from time to time aa more conclusive
evidence presented itself, that with the instrumental means
then available, stellar parallax waa an inappreciable quantity.
Bradley showed that it must fall short of half a second, and
although his reasoning applied strictly to only a limited number
of stars, it was rendered at once more general and more cogent
by the investigations of Pond and Airy, of Struve and BeaseL
It thus seemed that astronomers should content themiselves
^
THE DISTANCES OF THE STARS
285
with the knowledge that the etara were exorbitantly remote, so
remote that tight spent at least four or five years in travelling
to us from the brightest of them, and might, for anything that
appeared, need an indefinitely longer time for the journey.
The labours and refinements of two centuries had issued in
fixing a loyjeT limit for distance, an upper limit for parallax ;
in isolating the sun from his compeeia by setting between
bim and them an unmeaBured stretch of desert space ; in
widening to a startling extent the boundaries of the visible
universe. Kepler's "mighty bolus" had to be swallowed in
its entirety.
At laat, in 1827. Savary of Paria brought forward a
method for fixing an upper limit to the distances, a lower
to the parallaxes of binary stars moving in known orbits.
The further off from ua such orbits are, the greater of course
their real si^e* and the longer the time taken by light to
cross them. Hence, the deviations of the moving stars from
their true places due to inequalities in light -transmission
must increase with their remoteness, and thus serve in theory
to determine the distance from the earth of the pair. Or if
no such deviations are apparent^ it should at least be possible
to fix an amount which tliey could not exceed without becom-
ing so. Savary, accordingly, professed to demonstrate in this
way that f Ursa Majoris, the couple most favourably situated
for the purposes of the inquiry, must have a parallax exceeding
^^ of a second * — must, that is, be at a less distance than
would be traversed by light in 1000 years. But the informa-
tion, however credible in itself, was not fully authenticated.
Villarceau showed, in 1878,^ that the method was inapplicable
except to stars of known relative masses ; and it was by that
time already obsolete. The light-equation in stellar orbits ia
too small to be extricated from errors of computation and
I observation, unless where the occurreaoe of eclipses sharply
I defines positions and epochs.
^K Besides, the end in view can now be compassed by
^Bvpectroscopic means. Measures of radial velocity in an orbit
of known inclination give at once its linear dimensions, and
eomparison with micrometrical data, its distance from the
* Co-nn. dts Temps, 1830, p. IflS.
• Ibid. 187a, p. fig.
THK SreTEM OF THE STAJtS
> deemed nwiMwry, ih—hiI lanfe^d^ i-niimliiii , T1» <
wctc of tbe dilfeiotial kind, and lfa» i»«™^«t»fc
, of Ibe e«rT«B into whkh thej wete proiectod by Me.
[fnnptod tlw ooorktioo Ihftt ben at lart wba a st^kr
tte gtnviaaMM of wfakh wu beyood cxTil The
I impartaooe of ita dftectioa, proDOonoed b jt Sir John
Ibe grooteot tmoiph et«r ochkrTed faj pnctinl
I eoa be wlimolnit firara Bendji deeUzmtMm that, otittl tl «i
1 001110117 ooppoowd. be was OBaUo lo fona an opinicn 4s 1
wbeiber fcbo pocoUasooof the neozoofcatezB ohonki be
hj tenthi, or by thooootidUw of a secood 1 '
The difltaoce from the earth of 6 1 Cxgni has been i
freqoeQtlf laTcatigated thaD that of anj other otar, and Km
Infling diflciepaziciBa notwithstanding, may bo coiieadeied M
OitiifactorUy oacertained Beeeel'a p&ralUx of aboat a Hasi
of a oecood was aogmented to 0*'42 bj Aawers's
in IS66 of the o&me dau, and to 0**47 hy Sir fiobert
raeosurGO at Dunslak.' Dr. HertnAati Davia's diacnanm rf
the Butherford platee in 1898 yielded a Talne of 0'*36;'
Profeaeor Bamard'a obeervationa in 1900-2 with the Teriai
re&actor proved closeljr coa^ta&totj} This nnobtnuaTc etar-
pair may then be contidentl}^ located a( a distance of
li^bt-years from the earth/
We aooordingl/ aee the coupled stars, not where ihej on,
but whore thej wfrc nine years ago ; that ie (mnoe tbor
proper motion is about b'*'l2 yearly) just forty-sijc aeoondfl of
arc behind their true places. The effulgent pointe terreetria%
determined are then mere sinmlacra of the real stars; they
pursue, without ever overtakiiig them ; they would continue to
shine and to travel for nine years after their originals had been
blotted out of the visible creation. Our views of all moving
obJButs are of course to some extent affected by this curious
kind of Ugh t -aberration j but in the sidereal heavens it
attaint* proportions that are not only large, but, for the most
purl, incalculably large. Our survey of the background
*■ MejnoirB R, Awir. Sx. yq\. xii, p. 42^
» A9tT, Nath. No. 386.
■ Abhandl%n^tn Sim, Akad. Berlin, laGS, p. lU.
* CtftuTnUa Uniwraity ContribittioTiSf No. 13, p. \3&.
• ititport rcrkei Observatory, 187fl-I902, p. 18.
* BftrreU, Jttrt^h. Journ. toL xriii. p. 398.
THE DISTAJS-CES OF THE STARS
289
tbe sky ma.j lag ce&tmiea, even miUeuniums, behind om
aimultaneoua survey of its fot«ground ; and the disturbed
^fuchroaoua relatioDa between the varied luminous coutenta
the sphere are, to our perception, incapable of readjustment.
Transported to the place of 61 Cygni, our auu would
ar about eighteen times brighter. It would represent
a star not of the fifth, but of the second magnitude, such ae
Polaris, or one of the Pointers. Nor ia it likely that the
Swan binary is massive much beyond the proportion of its
luminosity. The extreme slowness of its revolutions, on the
contrary, intimates a comparatively slight power of mutual
Attraction.
Fraunhofer'a construction of the instrument with which
BdBsel observed 61 Cygni, marked the turning-point from
failure to success in parallactic inquiries. The heliometer is
apecially adapted to facilitate them. It has two chief points
of superiority over the ordinary equatoreal and micrometer.
In the first place, much wider pairs of stars can be grasped
with it, its compass being, by the mobility of the semi-lenaesj
extended far beyond the limits of a single field of view. The
selection of comparison-stars is thus greatly enlarged, and the
qhanoes of a systemic connection with the central star fatal to
the purpose of the designed operation, are reduced to a mini-
mum. In the next place, the stars under observation can be
visually equalised by placing a wire -gauze screen of any
desirable opacity over the segment of the object-glass forming
the image of the brighter one, whereby batSing personal errors
are completely eliminated. These are the chief, but not the
only features of the heliometer tending to promote critical
precision ; and not the least among Sir David Gill's services
to astronomy was his development of the powers and upplica-
tioua of this imique instrmnent-
Bessere success with 61 Cygni gave the impulse to
numerous undertakings of the same kind. Their result
depended mainly on the skill or luck of the observers in
picking out from innumerable indefinitely remote stars the
few near enough to be sensibly displaced through the efiFecta
of the earth's motion. Two circumBtancea maitily determined
their choice.
That distance is a factor of stellar brightnesd is so obvious
19
be ipeJL D M cd m tnoBB. Admic;. .
t nmfft id vvfiet^r u actual light-povBr, v
HMJKorf mSSk mmum tkal the mart lostrcNM ottyects inQ :
foood Bttoog tboM m doeest proximity to (be earth. Kiccp-
Jimtm^abooBd; bat^ one vide even^ kbe tfaeonCioU
iavctve ntio lail wiwe rtkttaffr «2>d the aqaerB not o( toul
ligbt fonuafaeB at leeet a flaeble gude to aotoal £ict'
Sewal l UMna i' iaw ilus^^Vcga, Arctorus, Ckpdk a
Cygnti and Pofaav— wer^ <n thk gnNmd, fixed upon t-i
iawitigrtinm I37 & A. F. Pecera in 1842-43.' Hk n^i
obtaimed with the PuIkQwa vertical dicle, were absolote, bt:
imapeetiTe of oompadfioiu with other stars ; bat the deduc- .
paraUazca were «> small. &nd their " probable erron " m xAf
tlydy Urge, tb&t it woa di£Gcult to place much cxnifidence ift
IbeiD. Vet LhejT came «urprifiiiigly near the truth.
A Becond ciiterioii of neameei vas found in the appear-
anae of mpid tnobion. Thia varies m the same proportioii tf
diitiiioe. but in the revenB aense. At twice the dist&Dce, u
ideotical velocity produces only half the angular disphu:eineiit,
at tbroa times the diBtonoe, one'third, and so on. Tbuti,
apparent Bwiftnees^ oo less than apparent lu^re^ depeuds in
part upon vicinity, and the largest proper motions must beJcQgi
on the whole, to the nearest stars.
Aud, on the whole, parallax -hunters taking mpiditj d
advance for their guide have prospered the best. A 7*5
umgiiitude stair in Ursa Major, flitting annually over 4}
necoudfl of angular space, was found by Winue<:ite in 1858*
to liave a parallax ( - O^^S) inferior only, among those as
yot determined, to that of a Centauri. This insignificsut
object, numbered 21,185 in Lalande's great catalogue, is
separated from the earth by a light-journey of seven years,
ttud to thtit extent our observations of it are retarded. So
tlmt it ia in reality always 33" in advance of the place we
ore Gomi>eUed lo o^ign to it For a body claiming the tank
of a Buu, it is either very small or very obscure. Our own
ruling orb ia 260 times more luminous.
' Btruvtt Jftm^ ^icrom. p. clxii.
* XtUttkH/t fv^r pvp. Mitth. Sd. iii, p. 104 ; Mimoirtt, St Fitanbourg,
t> Til. ^ 1*0, I&53 i A$tr. Kadi. No. 1147.
■ AitT. Kadi. No. 1147.
t
THE DISTANCES OF THE STAKS
291
An 8^5 magmtude star in the eame constellation (Lalande
Jl,258), also dtstinguifihed for apparent velocity, discloaed to
Luwers'a measuremente with the Kbnigsberg heliometer in
1860-62 a parallax of 0"*26,' corTesponding to a ligbt-journey
12^ years, and a permanent displacement on the sphere,
le to its proper motion in that interval, of 55". The real
lirilliaDcj of the star is only ^^ that of the Bun. A sbill
Jer 8tar in Draco (Oeltzen 17»415) gave au even more
aphatlc warrant to confidence in ewiftnees, rather than in
fcre, ag a certificate of proximity. Kriiger, induced by ita
^eEirly movement of 1""27 to subject it to experiment, obtained
parallax of one quarter of a eecond j ^ while the fine binary
fstem, 70 Ophiuehi, with an annual motion of 1""13, proved to
removed from tha earth by twenty years of light travel
lax 0"'16).^ And all these results seemed, from the
illness of their '* probable errors," to be exceedingly tniat-
rorthy.
The probable error of any result, however, repreeenta only
phat we may call the uncaiLsed inaccuracies of the observationa
upon which it is founded. It sums up» according to the
doctrine of 'probabilities^ the effect of their deviations, in
either directioDj, from the mean. But it takes no heed of
"systematic" errors due to causes working steadily in one
sense, but, so to speak, underground. These are the real
eourcea of mischief from which fallacious parallaxes have
abiindantly sprung in times past, and which cannot, in the
present and future, be too carefully guarded against Especially
formidable are certain slight idiosyncrasies of perception, by
which measures of distance become modified with the varying
positions of the line of direction between the objects measured,
lelative either to the vertical or to the line joining the
observer's eyes. And since this subtle spring of error rises
and falls hanuoniouflly in a period of a year (because dependent
upon the uranographical situation of the stars under scrutiny),
it would be capable not only of completely^vitiating observa-
tions apparently accordant, but even of simulating parallactic
changes that had no real existence. Instrumental erroiB, too,
^ MoTttkty Noticts, vol. ixiii. p. 74.
* Ada, SocielfU. £tieni. Frnnitte, t. vii. p.
' Krager, Attr. A'ach. Koa- 1210-12.
««&
ii
•Uj 111 Mill iBlo dbct bf Dc. Bruaiii>« tn • uniua of
|itioMoritaikrpKaIUz«iX>pbtuibrt«ttD 1868 and 1874
Th> Ma« pi> tiwM »t of tbe Uwr^igb fllimiiiAtkn of errata it
M0» p«MB«i And ptnodicAl, Iim mm» hma gmw\i ully fblkwi
Mom dfcctnaUjrltun b/ tzioifcoUisBHn»Uia&inoiis''Ka0V
tbjmlf" of til* old Greek phOiMopiMo hu faaen tdban to
liMrt by MtrouomMk Tbcir naiam and eUbot&te tnqoibBi
reftfd not aMselj BJocoacopic ttiequiUtiaa of Bcale-diriaQM
and aemr-rdiiea, dwngw in tefractim, oortectioiiB for aben*-
llon kdU proper motion, tml the cuxming tricka of their own
DcrVM^ ibe oaprioes of cerebiBiion, all the wying ooaditioas
of p«ro»pUoa in ^to orgaiuim «.( their individual oommaad.
N'on« of thene precautioDA were neglected in the imporUnt
work executed bj Gill and Elkin at the Cape In 18^1-33.'
Fully aljvo lo ita subtle reqiuremeata, tbey g*Te to th«ir
deterinjaatioufl a procisiaij entitling them to standard tank.
Sir Dnvid GiU'i diacuasion, especially, of the parallax of «
Ontauri in a uiodel inquirj. It leaves, one maj eay, no stone
unttirnoU bcnt-ath which a eource of illuaion might lie oon-
OBftldd. Tlie reflulting parallax of 0"'75, accordingly, obtained
by iaUt»periik'iit cotiiiwiri»ons with no leas than four pairs of
■djaoent itara, im probably more nearly accurate than any
value of tlifl uort yot rugistered. The fact is definitely assured
that liKht, whiuh llioH from the suu hither in eight minutes,
> iftutrtf f)intrvatiotu, 1848-53, Appendix ; Mtmoirt IL Aair, Soc
ixvil, ]i. 44.
< liuthiin dt I'Amd, SI, F4tAnboaig, t. xiii. Suppl
' Utnuiri R. Atir* Soq, vol. Klviii.
THE DISTANCES OF THE STAES
293
ads four years and four months on the journey from our
Bt known neighbour among the stars. The corresponding
einee is, io round numbers^ twenty-five billion miles.
A joint attack on Sirius discloaed a parallfix of 0""38,
iplying a light-journey of 8"6 years. These were the first
Bure^ of the dog-star made imder perfectly Buitable con-
itions, and their repetition by Sir David Gill in 1888-89
fith the 7-inch Cape heliometer, finally established their
curacy,^
Of the nine eouthem stars investigated by GUI and Elkin,
76 — e Indi, Og ^^^ ^ Ei'idani, Lacaille 9342, and f Toncani
-were chosen for their large proper motions, and all proved
be meaaurably near the earth.^ Canopus and ^ Centauri,
on the other hand^ included in the list l>ecause of their
distinguished brilliancy, averred their extreme remoteness.
Prom the former in particular, no symptom of displacement,
progressive or periodical, coukl be elicited then or subsetj^uently.
This is really, when we come to consider it^ an astonishing
result.
Second only to Sirins in the southern hemisphere, the
star of the Nile far outshines every star north of the celestial
equator. As chief of the great constellation Argo, it seems
to command, while standing slightly aloof from, the daz^Ung
array of all stellar ranks spanning the heavens from the
Greater Dog to the Cross. And since its spectrum is marked
by nearly the same kind and amount of absorption aa that of
Procyon, we cannot safely conclude its mass to be abnormally
small in proportion to its light-
Both, regarded absolutely, must be enormous. The failure
of persistent efforts to detect any parallactic shifting in
Canopus obliges us to suppose it so far o& that its
light needs ai least SOO years to reach us; how much
longer, it is impossible to tell. At this minimum distance,
our 3UU would shrink to a tenth-magnitude star; it would be
one of the dense shoal of telescopic objects im|>ercept!ble to
unaided sense, and scarcely yet individualised by the industry
of astronomers. But 22,000 stars of tenth magnitude give
only the light of one Canopus ; whence it follows that Canopus
^ Annah o/tfu Oape Obtervatory, vol. Tiii. pt. it. p. 24.
* See Appeudu, Tabk V.
Sir Bnii
feo it a f""---- oi O'^S^ aqnvBknl to
of 109 yemtm. On asn, ae maJu i^,
mUk m»mfitK ihu ^^ the loiiRar this wIuSb orK
TbeUne had now cocne wbc« a
vi'biob innwiriw of tbis Inid
Hittetoi, ntaw^ww ^d faMa CBBtt to aefeq^ tlv
rr'"*'"*g ■objecta for tEeir iinmiiamln vitboot anj
to ihB otMitJiiMtHiti of resttlta. Tbe ootoome mn a miniiitiw
' detached statemmts as to fltelkr ilkUiajiiH, iatereatiBgp flMft
I7 itadf^ in a high degree, yet fnmpahiw of
for the paxpoee of any genenl con dM on. So long age ■
1853, Dr. Peten had pointed ont that what was needod fr
obtaining a funduaaital acquaintaoee vtth the etnictizt« 4f
the sidereal world waa not 00 much the detecminackD <rf
flxoeptional paraDaxee, ae the steady compLUtion of dsta lor
■one well-grotuided inference relative to the ^i«t»««i* of
defined star-cUeeee.^ Bat it was not antH thii^ yeas letar
that it became poeeibk to act on tbe soggeetioo.
Encouraged by the eoooera of tbe work just aooomplidied*
Sir David Oiil propoeed. January II, IS 84, a acheooe of
attack upon the problem of etar-difitanoee in its widest
bearings. Two " great cosmical que^tionfi " presented thtifr-
selveQ to him aa answerable hj the judicious distributioa of
some yeare^ continuous labour* The first related to tbe
average parallaxes of stata belonging to sucoesaive orders of
brigbtneHB; the jsecond to the connection between poialkx
and proper motion.^
A plan was accordingly concerted by which I>r» SUkxa
undertook the measui'emenbt with the new Yale Collie beUo-
loeter, of a coOBidetable number of representative northern
atare, while Sir David Gill dealt with a corresponding
Bouthem list at the Cape. Its final outcome was tbe anthem
' U47MirsM de Si. PMerxbour^. t. vu. p, 149.
Mimoin B, Att/r. Soe. ^L sdviii p. IBl.
THE DISTANCES OF THE STARS
295
Btermination of thirty-two parallaseB — tea in the northern,
Iwentj-two ia the southera hemisphere, including those of
all stars of the first magnitude.^ And thus at last, a scale-
unit for the stellar universe was provided. For, once we
know the distance in billions of miles or light jears corre-
sponding to the first magnitude — the distance, that is, at
which a " mean star " would shine with about the luatre of
Spii^a or Kegulus — the distances corresponding eeveraUy to
the lower magnitudes follow as a matter of course. They are
linJced together (unless we are deceived by systematic changes
of brightness) by an invariable proportion. We have already
explained what is meiint by the "light-ratio,"^ but it may
here be repeated that a atar of any given magnitude is^ by
definition, one 2'512 times brighter than a star of the magni-
tude next beloWj and 2'512 times leas bright than a star
of the magnitude next above it. But, since light varies
inversely aa the square of the distance, any star removed to
^2*512 = 1-585 times its actual distance, would show exactly
one magnitude fainter than it did before. This number, then,
1"585, the square-root of the light-ratio, may be desiguated
the " distance-ratio." It represents the difference of dietanee
equivalent to a difference in light of one stellar magnitude.
The relative mean distances of the various classes of stars
are then known ; to render them absolute, we only need to
ascertain the real mean distance of any of thoee classes.
It is true that, within each class, vast diaparitiea
escist. Small stars, comparatively near the eartb^ take their
stand on the same level of apparent brightness with indefinitely
large, but indefinitely remote bodies. What is invariable for
each magnitude is the proportion between real brilliancy and
the sq^uare of the distance. Symbolically expressed, — is
constant. That is to say, photometric unifonnity results
from a certain balance being atruck between remoteness and
light-power, by wluch the effect of equality ia produced. The
law, however, connecting average dietanee with apparent
lustre ia not invalidated even by the limitleea variety included
> Anitals Goft ObttrvatOTij, vol. yiii. pt, ii. 1900 ; PublicAiiom Vale Ob'
jervatonf, vol, i. pt. vi. 1903.
* Sea antt, p. 19.
does to
tbti catao of brightnw to
disUDc« ii probttblj not wiwitaral wiUuD the |
oatmdt of it.
Mtaawhik, the Cape aad Y«le resolts give ^ of a
•teood of ftrc ■« tbe sfersge panOax of firatHxtf^nitade snxm
in aU parts of the ■ky. Tbej eatabUi» at a distance of tfantx-
iJuw light fcan. the first haltug-atage lor expkmtioaB of
Mata^ IN'ce. Thuit inoonoedTat^jr reieotev taken all romwL
are the brightaet of the itellar host Got sun, bo placed,
would Hjnk nearlj to the fi/tli magmtude. Its fellow anna,
then, far aiLrpaw ita glory*
On the acale determined at Yale College, the mean dJBUnc^
of atan of the gecond magnitude h Sfty-two light jean
(pandlfix 0'''063); stan of the third magiiitode are at. eighty-
two light yCAFH (parallax 0"'04), and ao on ; the invaria>bb
ratio of l'G85 rL'gulatiEig the incxease of distance and decneeae
of magnitiido for eiich descent of one step, provided only that
light flufffltH no ethereal abnorption. "When we get down to
tho MixUHintli iiiiiguitiide. which is ahout the minimum visibiU
' IVnwwimb, The Stan, p. 313, vhtte (u Ur. T, K. Hutta hu renurksd) «
Tftloft of ] '414 for the diMU&«0-rAUd ia implied.
THE DISTANCES OF THE STAHS
297
Sn the largest telescopes (the Yerkes re&actor attains to one
"Snaguitude lower still), we find the theoretieal light-interval
lengLheued to 33,000 years; but there is no certainty that
m:Dj aucb far-travelled rays reach ub. The regular progression
of distances may not extend so far. It must stop eomewliere»
if the stellar syetem be — as we have reason to think it
is — ^of finite dimensions; at what particular magnitude the
break occurs, it would at present be futile to conjecture.
All that can be said ia that, distance becoming at length
eliininated as a factor of magnitude, the diffeieuces of the
fainteat stars represent, chieSy or solely, real inequalities
in shining. There may possibly, for instance^ be no " mean
distance " corresponding to the sixteenth magnitude. The
stars of that rank would not then, on the whole, be further off
than those of the rank next above them, but would> on the
whole, possess only ^^^ of their real light. This must be the
case — so far as we can see — at some stage of the descent into
the abysses around ua
Besides Oanopus, four among the twenty-one brightest
etaifl in the sky were found by Gill and Elkin inaccessible
to parallactic research. These are Kigel, Spica, a Cygni,
and ;3 CruciB. AH five must be Brobdingnagian orbs ; their
magnificence defies the realising efforts of imagination. In
singular contrast to them are certain swift, but dijn etars
i measured by Sir David Gill, notably one in Pictor of 8"6
magnitude, which cannot, since it has a comparatively large
parallax, shine with more than ^j^ the lustre of our modest
sun- Ten, in fact, of the tweuty-two stars determined at the
Cape, proved to fall short, in sundry degrees, of the solar
standard of light-power.^ But to what extent they depart
from the wide average of the sider&al system, we have at
present no means of judging. All that can be said is that
the variety embraced by it has a prodigious scope.*
^L Of the ten stars measured at Yale, Procyon, with a parallax
^%f C-334, giving a light-journey of 9'8 years, was found to be
the nearest to the earth. Altair, at a distance of 14 light-
years (parallax 0"'233), came next; Aldebaran, at 30 light-
years (parallax 0''"109), third. From Arcturus and Betelgeux
' Cape AniuiU, vol. viii, pt. ii. p, HI,
* OiU, Prec, S. J/riean. Phil. Society. Sept, 17, 1002,
298
THE SYSTEM OF THE STABS
an aIiuo8t identical result was derived. Kach is plonged ia
tt profundity of Bpnce represented hj 12fi years of li^t-
travet ; and tbi^ implies tht? r«al luminosity of An^turus to be
itpproximaU'ly 1000, that of Betelgeux to v&ty a, Httld on
either side of SCO times the solar brightQeas.
So clooely and so coELfiequeati&llj hare advanoeii in thii
arduoLii^ bronch followed the growth of improvemetit in
holiometere, that direct visual measurements for the purj^Me
with auj other instrumeut might almost s(^m waste of labour
Nevertheless, the traneit^circle has been imexpectedlj rendered
thus available. Professor Kapteyn originated, in 1SS9, t^
determination of stellar paiallaioa by diSerences in right
ascension, giving for fifteen stara results at once acknowledged
ft6 authentic ; * and hie method woa applied to ninetj-aii start
by Professor Flint at the Washburn Observatory (I7.S.A.) ia
1803'OG.' It is safe and expeditious, and serves as a useful
adjunct to work with the camera. Photographic poraUai
researches were effectively set on foot by Frofesaor Pritchard
His first experiment was with the classic 61 Cygui, of which
330 separate impressions, obtained in 1886-87, furnished the
materials for 30,000 measures^or " bisections" of star-images.*
For the immediate end iu view, these extraordinary pains
were largely superfluous; but they had the ulterior object,
fully attained by their means, of establishing the credit of a
□ovel and unfuniiliiiT method. The most delicate of all
astronomical inquiries was thenceforward^ with the full a^enl
of experienced judges, admitted to be within the competence
of the celestial photographer.
The advantages of determining parallaxes from setiaitive
plates are manifold. Perhaps the chief of them is the nearly
indefinitt) power of control they afford. Any of the imprinted
stars, situated at all near the prolongation of the major axis
of the parallactic ellipse (in other words, with a tolerably
large " parallax-factor ") may bo used aa a point of reference.
Comparisons can thus be multiplied almost at pleasure, and
inferred displacements with regard to one star checked by
recourse to another, duplicate plates being at hand for addi-
* AHr^ Jfioeh. No. 203S ; Annaltn dtr ,*iUmieartf in Lcidtn, Bd. tU.
" Publ. fVarhbttrn Obtervatoiy, vol. ri. 1902.
* Monthly ytflka, v<A. xJviL i*, 87.
THE DISTANCES OF THE STAES
299
[>nal safety. By the proper as8 of euch safeguards, delusive
results can be all but certainly excluded. Moreover, relative
paralittx becomes virtually absolute when coinparisODS are niade
with a great number of stars, moat of which are presumably
too remote to complicate the result by perspective movements
of their own,
"Within its peculiar province photography compriseB stars
too faint to be conveniently dealt with by visual means. For
the images of those much brighter, over-exposed through the
necessity of giving the small etais in their neighbourhood
time to imprint themselves, become diifused into blurred disca
unfit for accurate bisection. Plates, on the other hand, taken
by Dr. Schlestnger with the Yerkes refractor in 1903-4 proved
well adapted for obtaining the parallaxes of eighth and ninth
magnitude stars.' Trial waa made of only three ; but one of
them was a double star in Cepheus. found to be ten times
nearer the earth than Vega or Arcturus (parallax = 0"'278).
Yet the pair give no more than ^^ the sun's light, though
their rapid mutual revolution suggests the presence in the
system of considerable attractive power. It will be curious to
aecertain, when their orbit develops sufficiently to be com-
puted, the relation in its members of mass to luminosity.
The main object of present inquiry is to obtain a wider
basis for general conclusions regarding the distances of the stars.
For this purpose it is mote important to secure a considerable
number of parallaices reasonably well determined than a few
reduced by scrupulous care within the narrowest possible
bounds of error, Eesearch in this sense is already well on its
way. From statistics of proper motion, Frofe^or Kapteyn
has derived trustworthy estimates of the mean distances of
the stars according to their photometric rank." In doing
so he found it advisable to distinguish between the
members of different apecti-al classes, since the fact clearly
emerged from his discussion that^ — as Mr. Monck had indicated
several years previously" — Sirian and helium stars are fully
twice aa remote^ on an average, as solar stars of the same
magnitude. A colossal scheme of direct inquiry was besides
^ Astraph. Jtmm^ roL xx. p. 123.
* Attr, Naeh. No. ^487 ; Onmii^en Astr, Fubl No. 8,
' Aatr^ and AMtrGphysica^ toL xt. p, 701,
300
THE SYSTEM OF THE STABS
sketched by the Groningen astronomer in 1889' azid iti
feMnbility eBtabliahexl by experimental measurementa ot pUlM
UJcan hj Ftofesaor Banner at Helsin^ors, the results of which
were made public in 1900,* But the proposed pbotograpluc
stirvey of the heavens, by which the parallaxes of 800,000
Stan might poeaibly become known, is stlU in abeyance^ Itt
execution would be most costly in time, labour, and monej;
and their lavish outlay ia discouraged by the bofSing irtalliMM
of the quantities sought to be discloeed.
Meanwhile we may attempt to summarise the outcome of
preliiuiuary explorations. It is, in the first place, decidedlj
unfavourable to the existence of any large parallaxes. Tbs
possibility is, of oouree, by no means excluded that stars mftf
be found much nearer to the solar system than a Centauri,
but their diflcovery is growing every year less and less probable.
Sir Bobert Ball^ examined some years ago about 450 objecti^
in a manner which, though summary, would have Buffieed to
bring to view any parallax of a single second of arc. If one
was forthcoming. His list comprised a number of red and
variable stars, Nova Cygni, Webb's planetary nebula, and the
Wolf-Rayet gaseous stars in Cygnus ; and it may be noted
in passing that spectral peculiaritiea are almost invariatily
associated with an uncommon degree of immobility id the
sky. The ninety-six stars reviewed by Professor Flint on
Kapteyn'a method were of a more promising character; and
ninety'two were selected by Dr. Chase for rapid scrutiny
with the Yftle heliometer, because their large proper motions
supplied an argument of proximity ; yet, among them all, not
one aeema to be within a five years' light - journey of the
earth. Indeed, parallaxes even of one-tenth of a second^
signifying a Ught-iDterval of thirty-three years, are held by
Proftissor Knpteyn to be extremely scarce.* On the whole,
perhaps one hundred stars * have been shown to swing to and
fro sensibly in response to the earth's orbital vibration ; and
the number of fairly well determined parallaxes may be put
at about seventy.*"
1 Bull, da la Carte dit tSW, No. 3, p. 262. Ct PulMoh, A»tr. Nach. No.
4013.
* Oroningen Aatr. Pnhl, Ko. 1. " Dunsink OhaerrutiiimB, voL T.
* Qnmingeti Publ. No. 1, p. S3. * Nowcomb, The Stan, p. 149.
* Sm Appendix, TftbU V.
THE DISTAilCES OF THE STARS
301
The cardinal truth emerging from theae inquiries is that
the extreme isolation of the solar system. A skiff in the
Iddfit of a vast unfurrowed ocean is not more utterly alone,
out the same proportion would be borne by an oasia one
tnile across to a desert twenty times as extensive as the
Sahara, that our sun with hia entire planetary household
bears to the encompaasing void of space. The enormity of
its blank extent is strikingly illustrated by Father Secchi's
remark that the period of a comet reaching at aphelion the
naiddle point between our sun and the nearest fixed atar»
would be of one hundred million years ;^ and, by recent
ujeasures, the nearest fixed star has been pushed further back
into space by one-quarter the distance assigned to it when he
wrote. Yet the sun is no isolated body. To each individual
of the unnumbered stars strewing the firmament, down to the
fainteat speck of light juat shimmering in the field of the
Lick refractor, it stauda in some kind of relationship.
Together they master its destiny and control its movementa.
Independent only so far as its domestic affairs are concerned,
it is bound, aa a star to the other atara, by inQuencea reaching
efficaciously across the unimagiaablo void whicli separatee it
from them. The outcome of those influences in the trana-
latory motion of the eolar system we shall consider in the
next chapter.
1 h«9 M»k9, t. iL p, 146.
Tkk «tadj of the stars inevitablj leads ua to oooeader
ttdvancsDg movement in the midst of tbem of tbe son Aad
atteodftiit train of pLaneUi. There c&q be oo resaonable
-^^tid the thought is an aBtaandmg one — that wv mn
ga^ed on a voyage throagb space witboat starting-proitt or god
that we can know of, which to&j prove not wholly nueventfiiL
Ite progress may possibly bring aboat» as millenniiuns go by,
chaog«e powerfiolly influential upon human destiniaB ; nay, «a
incident in its course inay at any time, by the injscnUalik
decree of Providence, terminate the terrestrial existeztoe of oor
race, and consign the records of its ciTiliBation in dnst
cinders to the arid boBom of a dead planet. A ciirioiia
of helplesanesa, tempered, however, by a higher trust, is
duced as we thus vividly realise how completely we are
the mercy of unknown forces- — how Irresiatibly our liti
" lodge in the vaet wildernees " of the universe is
onward over an aoDual etietcb of some four huadred mUlioos
of miles, under the mysterious sway of bodies reduced by their
almost infinite diatancea to evanescent dimensions.
But, aa things are constituted, the tranalation of the sun'
household is a necessity, albeit one of startling import to o'
I selves. The stellar system is maintaiued by the balanoe
' forces, and motion is the correlative of force. Aa a star amon,
stars, the sun can only maintain a separate existence by con-
tributing its share to those harmonies of movement by which
"the heavens show forth the glory of God." Destruction
woidd be the eventual penalty of even a moment's immobility
- — a penalty, indeed, which might not be exacted until after the
dO'2
Htd9
TBANSLATION OF THE SOLAE SYSTEM 303
Ipse of many miliioos of years. It may reasonably be
Bumed that a Centauri exercises upon the sun the strongest
Attraction of any individual star; but a collision would ensne
very tardily upon abandoninent to its influence. The aua (if
undisturbed by competing piiUs) would fall from a position of
Test to-sra-rds its next neighbour, less than the third of an inch
in the first month ; the second month would see despatched
nearly a full inch of the journey of twenty-five billions of
miles; and although the acceleration would of course grow
more rapid as the distance diminished, upwards of fourteen
million yeara should pass before the firea of aun aud star.
probably become extinct during their gradual approach, could
be rekindled by the catastrophe of their impact.
There is then an A priori certainty that the sun moves ;
and assurance on the point is rendered doubly sure by
inferences from observed facts. For besides their annual
paraLai due to the earth's motion round the sun, the stars
have a "secular" or "systematic" parallax depending upon
and attesting the reality of the sun's motion round an
unknown centre. Let as see bow this -systematic parallax can
be investigated.
If the sun alone were in motion, and the stare at rest, the
reaolts in perspective displacements would be simple aud iin-
mistakahle. Each star would appear to travel backward along
a great circle of the sphere, passing through the two points
towards and from which the sun's course was directed. So
that there would be the acmblance of a general retreat from
the " apex " or solar point dit 7/im, coupled with a thronging-in
from all sides towards the opposite point, or " anti-apex." For
each particular star^ the amount of displacement should vary,
inversely oa its distance from ourselves in space, directly as
the sine of its angular distance from the apes. Hence, if the
annual parallax of even one such aensibly shifting star were
determined, not only the rate, in miles per second, of the
solar progression would at once follow, but the parallax of
^very other sensibly shifting star in the heavens could be
ieduced by a simple calculation from the relative quantity of
its apparent movement.
But the stars are not at rest. They have movements of
their own, greatly swifter, in many cases, than that of the sun.
$04 THE SYSTEM OF THE STABS
Fts^eotiTS fiflecU Are thos ta a great «xtooft wmakeL l€
thtff ffabttiL U U tnAthemstacttUj cearUin that era; rttt;
whatever its own ootme or «poed« refiecto the son's moCiott a
the itiiet tne&sure of its positioa with regard to it What in
called the "proper tnoiions" of the stare are then madsupflf
two parU. one real, the other apptuneat. They inehide i
eomtuOQ element, the separatioo of which from the hetEtf-
g«neoU5 admixtures dis^oiaing it, constitiOes the prohiem W
be solved.
With the instinctive appreciation of genius^ Horscbel vest
■Izaight to the heart of the matter. Wliat had to be done, bt
saw clearly, was to fiud out the direction which abould )»
given to the sun'e couraet in order to make it account far«
targe a proportion as po^ible of the sum-total of $telUr
moTements. "Our aim must be," he wrote in 1805, "»
reduce the proper motions of the stars to their lowat
quantitiea." ^ And again: "The apex of the solar motioa
ought to be BO fixed iis to be equally favourable to every star."
But how is this to be done ? Very simply^ if we only cotiaider.
as Herschel did, a few of the brightest stare.
Take, for example, four stars with conspicuous movemente,
two in the northern, two in the southern hemisphere ; namely.
Vega, Capella, Sirius, and Fomaibaut. The great ciitles, of
which each annually describes u minute arc, traced backward
on the sphere, yeiy nearly intersect in a single point situated
in the oonetellation Hercules,* Had we only the motions of
those four stars to consider, we should accordingly infer with-
out hesitation the " suu's wa^ " to He thitherward. Nor
ahould we be very far wrong. The moat refined modeni
determinations of tbe solar apex, founded upon the motions of
several thousand atars, differ among thomselTes to an extent
comparable with their mean deviation from the result of the
extremely summary proceeding juat indicated.
The graphical methodj however, is evidently applicable
only to a very restricted stock of data. When a crowd of
atars have to be taken into account, the points of intersection
of their respective circles of motion become spread over too
wide an area for a " mean apex " to be struck out fairly
' Phtt. Trant. tdI. %vv. p. 2*8,
* TbLs irat rotQ«rkud by Kltukerfuw, QminfriH^Ae ^achnefOM^ 1S73, ^ 3tK).
TRANSLATTOI^ OF THE SOLAB SYSTEM 305
gtweea them, even bj the exercise of a judgmeut as dieh
criminating as tliat which in 1783 led Herschel to place the
go^l of solar travel in the vicinity of \ Herciilis, The
accumulated facts must then be dealt with by a method at
once stricter and more comprehensive. A glance at the
itura of the task in hand easily auggeats to a mathematician
rhat that method should be.
The proper motions of the stars give, as already hinted,
le plainest evidence of individuality. The lines pursued by
lem run in all possible directions. But a aub-stratum
regularity underlies this seeming confusion. A mere
spection of the signs plus and minus, eiguifying respectively
ist and weatj and north and souths attached in catalogues to
le CDinponeijt& iu right ascension and decUnatiou of stellar
movement, auihces to show a general prevalence of law through
le unequivoi;al tendency of the signa to vary concordantly in
sing from any one to an adjacent region of the heavena.*
Lt a c&up d'eeil^ Argelander fixed the point from which this
ider-cuiTent of motion flowed, and so gave an improved apex
ifor the course of the sun, confirmed in the main by Bubsequent
irch.'' It ia then clear, in the first place, that no movement
possibly assignable to the sun can explain all stellar displace-
ments; a large residuum being real, and therefore by no ingenuity
to be got rid of. While in the second place, the nearer the truth
is approached as regards the direction and amount of the sun's
motion, the smaller obviouflly this residuum will be. Iu other
words, the most probable value of the solar motion will be that
which renders the "sum of the squarea of the residuals" of
stellar motion a minimum.
But why the sum of the squ^^s, and not the simple arith-
metical sum of the outstanding proper movements ? It needs
only common senae, aided by the most elemeutar)' geometry,
to get a sufficient insight iuto the reason. Any one can see,
with the help of a pencil and a piece of paper, that, if a line
be divided into two segmeute, and squares be constructed on
the scgmeuts, the sum of those squares will be the least possible
{when the line is equally divided, and will increase continuaUy
|Vith the inequality of the segments. This simple fact gives
' stone, Monthly Notices^ voL xxvii p. 239.
^ Mhnoirtt -priawdis d VAmd. St. P^tcreLourg, t. m. p. SSfl.
$oe
THE SYSTEM OF THE STAS8
Uie clae to tbe prioctpW of * lawt ■qiiBz«&*' lu oibjeci ii to
«lidt toch A qoaaXi!^ m will nuike the ^^*»*-"^'iTg enw* «(
olfrrttiiMi, or mbj other kiod of rasidtaAla, sa miall «s poaiUB
off mnuf^ Not iner&lf stnftll takan in the ftggre^^U, Us
fadnead impartially to a tmifbDU ievBl of imrigniBniin
Ihidflr tbene dfcmnstaujces, as we have seen from tbe on*
nderation of our divided line, tbe sum of their sqiiareB wiQ te
a mmimmn ; and it oan be mathematicallr demoosttsted UMt
the most probable result of goch investigations as are vm-
oeptible of tbiB kind of trsatment, is arrived at when tbs
condition of " least squares " is fulfilled.
This mode of attack upon the problecn of the son's tiatis^
latton was first employed by Argekmder in 1837. Afisomiag
|kra\'iBionaUy the correctness of Herschel*s apex, he |jtoo ce il id
to compute for each of 390 stars with aaoertained piQpv
motioos tbe linea along which those motions fihould [Hrooeed
if due to ayatematic parallax alone. Their deviations bom
the prescribed directionfi gave him '* angles of error," wbidi,
placed in the category of casual errors of obserration, and
treated by the method of least squares, indicated a corrected
apeXi such that by its adoptiou, the sum of the aquares of
the dI3eren£«e between what was calculated and what was
observed — that is, between the purely jiarallactic drift of the
stars and their actual displacements — was reduced to the least
possibie amount. The solar movement wos^ in a word, so fixed
as, in Herachel's phrase, " to be eqimlly favourable to every
star/' a condition fulfilled by directing it towards a point in
right ascension 260" 51', north declination 31* 17V Bat
there is much r^son to believe that the position of TnATcininm
neutralisation — so to call it — really lies some fifteen degtees
further to the east.
An important modificatinu of his method was introduced
by Sir Gem^ti Airy in 1859-^ Abolishing the conception of a
spherical surface of reference, he defined the linear move-
ments in space of the aufl and staiB with regard to three
directions at right angles to each other (" rectangular co-
ordi Dates"). No assumption of any kind was then needed;
the subject was treated with the utmost strictness and gener-
' Mimoires pr^tnUt, 1 iii. p. 690.
^ Meitutirs B. A^. Site toI xxTiii. p. 143,
TRANSLATION OP THE SOLAR SYSTEM 307
lity, and some possible causes of error were removed. Airy'a
id many points of theoretical superiority over Argelander^s
lethod. That, however, of introducing the oonsideration of
le quantity of each star's movement was to a great extent
juaterbalauced by the necessity which it involved of adopt-
ig precarious suppositions as to the distances of the classes
stars employed. The apex for the solar movement resulting
3m the coDfiideration of 113 stars was situated in R.A,
IGV 29\ Dec. -1-24° 44'; while Mr. Main's similar treatment
1165 stars shifted it to R.A. 263' 44', Dec. -J- 25V
This great subject waa again investigated by M. Ludwig
Struve in 1887-' The incitement to undertake a task
Bndered formidable by the very wealth of the materials at
disposal, was afforded by Auwera's fresh reduction of
iley's Greenwich observations. From a compariBon of
le star-places authoritatively determined for 1755» with
given in the St. Petersburg catalogue for 1855, a list
2814 proper motions waa derived, of which 2509 were
Available for M. Strnve's purpose. Among the stars for
various reasons excluded, were the seveti swiftest travellers^
as unduly affecting the result through motions no doubt
mainly ohginaL
The outcome of this exhaustive diacussion waa to place
the apex of the solar motion in "R.A, 273° 21', north declina-
tion 27" 19', a rate being assigned to it such that the space
traversed in a century, viewed square from the average dis-
tance of a sixth-magnitude star^ would subtend an angle of
4*-36. Admitting that stellar distance varies inversely as the
square toot of stellar brightness, hence that stars of the first
are, on an average, only one-tenth as remote as stars of the
sixth magnitude, we can, with the help of Dr. Elkin'e mean
parallax, for the former class, translate this angular into linear
velocity. It comes out 14^ miles a second.
Well-nigh the whole of the stars visible to the naked eye
in the northern hemisphere concurred in M. Struve's deter-
mination. It was conducted on Airy'a method, likewisa
adopted in 1890 by Lewia Boaa in a discussion of 253 proper
motions extracted from the '* Albany zone," the observation of
1 Mcnoirs R. Asir. Soc tdI, Txxn. p. 27.
■ Mi»ioirA» dt St. r^irgbourg, t. luv. No. 3, 1S87.
808 THE SYSTEM OF THE STABS
which had just then been completed for the AjrtzoooiBkJH
Oeaallaohaft Catalogue. He obtained an apex in RA. 2^0'.
J>^40V near thti quadruple star e Lyrse; aod recurring to
the subject in 1901, finally concluded for a point five degicM
further north.* A Dotable attempt^ too, was nude "by IL
Oscar StumpQ in 1890' to show th^t the apexefl aepaiatelj
deduced from various clasaea of stars shifted ^^temiitically on
the spliere. This aeemed to involve the important difxjasare
that the groupa of stars oom^ider^ had distinctive aggr^tM
MorementSj and were hence dominated bj difj^rent gtaiita-
tional influences ; but the effects brought to Tiew have ptobahlj
aa much to do with the correction of catalogue-placee as with
the laws of sidereal construction/ That theae are alao ooa-
cemed, was proved by a reseitrch based on the proper niotioM
of Groombridge'a circumpolar atars^ executed by Measra. Byaen
and Thackeray at Greenwich in 1 905.* Solving their equation*
separately for stars of the first and second spectral types^ they
obtained from the separate eoUectioos markedly divergmt
directions for the sun's route» and thus, aa the upshot of
their experiment^ laid bare one of the hidden lints between
the dynamical and the physical relations of the stellai
world.
A material advance was made towards disentai^Iing the
intricacieB of tho solar movement by an innovation in the tnat-
ment of proper motions. It might have been supposed that eveiy
device for their manipulatian had been exhausted, and that tha
decipherment of their perspective significance was complefce, at
least in principle ; yet Professor Kapteyn contrived, in 1893,
to give it a novel stamp of clearness and certainty. ^Resolving
one by one the whole stock of star-movements at his disposal
along, and at right angles to, the great circle passing through
a solar apex aagumed as the most probable, he succeeded m
isolating their parallactic element much more perfectly than
had been done before. The fundamental nature of the
problem was thus laid bare ; obscurities wero dissipated ; and
there ensued a determination of first-rate authority, accor
1 Astr. Journ. No. 213. s jj^^ ^^^ ^qi^
* Astr. Nach. Jfos. 29M-S00O.
* Kaptejro, ihid. Kos. 3721-22, 3869-60 ; Pwu. A-m*terd^m Acad. ^^finaS}
Jiiti. 27, 3W0.
* Sfonlhli/ Jiotiea, voL Izv. p, 43a.
■din^
TEANSLATION OF THE SOLAK SYSTEM 309
which the sun's path is directed towards a point in R.A.
174°. D + SO", just six degrees south of x Lyne. Ita flub-
otial accuracy was vouched for by ProfeBsor Newcomb'a
Bterly researches.^ Profiting by long experience in evading
Wtfallg and estimating aources of error, he deduced from 2627
lall proper motions a solar apex in E.A. 274°, B + 31° ; from
SOO larger, one situated in E.A. 277', D + 31^ Which result
ervea more confidence, cannot off-hand be decided ; but we
ay hope — although this is by no means sure — that their
ifference representa the surviving extent of uncertainty.
The plan of inquiry just sketched, altliough it serrea
wonderfully well, on the whole, for the ascertainment of the
oute followed by the solar syetem in space, avails little
Dr determining its velocity. For this purpose, the distances
the stars employed aa indexes should be known ; and they
AQ only be estimated for ranks and classes, more or less
ariously. Kapteyn and Newconib htive, however, vastly
iproved the method of evaluation, and they agree in fixing
dn miles a second as the approximate rate of the sun's
Burney, But a more direct way of arriving at it has, in
ent times, been thrown open,
We have elaewliere explained the principle of spectroscopic
determinations of motion." Their peculiar value consists in
their independence alike of distance and of visible displace-
ment. Referring to movements visually imperceptible, they
complete knowledge of stellar velocities by giving their other-
wise unknown " radial components." Apart from this mar-
vellous application of the spectroscope, the real directiona
pursued by the stars as they ti^avel could never have been
ascertained, since we can immediately discern only that part
of their motion lying ticross the Une of sight, which, in
individual cases, may be all or none. By the spectroscopic
revelation, however, of motion in the line of sight, the miaaing
element is supplied, precise and particidar knowledge may be
had for the asking, and the etara voyage under astronomical
crutiny, no longer as mere flitting bright specks on the surface
an imaginary sphere, but as buds in space of three dimen-
sions, each with its secret in petto, and its deatiny in reserve.
' Astr. Joum. No. 457, 189S ; The Start, p. 91,
' Siti. o/Attr, 4th ed. jip. 200, 38S ; ante, p. ISiB.
310 THE SYSTEM OF THE STABS
The ejects of reoesBioD and approacb on the ligbt emitted
bj moviog objects being phygioal and real, the^ ranun
unimpaired by distanoa Out at the verge of the stdonL
Bystem, or cloae at hand withiD our own atmospbeie, thej ue
the HLme for the same velocities, and can, with a sufficient
Ught-fiupplj, be detected with equal facility. Hence their
special applicability to the problem of the suu^a speed. Tb
determine it with reij approximate accuracy, it needs oulj to
compare the average radial celerity of a good number of stan
lyiug in &t>Qt of the son's way with ibat of otheiQ he is tear-
ing behind. Movements of upproaeh must* on the whole,
predominate in the oue direction, movcinents of reoeasion io
the opposite, half the mean difference representing the late of
tranaport of our system relatively to the stais used for the
ooroparisou. The apectroseopic method, nevertheless, did not
become ideally effective for this purpose until the twentieth
centuvy had begim to run ita couree. Experiments with the
51 stars radially measured at Pot&dam were evidently tenU-
tiva;^ they forecasted rather than a£brded results. At Ust,
in 1901, Professor Campbell,^ having collected with the Mill*
epectrograph data lees iuadequate to the end in view^ deduced
from them ii movement of the solar system towards an apeat
in R.A. 277' 30/ D + 20^ at the rate of 12^ miles a second
The velocity may be depended upon — it is unlikely to bo
erroneous by more than a mile per eecond ; but the direction
ia subject to a somewhat wide uncertainty, eapecially aa
regards declination. For the 280 staia taken into account
being situated for tbe most part in the northern hemisphere,
the goal determined by their means was probably displaced
towards tbe equator. The deiiciency of southern stare wiU,
however, bo supplied by tbe work of the " Mills Expedition "
now in progi'eas at Santiago ; and a research, based on sym-
metrically an-anged materials, will then be practicable.
Thus, both the course and speed of the fiun and planets
are not only included iii the category of things knmoahle, but
there ia every prospect of their becoming known with more
and more satisfiictoiy exactness in the immediate future. All
1 Homana, J3lr. Nath. No. 3714 ; Schtinfeld, K J. S, Atir, 0«. Jthig,
Eli. p. 6& ; Voxol, J3tr. JVtwA. No. 31&0.
* Asf:r<fph. Jmij-n. toL liii, p* 80.
TRANSLATION OF THE SOLAE SYSTEM 311
\t is needed la a closer and a wider application of means
iy in the bands of astronomers. Still our cnriosity will
even Iheii be satisfied. The value of the two items of
formation within our reach is indeed incalculable. They are
Htu qud nOTi for the furtherance of intjuiriea into stellar
nechanics ; are they to be a n« plus ultra as well ?
The Bun, we are well assured, is not travelling along a
light line. The universality of gi'uvitation makes recti-
aear movement next to impossible, since no cosmical body
fcn traverse apaee under the sole guidance of ita own primi-
ve velocity. It is true that, supposing primitive velocities
Itogether abolished (and we know of no necessity for their
istence), any number of bodies might be united into a
fatem eudowed only with pendulum-like motions. The eun
ad stars might tbua, by an abstract possibility, be totally
void of advancing or circulatory movements^ each swinging
for ever to and fro through their common centre of gravity.
But it ia practimlly certain that this plan is not realised in
the sidereal system.
The path of the sun is then a curve, but a curve moat
likely of such vast proportions as to remain for ages indis-
tinguishable from a right line. Strictly speaking, its direction
is continually changing; the apex of to-day will not be the
apex of to-morrow ; atili less will it be the apex of a milUou
years hence. Yet in a million years, it may quite conceivably
not have shifted from its present place in the sky by more
that! the width of the full moon ; and our beat determinations
still fall far short of the accuracy which would enable ua to
detect a change of half a doxen times that amount. Directly,
that 18 to say; indirectly, a much more insignificant alteration
might disclose itself. We will endeavour to explain how.
Pond, who in 1811 succeeded Maskelyne as Astronomer
Royal, made the remark that the sun's motion must produce
a kind of secular aberration of light, by which the stars are
permanently displaced from their true positions.* The well-
known consequence of aninitd aberration is to make them appear
to describe little ellipses, the aemi-axes of which depend upon
the ratio of the velocity of light to the velocity of the earth
^ Li&gre, B'ulL d* VAcad. BnuolleB, t. till, p. 168, 1859 ; O. StniTe,
Mifiwirtt, St. P^terftbourg, t. r, p. 106, 6* Svrie.
313
THE SYSTEM OF THE STARS
ia its orbit. But the svLn*s orbital moTement being
BO far as experience yet goes> in one direction, the abemtko
due to it is in one direction too, and is heuoe constant, ud for
the present beyond the reach of obeervation. It is, boweTK.ooo-
stant only ao long as the movement producing it remains ssniti^
so. As the latter changes, it will change too, and may in thk
[manner be brought within the domain of bunaan cogmaurae:
For upon the acceleration, retardation, or deflection of llw
sun'a movement systematic changes among the stars sbo^
I ensue, the nature of which would at once betray t<beir oii^Ow
The total amount of this secular aberration may be roughly
stated as oae second of arc for every mile per second of the
sun's Telocity. Hence, stars 90^ &om the boIat apex an
pushed forward towards it by about 12", the effect upon
other stars diminishing with the sines of their distanoes im
the sphere from the same poinU These abeiralionaJ can be
distinguiahed from the parallactic displacements simiJarly
occasioned by their indifference to remoteness in space, Sl»n
far and nea.r, bright and faint, swift-moving and tardy, are
equally affected by them. But while it is quite certain that
visual disturbances of this kind are produced, their interest
must for a long time remain purely theoretical Indeed, it
may well be th^tt the modifications reodering them sensibls
and inBtmctive, will proceed with such exorbitant slowness
that not even astronomical patience will avail to nnmask them.
We do not know the plane of the eun'e orbit- — only the
direction of one line in it. And that line, pointing towards
the constellation Lyra, makes an angle of about 60" with ths
Sim's equator. Thus, the solar movements of rotation and
translation would seem to be unrelated one to the other ; and
the planetary revolutions to be similarly independent of inter-
spatial travelling. Our whole system is driven obliquely
upward by a power which, taking no apparent account of ita
domestic economy, must have a Bource dist'onuected from
originating impulse of the helicoidal gyrations illustrated
Fig. 36, from a diagram by Professor Yoimg.
A remarkable feature of recent improvements in the deter-
mination of the sun's course through the heavens has been to
reduce to insignificance ita deviation from the plane of the
Milky Way. This is an implicit testimony to their value.
ita
"I
TRANSLATION OF THE SOLAE SYSTEM 313
« "¥*
is difficult to coDceiye that course preflcribed otherwise than
the combined attractions of the galiictic myriads. The
lost probable auppositiou aa to the situation of the centre of
force ewaying our syatem is that it lies somewhere in the
cloudy zone which bo enhances the mysberious beauty of our
skiea. If the orbit we are puxauing be approximately circular,
tlien ita centre must be distant by a quadrant of the sphere
from the apex — it must lie
somewhere on a great circle of
which the apex and anti*apex
ate the polea. Now tliis great
circle cuta the Milky Way at
two opposite points in Cassiopeia
and Centaur, and there, accord-
ingly) two alternative centres
of the Bolar motion might be
looked for. Argelander chose
for its position the spot near
Cassiopeia »iarked by the
great cluster in the sword-
handle of Perseus ; ' but the con-
jecture made no pretension to
scientific authority, and the
postulate upon which it was
based of the sun^s path being at all nearly circular is in truth
of a highly precarious nature.
We are even ignorant whether the ascertained translation
of our great lumioaiy representa a primary or a secondary
order of etellar revolution. It perhaps merely indicates the
interstitial movement appertaining to the aun as a member of
a restricted group of stars, the common transport of which
proceeds undetected in a totaUy different direction. Hence
the possibility, suggested by Herschel, of the presence of a
higher kind of systematic parallax than that revealed in the
drift of bright stars.^ And Professor Campbell wrote, after a
full century had ripened experience : " Tlie motion of the solar
system is a purely relative quantity. It refers to specified
groups of stars. The results for various groups may differ
1 Minuiru prAunC^, St. P^tersboiu^, L iiL p, 602.
» Phil Trans, vol ksiiL pp. 1276-77.
Pio. 39.— Tb« EartLii Uotian Id SpouA
au
THE SYSTEM OF THE STABS
widely, and all be correct"^ So far. bowerer, no toi^ible
evidei&oe has been adduced to ehovr that difierenoea of thi^
kind^ grounded in the nutm^ of things, really exist If they
do, they esoape through the wide meebes of the neta wiib
which we oapture grosser facta.
Pro^resa is here only poeeible through careful and mina
study of the residual movementa of the stars — of the mo
ments, that is to say, which remain after the ge&eral
live effect of the sun's motion liaa been subtracted, and wb
fbetoag; accordingly, to their indiv^idua] selrea. The queedons
connected with them which most immediately present thca^H
selves are thc^ : Has the sun compunioDs ou its journey, c^l
does it travel alone ? and. Are real stellar displacemeDte
govemed by any obvious law 1 ^m
The great multitude of the stars are, to all appcaranoi^l
indifferent to the transport of our system. They have clearl/
no share in it. Just because they stand aloof, and act a?
indicators of the way, its progress becomes eensible to us.
For motion is not alone undiscoverable, it is even unimagin-
able without some fixed point of reference. Yet we caQoot
pronounce with certainty against the existence of a particular
dynamical bond connecting the sun with some few of the stars,
which form with it a company associated by subjection to
identical influences, and engaged on the same journey thiough
space. As to the criteria by which such associated stars, if
present, can be discriminated from the rest, something will
said in the next chapter.
There, too, we will consider what answer should be given
to our second query. A great deal depends upon it as regards
our conception of the sidereal universe. Nay, the result of
inquiry upon the point has a vital bearing upon the subject
we have just attempted, however inadequately, to deal with.
For the assumption that the absolute movements of the stars
have no preference for one direction over another forma tb^fl
basis of nearly all investigations hitherto conducted into th6^
translatory advance of the aolar system.* The Uttlc fabric of
' AitTOph, Jimrn. vol. liii. p. 87. ^^
* BrBT^ig, it LB true, diaciird«d th« hypothesis of casual propor luotiona, bq^B
hftd to flubatituta for it (^uasLiouiible aBsuniptions regmrding stellar mosses, dis-
t&Dcea, and velocities. -Vaurna2 de LiouviiU, t. riii. p. 1S£. [Sen Kaptej
AstT. NtKh. No. 3723.)
1
TRANSLATION OF THE SOLAR SYSTEM 315
laborioosly acquired knowledge regarding it at once crumbles
if that baaiB has to be removed. Profitable inquiiy into the
circumstances of the sun's journey have b^n rendered
feasible by the supposition that, for tiie purpose in hand, the
movements of the stars may be treated as casual irregularities ;
should they prove to be in any visible degree systematic, the
mode of treatment adopted becomes invalid, and its results
null and void. The point is then of singular interest ; and
the evidence bearing upon it deserves our utmost attention.
CHAPTER XXIV
THE PROFKR MOTIONS Or THS STAJtS
Wma^ the relative poaitiona of the Btarg are compared at
cotialderable intervals of time, they are i& many- oases found
to have uadergoue amatl, but unmistakable cbangea of a
Beemmgly capricious chamcter. ^eae are termed * proper
motions'* to distinguieh them from merely nominal ahiftings
due to the slow variation of the points of reference which
[serve to define the places of all the heavenly bodies as seeu
projected oa the inner surfaoe of an imaginary concaye epb^^
Proper motions are by no means easy to get at. Only from
the most delicate observations, and with stringent precautions
for bringing those at distant dates nnder preciaely similar
conditioua, can thoy bo elicited with satisfactory accnracj.
Otherwise, some trifling systematic discrepancies in the com-
pared catalogues, or oversights in corapufeition, might simulate
genuine effects of movement, with disastrous influence upon
Bideieal investigations. Hence, proper motions cannot gener-
ally be regarded as established unless, in addition to the
terminal observations showing a sufficiently marked change
of place in the course of thirty, fifty, or one hundred years,
at least one intermediate observation is at hand to prove that
the suspected motion has proceeded uniformly in the same
direction, and is accordingly not the creation of peEwmal
instrumental inaccuracy.
Although not one among the scores of millions of stars
can, with any show of reason, be supposed at rest, only
ten thousand of the stellar army have, up to the preaent,
shown measurable and progressive displacements.* Many of
^ DyaoD, OifMr%)atorfft vol> xiviii, p> 275<
316
THE PROPER MOTIONS OF THE STARS 317
ieae, icdadiug nearly all the l^ieidce of the northern hemi-
sphere, were observed by Bradley between 1750 and 1762 i in
the aouthem, Lacaille's amiultaQeouB tabours aerve to authenti-
cate the changea of some three-score of objects to which he
devoted especial care- So that a large stock of highly accurate
data already posseflses an antiquity of ooe and a half centuries ;
the cataloguee of Piazzi^ Lalande, and Groombridge are of two-
thiide that age ; while multiplied subsequent obaervationa
afford a further supply from which fresh and well-detennined
proper motions ai© continually being harvested from the seed
planted by an earlier generation.
The aspect of the heavens iy, to the unaided sense, virtually
unchanging. The conetellations disclosed at the present time
by the nightly withdrawal of the veil of twilight would be
famiLar, cotdd they revive to survey them, to the watchers
irom the towers of Babylon. And most of the star-alignmeDts
given in our text-books might be as useful to students of
celestial physiognomy a couple of thousand years hence as
they are to-day. Every one of the indicated stars will indeed
most probably, by that tin\e, have shifted ita place to the
extent of many thotisands of millions of miles. Yet so over-
whelmingly vast is the sidereal ecale that thousaude of nullions
of miles measured upon it sink into insignificance.
Stars advancing in a century as much as 30", or about ^
the width of the full moon, are counted rapid travellers ;
and the swiftest class, with secular motions of 100'' and
upwards now embraces about one hundred members. Each
of these, were it bright enough for ordinary perception,
would in a couple of millenniums become very sensibly
displaced even to an unskilled observer. But only a smalt
proportion of the quickest starB are visible to the naked
eye, and only ten reach the fourth magnitude ; hence their
shiftings make very little difference in the general e£fect of
the starry skies.
As might have been expected, the stars in most rapid
apparent movement are among thoae nearest to the earth.
Vicinity, in fact, and ang^dat velocity vary together. Die-
placements on the sphere are large just in the proportion that
the distances of the objects travelling identically in space are
small. Were there any approach to uniformity in the real
iia
THE SYSTEM OF THE STABS
velocities of the stars, we cauld then f&irly estimate, tMSn
^ their seeming movemeDte, their relative aituatiotia as legudi
' onrselvaB. But there is do auch approach to tmifonoi^.
Boundless variety prevuihi hero, as in every other branch
.of sidereal Btatistic& Stars with large proper motions ttt
Bometimea enormously remote; and, if stars with large pftril'
laxee and little or no movemeot have not been diacovercd, it
is perhaps because they have not yet been looked for. Their
occurrence, for a reason to be presently explained^ would be d
great interest^ and is not unlikely to be certified by mewure-
ments on photographic plates^
But, however great the range of variety, it aeems certain
beforehand that, on the whole, the amount of visible motion
in % given number of stars must decrease as their distance
incre&ees. And since their brightneas falls oCT at the «aiue
time, although mudi more rapidly, there appears no escmpt
from the concluaiou that motion and magnitude must, on i
wide average, vary together aoeording to a definite ratid
From stars of the sixth photometric magnitude^ for inatAnce,
we receive only oue-huudredth part of the light seat to us by
atara of the first magnitude ; they must then, one with another,
be ten times more remote. Otherwise, we should be driven to
the unwarrantable aasumptiou of a systematic diflTerence of real
lustre between apparently large aud apparently small stars.
But, if the average distance of sixth -magnitude stars be ten
times, then their mean motion should be only one-tenth that
of stars of the first magnitude. Yet in point of fact thia
is not BO, The proper movements of classes of stare diminish
indeed very notably with their brilliancy, but not in the
computed proportion. The discrepancy deserves attentive
study.
The average proper motion appertaining to the sixth
magnitude, aa determined directly by M, Ludwig Struve
from 64Y of Bradley's stars, is 8" in one hundred yeaiK*
■ Ten times this quantity^ or 80", ought to be the average move-
■ ment of stars of the first magnitude. But the mean derived
■ from the actually observed shiftinga of the twenty brightest
I stars in both hemispheres is only ^O".
B Stars of the second magnitude are still more noticeably
H ^ M^meir«4 tU St, POtrthourgt t, xixv. Vo. 3. p, S.
THE PROPER MOTIONS OF THE STARS 319
ert. They should be, on the photometric scale, 6"3 times
to the earth than stars of the sixth icaguitude. This
ovld give, for theix mean eecular motionj 8''x 6"3 = 50"'4.
Twenty - two such stars, however, from Bradley's and the
Pulkowa catalogTieSj show no more than 17". And even this
low figure more than doubles that repreaeutmg the average
movement of forty-two eouthem etars^ of 1"7 to 2'7 magni-
tudes, forming a descending Bcquence with the ten of first
magnitude. Nor is this average improved by considering only
the first twenty on the list, from ^ Crucis of 1*7 to k Orionia
of 2'2 magnitude. The swiftest of these (7 Crucis) travela
only 20" a century; taken all round, they move S'^ or with
exactly the speed of stars presumably more than six times as
rem^ote J
The anomaly of low apparent velocity is accentuated by
the close agreement between M. Struve'a results for stars from
the second to the fourtli rank inclusive. A glance at the
accompanying Table from his Memoir will Ber%*e better than
verbal explanation to make the matter intelligible. The object
of its compilation was to exhibit the divergence between the
proper motions actually determined and those computed from
the basis of the mean secular displacement corresponding to
the sixth magnitude. In the fourth column, however, we
have substituted figures derived from strict photometric star-
diBtancea for others depending upon a scale of distances in-
volving dubious assumptions.
Table of Stcvlar Mean Proper Motions of <dl BradleyU Stars
differing hy not leas than dffht-tenths of a ttiagnitude.
M&gbitudt.
No. of Stan.
Mmn MotiCNL
Obwrrvd.
OompnifKL
1
9
8
4
E
ft
T
8
Q
22
61
lOfl
S18
64?
92
11
l7"-2
ir-5
16"'2
S'-a
r-8
80" -0
60'-4
sr-a
20*^8
8"-0
ro
3*'2
320
THE SYSTEM OF THE STABS
It will be obvorred thjit the Telodty of each order farigbWr
thfta the mxth filU siunt of ita thMvetical ■mooofc, while tlMt
of the Cftinter onieni exoeedfl it. We hflflten to add that {m
IC StruYe pcanU oat) little or no dapendaaoe can be pUcsBil
on the Above mean rate of eighth^mgnitiide motion dedaoad
from measoremente of otdj elerea objecte.
And DOW, what are we to think ? How can we aoconnt
for the indicated deficieiM^ of proper motion in the brighier
aUra t Three poesible expl&fiatiODs pneent themselves It e
eonoeirable that atara, ray of the sixth and aevecthf axe leaUj
mailer ot dimmer bodieB on an average than ataxs of the fiiBt
and BBOond magnitodea. and ax9 coQaequeatfy lea retoote than
they shotdd be o& the mote uatuial supposition of their
equality. Their diminished distaace would then at oaw
render their extra celerilj intelligible: Again, thero ma^ be
a systematic Increaee of motion outward from the son, pro-
ducing m the fainter ators preponderating latee of displace-
meat. Or thirdly, there may exist a special cUs oi stna
deficient in light^power, but trarelling with exceptional speed.
by the inSueoce of which the balance of seeming ewiftaeaB ia
Corned in favour of the less brilliant ciaases of stars.
Of these alternatives, the second may be dismissed ai
being at variance with our best iuformatiou. There remain
the Srst auil tliifd, neither of which, certainly, represents the
whole truth, although each not improbably corresponds to
some p&rlial aspect of it A hannonious adjustment of their
olaima to credibility is thus difficult to bring about amid the
joBtling of mutually adverse inferences Professor Kapteyn
boa efttabliahed, by diligent sorting and aifling of multi-
tudinoa? data, the broad principle that proper motion varies
in amount in the due proportion of di&tance. But he has
also established that magnitude is no safe index to distance^
apart from the discrimination of spectral typ>ea Stars of
Sirian and helium quality taken all round ore, in fact, 2*7
times more remote than solar stars of the &ame pliotometric
rank. The former accordingly shine with a seven -fold
intensity comparatively to the latter. Hence, variations in
the distribution of the spectral genera may greatly perturb
the methodical progression of observed proper motions. Here
is one obvious source of anomalies ; and the large relative
THE PKOPEE MOTIONS OF THE STAES 321
iber of " white " stare included among the four or five
dozen most liisfcroufl gems of the firmament (aee Appendix,
Table I.) should be noted in this connection.
It muBt farther be inquired whether stars of all classes,
and eituatad in all parte of the sidereal world, are equally
mobile ? Kaptejn and Newcomb agree that systematic
differoBcea are unapparent ; but line-of-sight measures fumitih
evidence of a more direct kind than that examined by them.
Now, in classifying the radial velocitiea of the 280 Btara
employed in detennining the solar translation, Profeaeor
Campbell found their rate to increase notably with faintnesB,^
Within the acope of his investigation, the result was assured ;
but its scope was restricted. Individual peculiarities of the
etara embraced by it may have been concerned. This requiraH a
word of explanation. Measra, Frost and Adams have gathered
strong indicationSj from their work with the Bruce spectrograph
on the 40-incb Yerkes refractor, that helium stars really travel
in space more slowly than other atara.^ Hence, if objects of
this kind were represented more largely among the bright,
than among the fainter atars on Professor Campbell's list, the
discrepancies in their ratea of movement would be accounted
for. That their true explanation must be sought in some
such apecial circumstance rather than in any systematic
diversity, is practically certified by exhaustive statistical
inquiriea, and more particularly by Professor Comstock's
study of a collection of atara ranging from the ninth to the
twelfth magnitude.* Their average linear velocity, estimated
by Kapteyu's unexoeptionable mefchoil, agreed almost precisely
with that of CampbeH's stars, notwithstanding their photo-
metric inferiority to them, in the mean, by no less than six
magnitudes. Summing up, then, it appears that atars of the
same spectral type, wherever situated, possees, in a general
way, similar movements ; but that helium stars are perhaps
genuinely slow in pace ; while Sirian stare seem more leisurely
travellers than solar, merely because they show equally bright
at a much greater distance.
Yet the preponderance of small stars in every enumeration
^ AtiToph. Joum. vol, xiii p. 85.
* Ibid. ToL irii. p. 246 ; Deceit. PuW. toL ?iii. p. 100. ^
' AMtT, /own, Ko, 6&S.
322
THE ST81X1C OF TfiS SUJtS
«f npid pflopor matiam m a cbaBsBng ^eu Its
cspla^iiioB ■ that the «veBif» of iMllBr ue
tritoo-fODi an few. Miaaiyw WBrnanmrn. BdmUj, iMiveM;
fchsr dfificiflDCT >• in liciift mthfr Uuii itt aMM&. A nsik
€f Um evidme g bouing on the point M cwllBrted in Table ?l
of oar Ajfptmdix, which gifva the nugaifTuiiw aad motkai «(
th« Ukiitf qvkkMt alan oC ov aeqvn&taaea. Move thaa ktt
sfe iaviaCble to th^ aaked eje ; tha four H«^^"tg the Ixi hiR
A mflHt *"*c"i*"^ of 7*3 ; no kai than fclercD XBDge fnm ^
«i^itfl to hdow the ninth, while oolj two stazB of the in^
n9n4 oC the aeooiMl mod one of the third magniiade are ss-
clttdfld in the oooqwctittL The largest proper mocum yH
detected bdoc^ to an 8'5 magnitade ataf ntoated io tkt
•oathem ooiiftellatioD Pictor. Its diacoTerj in 1897, in
which foptejTQ and IniuM co-opented,^ was one of the
frnita of lidereal knowledge plocked during the
of the Cape Photographic Dui^limuistenmg. It aupeneded?
the chaaipion raoer^ aod far outfitripa 1830 Crooinhndge, ■>
ijurigniiiuiint star in the Great Bear^ picked out b^ ArgeUudsr
in 1 842 for a rate of progress which would carry it in 185,000
ymn round tJie entire sphere, or in 265 over as much of it as
the fiUQ*8 diameter covers The corresponding aunual advaace
amounta to 7" ; a-nd it ia very nearly equalled by two etoaU
southern stars observed by Gould during bis stay at Coxdoba.
One is a 7' 2 magnitude star in the Southern Fish (Lacadle
9362), the other, one of 82 in the conatellation Sculptor.
Next on the roll comes 6 1 Cygni with a proper motion of 5**2 J
and a Centauri, with Z"'?, h&s eleventh placa Double stare
are Gr^uently conspicuous for rapid movement; and it is
noticeable that three out of the four tirst- magnitude Btare
with proper motions exceeding one second of arc yearly^ —
namely, Siriua, Procyon, and a Centauri — are binaries.
Struve's geuerul inference aa to the quicker translation of
multiple than of simple objectSj has received much support
fitim further experience.*
The " proper moUoua " of stars include, as was explained
in the la^t chapter, an apparent, as well as a real element ;
they consist, in technical phraseology, of the motus parai-
' Attr, Natfi. No. 8468 {Kipteyn) ; Observtiit>ry. vol. iiiL p, 99 (Gill}.
■ Oftvin J. Burns, AUrvph. /oifrrw. toI. iviL p. 67.
THE PROPEK MOTIONS OF THE STARS 323
iaeticus, optically transferred to the whole stellar multitude
from the single real motion of the suit, and the m^tus
peculiaris, belonging to each individual Btar. The Beparalion
of these two constituents, blended together on a cursory
inspection, is a necessity for progress. This is what Kapteyn's
mode of analysis aims at, and in a measure accomplishea
For the motion of a star in a direction petpendicalar to that
of the eun'a route is altogether its own ; it ia an objective
fact ; and the comprehensive study of such components of
stellar velocities, purified by a sort of " fractionation " from
parallactic ingredients, afiforda undoubtedly the most promising
means of gaining insight into the general plan of celestial
revolutions.
But the motvs pecidiaris itself ia only a projection apon
the sphere of a line of ti-avel which may make any angle with
the line of sight, Its amount then varies with direction no
less than with distance sxkd actual velocity. A star may
appear devoid of motion simply because the whole of it is
" end-on " ; while the movements of others seem large because,
lying square to the line of sight, they are completely effective
for apparent displacement. Here, just where ordinary obgerva-
tioD ia baffled, the prismatic method cornea to the rescue. The
spectroscope " takes up the runniog " for the telescope.
The alliance could not have been rendered effective but
for the momentous improvements effected late in the nine-
teentii century in the processes of celestial photography. The
prerogatives of the cumera in this line of work are euormoua
Not only do the worst mischiefs of atmospheric disturbance
vanish with its employment, but the upshot of measure-
ments executed upon one line can be cheeked or ratified
by comparisons with other lines in the same spectrum, and on
the same plate. Where motion is in question, all must be
equally affected by it; hence perfect security against illusion
is afforded. The full realisation of these advantages through
Vogel's skilful use of the spectrographic apparatus erected
by him at Potsdam in 1888^^ thus constituted an advance of
_fiisb-rate importance in practical stellar astronomy.
The example thus set haa been widely followed — in
T&jnerica, at the Cape, in Europe at Cambridge, Pulkowa, and
1 ManaUberieiitet BerLiQ, March Ifi, 188@, p. 367.
zu
THE STSTEM OF THS STAfiS
thtfter; hm
ttfloed, Mtd bAVtt beeD Adrerted to xa aa
tbcj anna mortif is ""■■■"^■'^ giabntie^aad
not w cActm ■• tbe applei of Atikate ID divertnig
from on wltimiitft goal B aoe miie B mto
an iwinrtiTTy of a iMaitiod cbttwter; Ukj &iMnd Ihsi
IUHljff of d^a^ itrwt tiUdOB w w M^ f titT^ zadial tneiocitieB nnt bs
mdend ix>inpanble in sbundancr to thaee mlremdj •ocamslited
of the projected moremeDte of tbe «Ui% b«ibce ooch reseudMS
Oia be proRQcuted virith entaro roccwa EvcataaDf, too, radial
velocity can be made to aerro «a a teat of mean pajmUax. It
tmy lairly be amimed that atan tx&Tal on && avenge with
eqiUl speed along each of the three otMndiiutis of caldcil
space. Comparing then the mean radial speed in miles per
Mcond of a given group of atani with their mean displace-
ments in aeoonds of arc along circles of declination or rigbl
aacetiAion, we at once learn their mean distance, since we thus
virtually tranaUte angol&r into linear displacements.^ It is
true (oA can be seen &om an inspectioQ of Table TIL in onr
Appendix) that much swifter rates of stellar transport have
been determined in a tangenti^ direction than in the line of
night ; but tbe ineqnsJity m&y be an accident of investigaUoQ
which its further progress will redress. Meanwhile, there is
much reasou to believe that no general disparity of the kind
subiiiAtfl, Kitimates of the average total velocity of tbe stars
in space were derived by Kapteyn and Kewcomb from their
observed proper motions, and by Campbell from their measured
ratM of upproacb nr recession. They agreed almost exactly.
With reference to a fictitious atationary centre of tbe stellar
asoumblage, a niedtutn star is displaced by 21 or 22 miles
a Bocond, V2^ miles being the rate of our sun. We are
accordingly borne along in the train of a somewhat sluggisb
lumiuiiry."
Table VIT., 2, gives a list of etara with thwartwise mov«>-
tnotita exoeediiig 25 miles a second, They are sometimes
ciiUi^d " runaways," because their headlong course seems hardly
compatible witli entire subjection to the sway of gravity.
The first of theee startling examples to become known
1 KluiW, Jsir. ^<K}t. No. 3037,
• Nowcomb, The Starts p, 3(M.
THE PEOPEE MOTIONS OF THE STAES 325
1830 Groombridg«> The large proper motion and email
a.llax of this Stat compel the ascription to it of a speed —
dng into account only that part of it lying square to oqr
iew, of at leaat 150 milea a second — a speed uncontrollable,
aeeording to Professor Kewcomb, by the combined attractive
power of the entire sidereal tuuverae. For hia calculations
show that the maximum velocity attainable by a body falling
from infinity towards and through a system composed of
100,000j000 orbe, each five times aa massive aa our sun, and
diBtributed over a disc-like space 30,000 light-years in ex-
tent, would be 25 milea a eeoond.* But 1830 Groombridge
poeeesges more than six times this speed ; and because velocity
varies with the square root of the attracting mass^ a world of
stars of fully thirty-aix fold the potency of that assumed as
probable woiUd be required to set this object moving as it
does unquestionably move !
Kow the velocity producible by an attractive syatem is the
limit of the velocity it can control — that is, bend into a closed
curve. It is then certain that unless the stellar system
possesses what we may call occult gravitational energies, the
star in questiou cannot be one of its permanent members.
Virtually in a straight line and without slackening, it will
pursue its coui'se right across the starry stratum it entered
ages ago on its unknown errand, and will quit ages hence to
be swallowed up in the dusky void beyond. There is, how-
ever, an alternative supposition. The star may be acted upon
by unknown compulsive influences.
Lord K^elvin has lately estimated the quantity of gravi-
tating matter needed to produce velocities such as the
generality of stars exhibit. He finds it to be that of a
thousand million suns like our own, evenly distributed
throughout a sphere wi th a radi ub of 3262 light - years,'
A prodigious lapse of time would further be needed for the
development, by continuous acceleration, of the observed
higher rates of speed ; nor can we be quite sure that even
these heroic measures would suffice to produce them. Yet
they are patent, and not extremely scarce. Groombridge
1830 is no longer the only "runaway" of our acquaintance-
* Pop, Asttanomy, p. 4ti9.
^ RtpoTt Brit, Aa. 1901, p. £63 ; Natwrt, vol hdv, p. 02«,
326 THE SYSTEM OF THE STABS
linear stellar speed, apart from that share of it directed
along the line of sight, exceeds Newcomb's computed maximum
of 25 miles a second in about one- third of the cases in which
it has been ascertained, and the excess is here and thete
very large. Arcturus, for instance, travels at the tremendoos
rate of 257 miles a second, /& Cassiopeiie at 113 ; while fire
southern stars progress by 60 to upwards of 80 miles per
second.
" Fljing stars " can then no longer be regarded as men
intruders into stellar society. Whether or not belonging to it
" for better for worse," they evidently at present form an im-
portant part of it, and the problem they present cannot be
excluded from a general consideration of sidereal mechanism.
Indeed they furnish a most significant index to the working
of its secret springs. They pursue their careers, so far as
observation can yet tell, in right lines, and at a uniform speed
Their high velocities would be otherwise less perplexing ; for
they might plausibly be attributed to the powerful attraction
of invisible bodies in their neighbourhood, representing, by
analogy, tlie rush past the sun of highly eccentric comet&
But the evidence is wholly against any such hj'pothesis. All
pro}>er motions known to us — whether of single stars or
of the centres of gravity of multiple stars — are sensibly
rectilinear. The centres of curvature, presumably, of the
imaginary lines traced out by them, are inconceivably remote.
A straight line is only part of the circumference of a cirtle
of infinite radius.
The fact accordingly confronts us that not a few of the stars
possess velocities transcending the power of government of the
visible sidereal system. Is that system, then, threatened with
dissolution, or must we suppose the chief part of its attractive
energy to reside in bodies unseen, because destitute of the
faculty of luminous radiation ? The presence of many such
bodies is unquestionable ; and those of which we take in-
ferential cognisance may be few compared to the multitude
wholly beyond our ken. The power of the univei'se is certainly
reinforced by the dark stars it includes ; but to what extent is
unknown ; and the uncertainty helps to maintain inviolate
the final secrets of our cosmical environment.
Physical peculiarities are not, in any obvious way, related
THE PROPEB MOTIOJfS OF THE STAKS 327
excessively rapid movemeiits. Arctiiraa ifi a solar star,
sowing promineut titanium-absorption, and apparently well-
ivanced towards the Antarian stage. Its masa is presumably
enormous, since its light-power must be equivalent to that of
Cwelve to thirteen hundred suns! Its nearest competitors in
swiftness, 1830 Groombridge and ^ CassiopeijE, are, on the
other hand, comparatively unpretending orba ; and neither
differs markedly in spectral quality fi-om our aan. Indeed,
the eolar type appears to be more often asaociated with Iiigh
velocities than any other. Stars with banded and gaseous
spectra, and variables of all elates mostly exhibit bub slight
signs of displacement ; but this ta^y be aji effect of remote-
ness, rather than of genuine inertness.
An unmistakable connection, however, exists between
proper motion and sidereal locality. The late Mr. Proctor
drew attention to the prevalence in certain regions of the sky
of what he termed " etar-drift/' ^ Here and there, unanimity
is, to some extent, substituted for tlie caprice superficially
characteristic of the " peculiar " movements of the Btar&
Amid seeming confusion, order and purpose by glimpses
reveal themselves. Battalions of stars — ■" flying synods of
worlds " — regardless, as it were, of the erratic flittings of the
casual surrounding crowd, iDarch in widely extended ranks, by
a concerted plan along a prescribed track, under orders sealed
perhaps for ever to human intelligence.
Among the stars situated between Aldebaiftn and the
Pleiades, there is little relative movement. They all drift in
company towards the east, by about 10" to 20" in a century.
Not, it is true, along strictly parallel lines. A fresh investiga-
tion by M. Weersma* of 66 members of the Hyadea group has
brought to view considerable divergences. Dr. Downing's dis-
ouaalon/ too, intimates very clearly the division of the main
cluster into subordinate families, travelling to some e^teut on
their own initiative. The general tendency of their course is
no doubt largely due to the sun's oppositely directed progress.
Five of the " Seven Stars" (sepicwt triones) forming the
Plough (those excluded being the " Pointer " next the pole,
' Froc. RoU' Society^ roU XTJii. p. 109.
* OrfmiTigen Publications, No. 13, 11iK)4>
* JoMrw^ Srit. Attr. Am. toI, xr. p. 2S.
323
THE SYSTEM OF THE STABS
aud 7} at the extremity of the handle), wct& regarded by Ul
Proctor m members of a vast united group ftdvancing witlt,
though outpacing the sun. This remarkable inferanoe hw
been endorsed by ProfeaBor Newcomb ; * and the reality d
the visible flow of movement was substantiated by specoo-
graphic evidence obtained at Potadam, showijog that the fltaiS
in {jueetiDn are approaching the earth with a common veloeLiy
of about 18 miles a aeconi* The system they form has been
roughly estimated by Dr. Hoffler * to bo eitn&ted &t & distance
of 200 Ught-yeara, whence it followa that each must greatly
exceed our sun in ladiative splendour. One of these linked
orbe^ moreover, carries with it, as our readers are aware, three
dependent atars, namely, the Eider- star Alcor* a slowly re-
volviog telescopic attendant, and a more intimate associate
apectroecopically revealed.
It ia scarcely likely that the combination is self-
centred. Concordant motion does not necessarily imply the
mutual revolution of the objects to which it belongs. What
it does imply is their dynamical connection. But that
connection need not be of the kind exemplifed cloee at
hand by the earth and moon. It may rather be such as
prevails between the earth and Venus, or between Jupiter
and Saturn. The group in Ursa Major, it is safe to aaeert,
includes examples of both kinds of relationship, Of the
movementfl of two satellites, Mizar (if Ursfe) is the un-
doubted mainsprmg. The statue of AJcor is dubious. Its
path at present appears strictly rectilinear; but latent curva-
ture relative to the large adjacent star may in time become
sensibla About the personal independence, however, of all
the rest of the company there can be no questioD. Although
dominated by the same influence, they advance each on its own
account ; nor can their relative situations be looked upon as
beyond the reach of change. Ultimately, the bond of union
between them will perhaps even cease to be traceable. Slight
ine<iualiti©B betraying differences in the period of revolution
round the same remote centre may eaaily co-exist with what
is known as common proper motion. Such discrepancies can
alone hold the stars affected by them aloof from binary com-
1 Th* Star$, p. 80.
* H. C. Vagal, P^lietUiown, Bd. rii Th. L p. 164.
» Aatr, Naeh, No. 34B6.
THE PEOPER MOTIONS OF THE STARS 329
binatioD. Whila travelling along parallel lines, they have
BtiU a relative velocity exceeding^ at their distance apart^ the
power of their mutual gravitation to Bway into an ellipse.
One must hence fall very slowly behind the other, as Saturn
falls behind Jupiter after conjunction. Evidence of their
afi&nity ia then only temporarily acceaaible to ua. After
many ages it will evade recognition. There may be,
probably are, in distant parts of the sky, stars revolving in
boundle&aly spacious orbits round the same focus of attraction
with the stars of the Plough ; bat we have no means of
identifying them.
" Partial systems," governed presumably from without, are
of tolerably frequent occurreoce. The first to become known
was discovered by Bessel in 1818.' It is composed of a fifth
and a seventh magnitude star, known respectively as 36 A
Ophiuchi and 30 Scorpii, thirteen minutes of arc apart, yet
endowed with an accordant movement of l"-25 yearly. The
former star has a close attendant ; and an intermediate minute
object also forms part of the company.^ Another interesting
quadruple group was detected by Flammarion in IS??." Two
couples in the Swan, one revolving^ the other in appearance
fixed, separated by an interval of 15', drift together slowly
Bouthward in a direction nearly perpendicular to the Una of
march of the sun. Their movement is hence " proper " to
themselves, perspective effects being unconcerned with it.
The stationary pair is the fifth -magnitude yellow star, 17
Cygnij with its bluish satellite at 26"; the circulating pnir
consists of two eighth-magnitude stars at 3'', numbered 2676
in Struve'a great Catalogue.
A curious instance of concerted movement is afforded by
two ninth-magnitude stars in Libra, discovered by Schonfeld
in 1881 to progress across the sphere at the exceptionally
quick rate of 3"*7 annually.* Notwithstanding the wide
interval (6') separating them, their advance seems perfectly
harmoniouBL They flit side by side, as if rigidly connected
across a chasm probably some thousands of millions of miles
^ Fiittdamentit Astf<»wmia, p. 811.
^ Flannnanon, C^mptcM Bendw, t Ixxxr. p. 783 j Cat, dit ttsikt Do^Ma^
p. 106 ; luiies, Rt/ertnci Cat. p. 170 A,
' Comptea Htmdm, t lixiv. jj, BIO.
* SiUun0sb«richte Niederrhtiniicht Ot$. Bonn. 18S1, p. 173.
8S0
THB STSTEIC OF THE STABS
jo width. A sttU wider sjrstaii* noted by lit. Ibih^
falPMl bj two stAT-pain m Toiicazi.' la neither cMe
mauHree for parallax jet been executed.
To the queetioii^ — Ha» the van anj osBOciate in his ,
through space? only a prorisonal answer can be
lXtfo6 are known, bat inreetigHtioDS on the point are lanlj
tiAnent. The pecoliaritieB which we should expect befarebAud
to attend such campamon-stars^ are comparative proxiouij
Md l«latiT« immobililTf. They should hare sensible paraflawi
and be deroid both of radial and tangential velocity. Xeitlur
apectroaoopie nor telescopic eridenoe of motion should Iib
derivable from tbem. No star up to thia thoroughly ^^awiinM
combines thef>« characters -, but tben they could not pom^j
be found in the " proper motion '* stars chosen by prefsrenoe
00 the Gubjects of parallactic obs^rvationfl. Only in one of
the Btellar points employed for comparison with 61 Cygni h^
their presenoe been suspected. Dr. iSchur measured^ in 1899,
what seemed like a parallactic «hift of this nameless star tfi
the extent of 0"'6 j* and Mr. Grorameliu* having deduced far
it an evanescent proper motion, threw out the suggestion that
it might belong to the sun's bodyguard.* The possibility,
however, depended upon the verification of the parallax* which
ifl not known to have been effected. When mora has been
done io photographically registering Une-of-sight movements,
Btars may perhaps be discovered sensibly fixed as regards the
aun, because borne along with him at the same tr&nslatoiy
speed The construction of Buch a group, and the diBtinctive
charactorisdtiou of its members, might open up a fascinating
branch of inquiry. But its methods cannot well be eatabl iabed
until its subject-matter is rendered less evasive.
If the system formed by the stars be destined to
nenoe in its present shape, some general law of movement
must be obeyed by them. Even if its state be one of pro-
gressive modificatioHj a definite mode of change ought to
become apparent. Local irregularities, however, so effectnally
di^^se the fundamental harmony that its prevalence may long
continue a matter of speculative belief.
The assumption is indeed indispensable^ as Dr Schonfeld_
1 Se» mU4, p. 97. ^ Aatr. Naek Ko. 36ftO,
■ Obtervatory, voL riii. p^ S76.
ibli^e^i
THE PEOPEE MOTIONS OF THE STARS 331
minted out in 1883,^ that the motions of the etars are some-
related to the plane in which the vast majority of them
are diepoaecL For otherwise their actual conhgurfttiou would
be a wildly improbable accident of the time in which we liTe.
The Milky Way, to put it otherwise, should he regarded as an
evanescent phtiiiomenon, unsufltained by any persistently
acting forces, the outcome of a hundred millions of casual
conjunctions. If this be jucredible (as it surely is) then we
are constrained to admit a preference^ in the long run, among
stellar displacements for the grand level of stellar aggregation.
The Milky Way must be, in some true sense, what Lambert
called it one and a half centuries ago — the " ecliptic of the
star^/'
Sir John Herschel imagined the law of harmony to consist
in a general parallelism of stellar motions, involving a kind
of systematic circulation, as of a solid body round an axis per-
pendicular to the galactic plane. Innumerable exceptions to
any such rule are of course to be found, but they were
assumed, in the upshot, to be mutually destructive, the main
•* stream of tendency " 6owing on irrespectively of them. But
it ie difiScult to conceive a physical basig for a quasi-rotational
system wholly without warrant from experience. More
plausible 18 M, Ludwtg Struve'a view that the main part of
the revolutions of the stars round theii* common centre of
gravity situated in the Milky Way, are performed in planes
slightly inclined to that of the zone towards which they are
concentrated.^ His attempt, indeed, to elicit a "rotation-
component" from the secular movements of Bradley's stars,
proved unavailing. Yet this is not decisive against the truth
of au hypothesis compatible with a btilanced stellar circulation
pursued in opposite senaes. An apparent drifting movement,
detected by Sir David GUI in 1902.^ of the brighter stars
witliin a southern zone 12^ wide relatively to their fainter
associates, involves considerations of a different kind. It haa
yet to be substantiated. Every imaginable precaution was
indeed taken against insidious errors ; yet such a phenomenon,
if genuine, should almost necessarily be universal; and Pro-
» V. J. S. Aair. G«s, Jiihrg. xvii, p. 2B&.
* Mtmaires d« Si. FHirabotiTg, t. xxxt. No. 3, pp. C, 19.
» Attr. Nach. No. S9i>0.
332
THE SYSTEM OF THE STABS
feseor Turner^ failed to derive from the Oxford zone-plates
convincing evidence of iba extension to northern gtars,
M. Bancken dealt in 18S3 with a strictly selected list of
stars.' He admitted only those within thirty d^reefi on
either side of the Milky Way^ and possesaed of annu&l proper
motions not exceeding a quarter of a second. The solution of
his eqtiationa showed these movements to include a common
element of very alow progressive increase of galactic longitude
That is to say, the 106 stars considered were being graduallj
swept along the Milky Way in the direction from Aquila up-
ward towardiB Cygnus and Ca^iopeia, and down past Opella
through the Club of Orion towards the Ship. The reality aod
extent of this flow of displacement will be a matter for future
investigation. Should the one be confirmed^ and the other aacer-
taiued, something like a clae to the labyrinth of stellar mo vements
will have been provided. Perhaps the restricted nature of the
inquiry contributed to its success. For the exclujsion of large
proper motions was the most effective mode of aiftiug oat
stars of the solar type, to which they in the main belong.
And since this class of bodies are not perceptibly condensed
towards the Milky "Wiij, they are unlikely to obey any law of
subordination to it in their revolutions. In this line of
research, accordingly ^ as in most others connected with sidereal
structure, the discrimination of spectral types is prescribed
nnder penalty of hopelessly confusing the issue.
' JforttWy Koticf:^, Tola. Lriii p. 66, Ixiv, p, 3,
' Jgtr. Nadi, No. 24831,
CHAPTER XXV
THE MILKY WAY
The Milky Way showa to the naked eye as a vast, zone-
ehaped nebula; but is resolved, with very slight optical
assistance, into innumerable small stars. Its stellar con-
stitution, already conjectured by Democritus, was one of
Galileo's earliest telescopic discoveries. The general course
of the formation, however, can only be traced through the
perception of its cloudy effect ; and thia is impaired by the
appLcatiou even of an opera - glass. Eendered the more
arduous by thie very circumfltanoe, its detailed study demands
exceptional eyesight improved by assiduous practice in catching
fine gradations of light Our situation, too, close to the
galactic plane is the most dieadvuntageoua possible for pnr-
p<jses of survey. Groups behind groups, systems upon
eystems, streams^ sheets, lines, knots of stars, indefinitely far
apart in Bpace, may all be projected without diBtinction upon
the same sky -ground. TJnawarea, our visual ray sounds end-
less depths, and brings back only simultaneous information
about the successive objects met with. We are thus presented
with a flat picture totally devoid of perspective- indications.
Only by a long series of inductions (if at all} can we hope to
arrange the features of the landscape according to their proper
relations.
To the uncritical imagination ^ the Milky Way represents a
sort of glorified track through the skies —
A brand tmd ample rood, whoee dust it gp>\d
And pavement stara, oa ston to tbec appear,
Been in the ^bxy, tbat milky way,
Which nightly aa a circhng zone thou eeest,
Powdered with stare.
333
334
THE SYSTEM OF THE STABS
Id Aineric*!!- Indian fftnoy a mystenons " pAth of aavh,"
ito popular Oerman n^tcae, "die JakobsstiBflB^" raealh tk
Cime when it stood as & celeetial figure of the wm; cf
pUgtimage to CompoeteUA. Siimlarly. in medifleral ICwgWmi
it got the title of " WftTfflnghAin W^y ** \jj asBOcdAtion with
Our Uidy s Norfolk sanctuaiy ; while the Dutch dftHkatwl it
to St Hilda, and the Finns aet it ap&rt for tha fiittog
procasaiotiB of birds. More anciently, in the ocder ol
ideas iuitiated hy the Accadians, it represented ibe mystic
Snake-riyer of the abyss ' — the Homeric Ocean-stnAin navi-
gated by Odysseus in his voyage to HadeSu Superficial
iinprossionfi of homogeneity are. however, replaced, on closer
inspection, by an aspect resembling rather that of a mgged
trunk marked by strange cavities and excreaceDces, and sending
out bmnchea in all directiona.
The medial line of the Galaxy is scarcely distingnl^iable
from a great circle* although Professor Jfewcomb's later
invefltigationa indicate for it a southward displacement of
nearly two degrees.' This would imply our position to be
somewhat north of the main level towards Coma Berenices;
but whether it i& central or eccentric there ie nothing to show
decisively. Tlie movements of the earth bear uo obvious rela-
tion to the etarry coUixstion around it. Jfeither the equator nor
the ecliptic manifeats any trace of conformity to its plane. Tlj^
great circle of the Galaxy is inclined about sixty-three degilj^H
to the celestial equator, which it intersects in the contst^Ia-
tions Monoceros and Aquita. It passes in Cassiopeia witliitt
twen^-seven degrees of the north pole of the heavens, in
Crux, as near to the south pole, while its own poles are
located respectively iu Coma Berenices* and Cetus. Over
two-thirds of the celestial circuit, the general tinity of this
stupendous structure is preeerved. Broken, however, near
a Centaun by the interposition of a great fissure, it is only
regained, after an interval of some 120% through the re-
onion, in the neighbourhood of e Cygnij of the separated
portions. Involuntarily, the image presents itself of a great
' iL Q, Allen, Star Sanies and thfir Mranimgs, pp. 37i-79<
* Gould, (Tranometria Arffentinaf p, 370.
' AVfiCuw, ToL lix. p. 308.
* B.A. lib 44» Dec. +2fl' 48' (Kewcomb).
THE MILKY WAT
335
river, forced into a double channel by an encounter with a
powerful obstacle, the removal of which lower down permits
its waters to flow together again. The intervening long strip
of islanded rock and gravel might stand for the great rift
between the branqhcB of the sidereal stratum, which, although
to the eye, owing to the effect of contrast with the " candid
way " on either side, darker than the general aky, is in reality
nowhere quite free from nebulous gUmtneringa. It ia en-
croached upon by fringes, effusions, and filaments, spanned by
bridges of light, and here and there it is half filled up by
long, narrow, disconnected maaeea, or luminous pools, lying
parallel to the general flow of the stream. One such
" brilliant and tortuous streak '' ^ extends, in almost complete
isolation, over nearly 20'', from the tail of Serpens across a
corner of the Shield of Sobieski. Moreover^ only the more
easterly of the two principal branches — that traversing AquLla
and the bow of Sagittarius — is continuous. The other, after
covering part of Scorpio " with a complicated system of inter-
lajced streaks and masses," ^ dies out in Ophiuchus, about
fifteen degrees south-west of the termination, just at the
equator, of the arm sent out to meet it through Cygnus. The
gap is, nevertlielese, partially veiled by a faint luminous
extension from the souths and shows as absolute only over
some five degrees of the sphere.
This ia not the sole interruption to the course of the
Milky Way. Another, visually, though not photographically
apparent,^ cuts sheer across the imdivided stream in Argo.
Here, at south declination 33°, the formation^ Sir John
Herschel says, "opens out into a wide, fan -like expanse,
nearly 20° in breadth^ formed of interlacing branches, all
which terminate abruptly in a line drawn nearly through X
and 7 Aig^H,"* On the opposite, or eastern side of a
moderately broad blank space, a similar assemblage of branches
converges upon the variable star rj Cariase. There is an
obvious correlation of structure on either aide of the chasm ;
subdivisions mutually correspond ; the broken series on one
margin is resumed on the other. The impression is strongly
'i VrwL. ArffoU. p. S81. * Hersohel, Ovitijua, art. 780.
■ a. C. RuBBeU, Monthly NoUces, vol. IL p. 498.
* Outlimi, art. 787.
336 THE SYSTEM OF THK STAltS
conveyed that star-strata oucd united, have here jieUed
to the influeboe of some imknowti dis|)etsive force or foroofi,
peiliApB etiU ID operation. Vet we can acarcelj' hope evet
to omuoand the meaua of testing the conjecture. For the
Iffoper motioQA of the faint telescopic stais near the edges of
the gap^ aro do doubt of auch exceaaiTe minuteneee tbat
oentariea, nay, uiilleummua may pass before they can became
perceptible.
The repTesentJttiOQ of the Milky Way aa a imiform atony
afcream is purely eoDTODtioDol, Its real texture ia of a curdled
or flaky description.' Between PerseuB and Sagittariiia» Sir
William HerHchel counted eighteen luminous patches, *' re-
sembling the telescopic appearunce of largi^, easily teaolred
nebula" ;* and hi» eon perceived the lucid ramifications in
Sagittarius to bo made up of " great cirrous maaaoa and
streaks," the appearance, as his telescope moved, being "that
of clouds passing in a scud, aa the aailora call it/' Furthei
on, he remarks : " tho Milky Way is hkt) sa^d, not strewed
evenly as with a sieve, but as if flung down by handfuls (and
both hands at once), leaving dark intervals, and all consistii^
of 14tb, 16th, and 20th magnitudea,^ down to nebuloaity, in a
most astonishing manner/**
The bright spao^ of the galactic zone are commonly sur-
rounded and set off by dark winding channels, and the rapid
alternation of amazingly rich with poor, or almost vacant
patches of sky, is a constantly recurring phenomenon.*
associated by Mr. Maunder*^ with slow processes of stellar
agglomeration. The most remarkable instance occura in the
Southern Cross, the brilliant gems of which emblazon a
broad galactic mass very singularly interrupted by a pear-
shaped black opening eight dt^greea long by five wide, named
by early navigators the " Coal-sack." This yawning excava-
tion figures in Australian folk-lore as the embodiment of evil
in the shape of an Emu, who lies in wait at the foot of a tree
1 EouEwu, Uranom^rii OiniraUt p. Iff, 1ST8 ; Kloin, WocKtMehrifl /Or
A»tr. 1867. p. 2B8.
* FMl. Tratu. vol civ, p. 262.
* Herschel'^ "20tli magnitude" QorrMponcU (pproxinuitelj with the Htb
OQ the pliototii«tric £c«>Ie.
* Cope ObafTvaiion*. p, 388. " HerBohol, Outtiiut, uts. 7W, 7ft7.
' Knoicledffe, tqI, xviii. p. ^6.
^
THE MILKY WAY
337
ipteaenteci by th& atara of the Cross, for an opossum drivea
his peTsecntioDS to take refuge among its branches.^ The
igend reads almost like a Cbriatian parable. The denudation
the Coal-8ack is, however, shown bj Mr, H, C. Russell's
otographs to be complete only towards its northera end*
o the south, a considerable invasion of small stars modi£ea
e contrasting darkness.
Partial galactic vacuities, evidently of the same nature
'th the southern Coal- sack, occur elsewhere, notably in
lygnus; but they are inconspicuous to casual observers. A
larkable doubly perforated star-cloud la exhibited in
late XIX. from a photograph taken by Profe&sor Barnard
in 1892. It makes part of the vivid scenery of the MiUcy
Way in Sagittarius.
An admirable deliueation of the formation, ao far as it
ia visible in the northern hemisphere, was completed at
PaTBonetown in 1889 by Dr. Otto Boeddicker, after five years of
labour, amid climatic conditions of the lenst propitious sort.
The general effiect may be best described ag that of a thick
stem of light, closely set with curvilinear ramifications ; the
stem itself being riddled with dusky convolutions, intricate
panares, and '^ hoise-ehoe " or " key-hole " apertures, separated
by lustrooa wisps and nebulous " pointed arches." The
circumstance that " feelers are thrown out towards nebulEB
and clusters,^ is of profound interest. Thus a feeble branch
starting from a Casaiopeise terminutea at the Andromeda
nebula. The Pleiades stand at the peaked summit of a
dim vault springing, on one side, from near p Tauri, on the
other, from e AurigiE, The Hyadea are separately involved ;
Prsesepe is all but reached by a long streamer iasiting from the
vicinity of ^ Cauis Minoria ; while a thin sinuoua eifuaiou,
perhaps of a spiral nature, includes the great nebula in itft
sweep through Orion. The subject was next prosecuted by
M. Easton of Kotterdam. His galactic charts * are of high
authority; and, following up the initiatory efforts of M,
Houzeau, he has lately studied, with instructive results, the
I intimate structure and sidereal relatione of the great zone by
^1 * Mml
■ MorUht^ A^oiKn, toI. li. p. 40. " Ibid, vol 1. }i. 12.
« La Voie LaeUe, Farv, 189S,
338 THE SYSTEM OF THE 3TAES
means of " isophotal curves" ' or coDtour-UneB of lonunostx
YiGual recorcU, however^ of bardj pensepUble deUOa ounot
be entirely satisfiictoiy, their agreement being impaired )tj
iadividual diversities both of purpose* and of faeoltf; lod
they have been lar^ty, though not wholly Btiperaedod, hj tbe
pn>mptly-8e«ured impreasions of the impartial and iHHtiiiBUr'
sensitive pUte.
The Milky Way Tanes greatly in latctral asctflol A
brilliant stream no more than three or four d^fraM vide
where it enters the Ciobb, it expands to AUlj twonty-twu
degrees in tbe bifureated section stretching from Ophitu^us
to AquiR At some apota, too, the nebulous effect Ui the eyr
fadea away imperceptibly along tbe margins ; * at othflrs. Uje
line erf demarcation is so sharp that a telescope may have aDe-
half of its field crowded with galactic stars, while the other
half is welt-uigb blank.' A de&nite semi -circular bounduji
for instance, liiaits the formation near 2^ Aquila? ; its aoatfaen
edge in Ophiuchxus was remarked by Sir John Herscbd, v
" terminated by an irregular nebulous fringe aa if lacerated " ; *
and marginal projectiomi, knobs, and briBtling outliers azv easitj
perceptible elsewhere. The prevalent rule aeems to be (bftt
the smaller the gtars considered, the more abrupt ia the
commencement of the Milky Way ; while a mote and mort
gradual condensatiou aooompaniee each step upward in
brightness.*
Sir William Herschel waa perfectly satisfied Chat, with
his 20-foot reflector (equivalent to a modem reiiactor about
14 inches in aperture), the Milky Way was, in general,
" fathomable." The stars composing it, that is to say, wct?
of definite numbers, and appeared projected upon a perfectly
block sky. But this was not so everywhere ; certain jmuU
completely baffled the penetrative faculty of his instrument
One such was met with in Cepheus, where he found the eooall
stars to become "gradually leas till they escape the eye, so
that appearances here favour the idea of a succeedingj more
' La Dittribuiian tU la Lumiire GaltKtiqut^ AlQsUcduSj 1903.
' Rid. p. 7*
' W, Horwhd. Phil. Tran$. vol. civ. jx 283.
* Proctor, UnivtTM of Start, p. 86.
* Klflid, Wodtenaehri/t, U67, p. 2S6 ; J, Hefichel. CojH SttuUt, p. 88».
* Celoria, Memorie del M. J^iituio LfmibardOt t xit. pi e37>
^^^^^^^^^^^^^^^^^^^^^^^^^f XIX.
1
*
1 ■>^--^'^j:.>yy^^yvv,;.;,i;^-,.^-.-^:v^
1 ..:: r- ■'■■.■■ ■ -..-.-
1
Bv^'^^" '- '■■--■^ , .; .V.--.: .:. ..,' ..i. -■'.■■■;, -■■
^H Perfonitwl Oatactic Gi-oup in Sagittarius.' Photo({ra|^^led by K. K. IlmuonJ,
J
THE MILKY WAY
KS»
,nt clustering part." And he remarked, in exploring
^^*^tween Sagitta and Aquilaj that " the end of the stratum
^^^nnot bf Been." * Again, in the galactic branch traversing
*<^^phiuchua. Sir John Herschel encountered " lai^e milky
bulous iiTegulai patchea and banks, with few stars of visible
^toagnitudea " ; he described " a very laige epace " of the
^Kt jlky Way in Sagittarius as " completely nebulous like the
diffused nebulosity of the Magelliinic Cloud " ; ^ and observed
^ similar spot in Scorpio, " where, through the hollows and
deep recesses of its complicated structure, we behold what has
a.U the appearance of a wide and indefinitely prolonged area
strewed over with diecontinaous masses aad clouds of stars
which the telescope at length refuses to analyse." *
Even with the best telescopes of recent construction, this
perplexing and indeterminate aspect cannot be altogether got
rid of. Professor Holden could obtain with the 36 -inch
Lick achromatic directed to the Milky Way " no final resolu-
tion of its finOT parts into stats. There is always the back-
V ground of unresolved nebulosity on which hundreds and
thousands of stars are studded^ — each a bright, sharp, separate
point"* The lingering nebulosity was strongly indicated to
be of stellar nature, but whether it was due to the presence of
inniimerable small stars mixed up in the same region with
larger ones, or to the indefinite extension into outer space of
galactic agglomerations could not be pronounced off-hand.
The explanations attempted of these complicated pheno-
mena may be divided into disc- theories, ring -theories, and
spiral -theories. The " disc - theory " of the Milky Way was
first propoimded by Thomas Wright of Durham in 1750.
He supposed all the stars to be distributed in a comparatively
fihallovv layer, producing iin annular effect by its enormous
lateral spread. Irregularities, he thought, were partly due to
our eccentric position within the stratum, partly to " the
diversity of motion that may naturally he conceived amongst
the stars themselves, which may, here and there, in difierent
parts of the heavens, occasion a cloudy knot of stars." *
' PhiL 2'rajLs. 7ol. evil. p. 328,
- Capt Obaervalwns, p. 389. ' OuUinet of Aatr, vt 78B.
* AW. Mtst. August 1S8S, jr. 2&S.
* An Original Theory of the Univem, p. 03.
THB nvnU OF TBS SiABS
m
To that view Mr Williua HendKl |
mMilji by the ■ypHertMa
MdHd of " itg-ff^w"
wntHitMiwwy WNiM wnb lua gnM
iflCtha Ay,fcarfiiiwii t^tlfc»p
«poD tte Awtta of tibe gn^
lb* Mflkjr yfmj. In ita ncig^ibovbooa, «
mw%f InxB U, Umj «w» w ymadf ^iMnbolad Aad tldi faf i
ngtdu yro^nmknct 6Batitf tnm tfca 0UK*ic polv to tbt
gBLM^tic ee^uator, tb« UUer regioa Wag oo an avaage thmj
tiiBflB riebar than tbt fotiMK. Ka«r, if wm «cn to admil. m
Haidid did, a nenlT- eqaable acstteriiig ol ^ns in apMee. tJun
woflld bt ao altemalive bat lo soppoae tbe adareal ajitfiat ex-
lendad io otij direction proportiooately u> the comber of itm
attn io thai diroctioiL Their crowdiiig Bfaoold^Mk Ukmi hypUkmt,
be purely optical — the eSbct of the iniipfinita x^wesding out
in tho line of ligbt of their erenlj aemed raoka. Soondiji^
the itar-d«pthfl upon tht« principle, Herwihd meaBnred tfas
IflDgth of hiM line bj^ their Hceming popnlpa^aeae;, and OOB-
•truotod, ftvm tbo PUmericaJ data tbos obtained^ the " dorvB
diao " iDode]> bog aQoept«d «a repTeMtntlQg tbe croe fona of
Ibti BtolUr unirtirae.
But hiii own obnervattOQa at the vety moment of enoimciiig
thifl theory, fiitdlly undermined it. Already^ in 1735, be
romnrkfxl thut twrj or thrce hundred ^' beginnings or gaihefing
chiHtem," might t>e pointed out in the galactic aystem, and be
sunuiiKNJ iu cveutnul sopiirtttion, " after numbers of ages," into
no nmny diHtinut '• nebuk;."* " Equable scattering" then, was
nn iili^al Htatis of things long since abolished by th@ " ra^v&gea
of tiniu." The couvit;tion that euch was the case grew with
hie experienoe. " The immense starry aggregation " of the
MilVy Way, hn wrote in 1802^ " ia by no means uniform.
Th*i HtarH nf wliii;]i it ih (lompoBfid are very unequally scattered,
and (thow ovidont marks of clustering together into many
Mparato allotinoutH." Nor did he fail to perceive, from the
^adiml iucroaMe of brightneaa towards the ceuLrea of the^e
" allotmoutM/' thut they tended to assume a spherical form,
and thuB auggested " the breuking-up of the Milky "Waj, in
all it» minuto partH, aa the unuvoidable conaeqiaence of the^
^ PKil, TVvM. vol. Uxv. p. 20&. * Ibid, vol xcil
THE MILKY WAY
341
lostering power arialug out of those prepondorating attractions
rhich have been shown to be everywhere existing in its com-
I." ^ The formal announcement o£ his conviction " that
le Milky Way itself consists of stars very (litferently scjittered
those which are immediately about us," * amounted to a
antation of the principle of atar-j^uging.
With it disappeared from Herachel'e mind the conception
an optically -produced galaxy, In his ultimate opinion the
tual corresponded very closely with the apparent structure :
was composed, that is to say, mainly, if not wholly, of real
louda of stars. Credit was thus restored to the early im-
pression of Galileo, who in 1610 described the Milky Way
" nothing else but a mass of innumerable stars planted
aether in clusters," ''
Wilhelm Struve's* effort towards the reorganisation of
ie stratum-theory, though aided hy all the resources of hie
great ability and address, could scarcely be counted as a step
in advance Substituting for the hypothesis of equable dis-
tribution that of concentration in parallel planes^ he imagined
the avenge interval of space between the stars to dimixush
regularly with approach to the central horizon of the system.
The swarming aspect of the MUky Way was hence interpreted
as agreeing with factj but the annular appearance as being
illusory. Of illimitable dimensionB, the system was conceived
to stretch away, still preserving its specific character, to an
infinite, or at least unimaginable remoteness, comparatively
narrow visual bounds being set to it by a supposed extinction
of light.
But the quasi-geometrical regularity of Struve's galaxy is
belied by innumerable details of the original. The swell of
the tide of stars towards the j^lactic plane is neither uniformly
progressive,^ nor does it proceed without couspitiuous inter-
ruptions. Thus, the region near the horns of Taurus, although
close to the MUky Way, is absolutely the poorest in the
northern hemisphere ; * and it is matched in the southern ^ by
' FhiL Trant. vol. civ, p, 282, ' Ibid, vol. xcU, p, 480.
' iSVdtfnvJ Nuneius, ii^txs. by E. S. Cw\em, p. 4.2,
* Mudes d'Astronomii Stellairt, IS47.
* C. 8, Peirce^ Sarvard Annals^ vol, ix. p. 174^
' ArgciIaudeT, Simntr Stcb. R<1, v. Einkiiung ; Pto&tor, U-mwrst of Start,
p. 32, "^ Thomej Conkita Dur^mttstentngt IntroductiDii.
■fj l w — «
Sir JobB niHiihJ fay Ui G^» f^ffwifwrn,
Ui Mtaal idadMoe to diift &r cw»j fiw
tiM poiitioB origiatttf taliM up t^ ha teliec ne dMp
bgrUaiar tte |pk^ wm UmI of "« fiat mg,^
otlMria-wtfldig foia «f iwnaMB aad iniggmlglpiwM
•od UttdaMHL'" BfpawW inditfnitelx fllaog tl» oootal
]]>UiM, tike o«v Bodil mmfy diflbed ten the old exocfi ia
no for u Itie idtt of boakoipaooai oonotmction wm given iqk
T\m (Ii«c rom&iiied, bat with ita oeubre Kooped oqI The oolar
nyfltflm WM locatod ia on odotbuhis ^ao^ of relative Tucoi^.
The Milky Wajr, thtw reguxted* sppeafed to cMuist of an
indit^tiiVo nantber of atellar coUecttone "brought by projectioii
into Dearly the lame viaoal line" — to repreepot the fore-
ftborittied tfTect (movft especially at a pamcular spot in
HagiUariuA) of '* a vast and illimitable area scattered over with
diiK;rjtiLitiuauH nuiiioa and Jiggregatea of stars in the manner of
tho 4:LUiiiilt of a inadceral-sky/'' Bat in an aaaemblage of
thiit iiiitnro neon edgewieej a " Coal-sack " would be a pheno-
Tminoii fiH nnoimtlotm an in a uuiform stratum ; nor could it,
wilJifniL viuluiit improbability, be conceived of aa rent by the
«i»!iiHNal hvuituroH dividinj^ the actual Milky Way in Argo and
UphiucUiia.
t Frcnior, S\>c. eit> j*. in. * Outliiut, Art. ?BS.
> Cap* Obitrmiiiotu, p. 380.
THE MILKY WAY
343
To remedy these utconveniences. Professor Stephen Alex-
ader devised in 1852/ upon the model of the wheel-shaped
aebula in Virgo (M Q9), a spiral galaxy witli four curvilinear
aches diverging from a central cluster formed hy the aun
id lucid stars. By properly adjusting the mode of projection
these radiating star-streams, the effects of rifts and coal-
cks were duly produced ; but the arrangement, however
lired for ingenuity, gave no persuasion of reality, and
|uick]y dropped out of remembrance. E^entially diJTerent^
Ithough with some featuree in common, was that by which
Proctor replaced it in 1869.^ Rather than a " spiral "
adeed, the new desigu resembled a bent and broken ring,
lib long, riband-like ends, looped back on either aide of an
ening, accommodated to the shape of the gap in the visible
acture in Argo, One of these loops, by the apparent
intercrossing of its near with it& remoter branch, was sup-
posed to generate the Coal-aack in Crux; while the other
end, trailing lengthily backward^ afforded a deceptive effect
of bifurcation. Excessive distance was invoked, as in Profeeaor
Alexander's scheme, to explain the cessation of nebulous light
in Ophiuchua.
Of the manifold objections to which this hypothesis is
liable*^ only two need here be mentioned. In the first place,
it involves a wholly inadmissihle rationale of the openings seen
in the Milky Way. If these were due to the interlacing by
perspective of branches really far apart in space, the enclosing
luminous formation should be markedly fainter on one side
than on the other. But this is not eo. The borders of the
southern Coal-sack are approximately of the same brightness
all round. A single vivid moss has obviously been the scene
of what, in the absence of better knowledge, may be described
aiS an excavatoiy process.
Again, on the spiral theory, the ^at rift in the Milky
Way should represent the interval between branches mutually
disconnected except through the optical effect of projection.
But their mutual dependence is manifest. They strike apart
^ Aiir. Joum. vol. iL p. 101.
* Mimihljf NoiiceMj vol. xxx. p. 50,
* See Mr. J. tL Suttoa's retoarks, lUuttratid Siienei Mcnthi^, tdI. ii. pp.
63, 109 ; Knawled^St vol, xiv. p. 41 ; Eoetou, ibid, voL ixi. p. 13.
344
THE SYSTEM OF THE STABS
gradually', und aa the result of changing conditions. Pre-
monitory caritieg seem to Jinnounce their impending eepara-
tioQ ; and even after it haa become definitive, abortiTe efforts
towards reunion are indicated by the correspondence of oppo-
site projections and by the occasional bridging of the fissure.
The bifuication is beyond question a physical reality.
The prevalence of spiral forms among the nebulge, em-
phasised by Keeler's photographic explorations, adds weight to
the ai^uTxientfi for assigning a more or less similar structure to
the great firmmnental zone. M. Eoaton has illustrated tbe
"' a y--;^
»H,
-%,
^AA
-T>
-*-^
AS
\'
1
ajr^.
S^^
^^
no. n.^Tb« 6*Uctic Splrmt (Euton).
subject by a plan-sketch, copied in Fig, 3 7. It does not profess
to give " even an approximate representation of the Milky
Way, seen from a point in space situated on its axis/' ^ but
merely to indicate a possible mode of distribution of stellar
accumulations by which the observed phenomenon might be
produced. A remarkable bright patch of the Milky Way in
Cygnufl serves in it as the nucleus of the convolutions. The
sun's position, though central, is detached from them.
Some such design strongly tempts thought. It is recom-
mended by analogy ; it is recommended alBo by its adaptability.
A multitude of facta, at first sight incongruous, are combined
' Astroph, Joum. Toh xii. p. }&7,
THE MILKY WAY
345
by it into plausible unity. The ring-theory may be said
to have broken down when Celoria' found it necesaary to
establish a double annular eyetem. Hia researches, together
with thoae of Plasamann, Seeliger, and Easton, leave no
doubt that the Tarious sections of the stariy girdle differ
prodigiously in distance. Moreover^ it seenjB impossible eo
Ui place the bud in such an enclosing structure ae to
get a reasonable explanation of these diffeteucea without
having recourse to further complexities of artificial arrange'
ment. True, no deeign corresponding in any degrea with
what appeaig, caa be other than intricate. Were it permissible
to adopt the opinion that the Milky Way is very much what
it a^tmi, we should deecribe it as a ring with atreaming
appendages extending from the main body in all possible
directions, some nearly straight towards, or away from ub,
others at every imaginable angle with our line of aigkt. The
resulta in perspective foreshortening would evidently, under
theae circamstattces, be highly complex ; the eye being pre-
sented with groups and streams of etars, immensely various in
remoteness* but all projected indiscriminately upon the same
zone of the heavens. Thus, while some branches, pursued
along their outward c-oiLree, fade at last into dim nebulosity,
other Milky Way groups may be distinguished as bright
separate stars, because much nearer to us than the generality
of their associates. Closed ringSj however, are beginning to
appear alien to the cosmic plan of structure. Nebulae pre-
tienting that aspect are, perhaps without exception, resolvable
into helical or spiral figures. And it would be hazardous to
assert that the Milky Way lies outside the mysterious law
imposed upon minor aggregations.
Its internal organiHatiou is of baffling intricacy. It collects
within its ample round, there is every reason to suppose, an
absolutely endless variety of separate systems, A multi-
tudinous aggregate of individual clusters, it is composed more-
over as a whole very much like one single cluster on a colossal
scale. Its fringed edges, its rifts and vacuities, are, as we
have Been, reproduced in miniature in nimiberleae star-groups.
" Einge," and "sprays,*' and " streams" of stars are unmistak-
ably common to the two orders of formation ; and the stellar
^ Hemorie dei R. IitUato Lomhardo, L xir. [k 62.
T m
hndd
-f The twtiii ■ «9vvakMt te tka
What k tfav «vKig» dii-
I How far
hftw lo KbtcI bdbre isdiDg onmiwm mUmkOj in tfae
ci Um CRKwdMlobiKto paodMo^to
" nllkr " dfeet «f • Debolooi atntaB ?
Certuzi ktiomibA^ in thk mmttcr ii not W> be had; inliar
tKMU sad profaabb Tititi»wt-ni bare to tak» ila phea
Vairoomb, *■ Uie vpaboi of a disciunn enbnong all tbe
sTsiiable fiute, arriveB at the oooohtnoa tliat the Milky Waj,
in iDOtt of ita aedioiia, it no Dearer to ns Uksa mxdd be
Jiignified by a pai^lax of otie-Uunuandth of a aecww],* oarz^-
vpandin^ to a ligbt-joumej of S 200 yeai&. Now oar son, if
thu» uaimaginably removed into space, wotild ahnnk to a sur
of tb« fiftaeotb magciitiide; it would seem just one of the
grainii of Bhining aand coagiilated into heaps out near Um
oonfincM of the sidareal worhL PreBumablj, tb^n, a large pro-
portion of tba loatrouii speclu formings in tLeir mmumbered
agffregate, the nebtiloua arch amid the confitellations are really
Mutw on tin* mixh of our own. They are, however, pretty
avidenUy intermmgbd with many amaller globes, and with
HOiiid vaMtly larger. M. Eaaton has nucoeeded,* by detailed
coriijHFiriHoaa, in efitabliabiug a correlation between galactic
KtrtuliircB tiiid tliu nUiTti, from about the sixth to the fifteenth
niJiynitiidtw, cnuTiiefatt^d by Argelander and otbets. The in-
fereuw jm thua n*ndcryd oompulsory that a percentage of these
oomparativcLy bi-ight orba are geuutne cgtistituents of the clustera
1 Th4 Stitrg, p. »ir.
• ViMtriimtiim dt la iMmUn OatacligM, p. 24 ; Newoomb, Tk« Stan, p. 273.
THE MILKY WAV
347
with which they are colliueated. There are be&idea strong
grounds for the belief that manj*, if not moat, of the bluiBh
brilliants giving helium apectra domioate these comprehensive
groups, Mr. Kanyard pointed out in 1891/ from the evidence
of M>, H, C, Ra83eU*8 photographs, that the chief luminary
of the Southern Cross is centrally situated in a curiously
symmetrical little cluster of excessively faint stare ; and the
irreaistible concluaion of its being physically related to them
may be safely applied to a number of other lustroiwi objects of
the same spectral class. The range of actual size and splendour,
then, among the components of galactic atar-drifta is astonish-
ingly great — much greater, in Professor Newcomb's opinion,
than in ordinary detatilied clusters, such m the Pleiades, or
the double Sword-handle groups The helium Htars of the zone
arej indeed^ veritable tritons amidst shoals of minnows ;
they are frequently of a magnitude transcending the powers
of imagination to realise, while their dwarfed aasociatee may
L. weU be of average sun-like stature.
^B The Milky Way clouds are not condensed from the general
" contents of the sidereal heavens ; they are markedly distinct,
I Their spectral peculiarities make thia clear. They are built
up, essentially and fundamentally, out of Sirian stars ; * those
of the solar and Antarian types seem to be totally absent
from them. They include, however, nearly all the helium and
bright-line stars that exist ; but they are relatively few ; they
scarcely count as ingredients ; they are rari nantes in gv.rgite
vctsto. Many galactic tracts, too, are suffused with a phos-
• phorescent glow ; they harbour nebulous formations which
only the photographic camera, through ite faculty of persistent
gazing, has been able to actualise and define. Thia surprising
characteristic affords an additional proof that cosmic conditions
of a special kind prevail in the enigmatical girdle wluch
L enclasps the mystery of the universe.
^H From a most careful study of the Milky Way at Cordoba,
where it was seen to peculiar advantage. Dr. Gould inclined
to regard it as the product of two or more superposed galaxies,'
The fact of the two narrowest and brightest, and the two
^ KndioUdgtj voL xir. p. 112.
■ PickeriDg, Harvard AmutUf vol. M, p. 2£,
* Utw\. Arijenti'nai p. 381-
348
THE SYSTEM OF THE STARS
moat diffused parts lying in pairs opposite to each other
is certainly remarkaWef and lends gome countenance to
the Burmifle that the " necka " in Cassiopeia and Cnix really
repn^Bont the intersections of the two croesed zings visiblj
divergiag in Ophiuchns. H. Celaria^ too, as we have seen,
adopted the hypothesis of a compound Milky Way, but of
eucli a form aa to allow the possibility of one of its oonstitueot
annuli being comprehended by the other. The transition to
a true gpiral shape was thence easily effected, and a wider
range of facts was rendered capable of theoretical accommoda-
tion. Whiit is unmsstukable is that the entire formation,
ningle or compound, wliile individual and specific, is yet no
isolated phenomenon. The contents of the firmament aw
arranged mtiinly with teferenee to it. It ia a lai^ part of &
larger il^ign exceeding the compasa of finite minda to gnep
in its entirety.
CHAPTER XXVI
STATUS OF THE NEBUL«
question whether nebulae are external galaxies hardly
jy longer ne^ds diflcuaeion. It has been answered by the
rogresB of research. No competent thinker, with the whole
of bhe available evidence before him, can now, it is Hafo to eay,
maintain any single nebula to be a atar system of co-ordLnate
rank with the Milky Way. A practical certainty haa been
attained that the entire contents, stellar and nebidar, of the
sphere belong to one mighty aggregation, and stand in ordered
mutual relations within the limits of one all-embracing scheme.
All-embracing, that is to say, bo far as our eapacities of know-
ledge extend. With the infiiute poasibilities beyond, science
has no concern.
The chief reasons justifying the assertion that the etatua
of the nebulee is intra-galactic are of three kinds. They
depend^ first, upon the nature of the bodies themselves;
secondly, upon their individual stellar associations ; thirdly,
upon their systematic arrangement as compared with the
systematic arrangement of the stars.
The detection of gjiseous nebulae not only directly demon-
Btrated the non- stellar nature of a large number of theae
objects, but afforded a rational presumption that the others,
however composed, were on a commensurate scale of size, and
situated at commensurable distances. It may indeed turn out
that gaseous and non-gaseous nehulee form an unbroken aeries
rather than two distinct classes separated by an impassable
barrier. Their spectra have perhaps more in common than would,
at first sights be supposed. For the vivid rays of green nebul»
are superposed upon a gauzy background of continuous light,
34^
850 THE SYSTEM OF THE STABS
which appears to be resolvable into a mulUcude of bright lines
in juxtn{H>aitioa [^ and the spectra of white nebulie show, wA
a emooth, priamatic gradation, but alight inequalities in the
flow of light, indicating effecta of abaorption, of emiasioD, or
of both combined Before indeed anj settled opinion can be
formed as to whether these analogiea have reallj the tiaoa-
tional meaning we might be inclined to attribute to them,
nebular spectroBcopy oiust be a good deal further advanced
than it is at present. But apart from this question, rektioo-
ehip between the various orders of nebula is manifest. The
tendency of aU to assume spiral forms demonetrates, in itself
their cloae affinity ; bo that to admit some to membership of
the sidereal system while excluding others would be a palpable
abaurdity. And unce those of a gaseous constitution must be
so admitted, the rest follow inevitably.
Of the physical connection of nebulse with particular etars,
fresh and incontrovertible proofs accumulate day by day.
Nothing can be more certain than that objects of each kind
coexist in the same parts of space, and are bound together by
most intimate mutual ties. To argue the matter seems, as the
French say, like " battering in an open door." We need only
recall tlie stars of the Pleiades, photographically shown to be
intermixc^il with nebulae, and those in Orion still bearing in
their spectra traces of their recent origin from the curdling
maasea around. The nuclear poeitions ao frequently occupied
In nebulae by stars single and multiple, reiterate the same
assertion of kinship, emphasised still further by the phenomena
of stellar outbursts in nebulee. The scenes of these must, as
the late Mr. Proctor insisted, lie within the circuit of the
MiUcy Way, unless we are prepared to assume the occurrence!,
in eitra-siderffiil space, of conflagrations on a scale outraging
all probability. It has been calculated that if the Andromeda
nebula were a universe apart of the same real extent as the
Galuxy, it should tie situated, in order to r^uce it to its
present apparent dimensions, at a minimum distance of
twenty-five galactic diameters,* And a galactic diameter being
estimated by the same authority at thirteen thousand light-
years, it follows that, on the supposition in questioi
1 Pftlmer, Lick Bullttin, No. U.
" Woaae. Sdtr^/ten Witner VtrnnSy Bd. t. p. 318.
STATUS OF THE NEBULA
351
Duld require 325,000 years to reach us from the nebula.
ie seventh -magnitude star then which suddenly shone out
the midst of it iu August 1885 should have been an
aluteiy portenfcouB orb. In real light it sliould have been
^uiviilent to 762,000 stars like Siriua, or to sixteen million
ach suns as our own J But even this extravagant result
inadequately represents the real improbability of Ihu hypo-
thesis it depends upou; since the Andromeda nebula, if un
external galaxy, would almost certainly be at a far greater
remoteness from a sister-galaxy than would be represented by
twenty-five of its own diameters.
Just as the Milky Way might be described as a great com-
pound cluster made up of inuumerable subordinate clusters^ so
the greater Magellanic Cloud seems to be a gigantic nebula
combining into some kind of systemic unity multitudes of
separate nebulie. To the naked eye it shows vaguely a
brighter axis spreading at the extremities so as to produce h
resemblance to the " Dumb-bell " nebula ; photographic ex-
posures bring out unequivocal traces of a spiral conformation ;
either way it shows signs of definite oi^anisation as a coherent
whole ; and it includes, strangely enough, among its inmates, a
miniaiure of itself (N.G.C 1978), but of much greater
intensity and distinctness. Sir John Herschel's enumeration
in 1847, of the contents of the "Cloud," gave conclusive
evidence of the interstellar aitnatiou of nebulie — evidence, the
full import of which Dr. WheweU was the first to periieive.
Over an area of forty -two square degrees, 278 nebular objects
(stare being copiously interBpersed) are distributed with the
elsewhere unparalleled density of 6^ to the aq^uare degree.
" The Nubecula Major," Herachel wrote, " like the Minor^ con-
sists partly of large tracts and ill-defined patches of ineaolvable
nebula and of nebulosity in every stage of resolution, up to
perfectly resolved stars like the Milky Way, as also of regular
and irregular nebulie properly so ealledj of globular clusters in
every stage of reaolvability, and of cluetering groups sufficiently
insulated and condensed to come under the designation of
clusters of stars," ^
Here then we find — in a system certainly, as Herachel said,
' $ui generis*' yet none the loss, on that account, instructive
' Cape RMults, p. 14^.
wd iwowwd (7 Dr. Max Wolf It k cwri— dty exaB|Aifed
ia Clw rtarnlieQiided nidoi of the Aatnm B«baki' (■>
Pbl« XVUL). which soons to hare abevfaed or npeOed haaa
iti hmriftiatot nc^botu-hood the dtmm galacck ctetU impmA-
big tomrdf IL Sunilarij, a eampaiBtiwely TMaiit itjgion
aooDfDpUMi the Onoa nebula, within whkb. seveftbeloBr
ttttt twuni Mftd flicker nfter the muDer of the componoatB of
globohv ciiiitwi. Thfl i^laoement of stan hj n^mkna laattflr
it flftfal ooofpiciioua in Plate XX., which reprodaoM, bj* Dr.
Wolffl kiuil permiMion, a phot4^raph taken by hisn, July 10.
1904, with an «xp06ure of four boom The depicted Dcbola^
which hod been discovered ten yeara previooalj. is about 10' in
> /'Ml. Trtuu. vol IxxiT, p. U»,
(lUi*).
^Mi
STATUS OF THE NEBULA
353
diameter, of a round shape, and a complex Btructure. " It is
placed centrally," Dr. Wolf Writes, " in a very fine lacuna ^t^id
of faiitt stars, which aurrounda the luminous cloud like a
trench." ^ Moreover, this negative " halo fonnfi the end of a
long channel, running eastwai-d from the western nebulous
clouds and their lacunfe^ to a length of more than two
degrees.'* The coexietGnee in the same Bidereal district of
nebulEe and stars could not well he asserted with stronger
emphasis than by the clearing of a dark foaae for the accom-
modation of the cocoon-like object in Plate XX.
The larger plan of nebular distribution, as being the
inverse to that of stars, partially revealed itself to the elder
Herachel ; but Sir John first brought into clear view the
distinct and striking division of the nebuhe into " two chief
strata, separated by the Galaxy," Taking the circle of the
Milky Way as a horizon, he remarked that the accumulation
of them in Virgo and Coma Berenice© " forms, as it were, a
canopy occupying the zenith, and descending thence to a con-
aideiable distance on all aides, but chiefly on that towards
which the (oelestifil) north pole lies.''^
Tliie crowding about the galactic pole is less marked in
the southern hemisphere, though here too there is a ''chief
nebular region " approximately corresponding to that in Virgo,
The distributioD isj however, on the whole much mote uniform
than in the northern hemisphere, or rather, more uniformly
patchy, rich districts alternating with more or less ample
vacuities. One of these exteuda about fifteen degrees all
round the south pole, the Leeser Cloud marking its edge.
The remarkable fact, too, was noticed by Sir John Hersehel
that the larger nubecula seems "to terminate something
approaching to a zone of connected patches of nebulce," reach-
ing across Dorado, Eridanus, and Cetus to the equator, where
it unites with the " nebular region of Pisces." A similar line
of communication is less conspicuously kept open with the
minor nubeculaj and this feature of "streams" of nebula?
with terminal aggregationa was considered by Proctor to be
distinctive of southern skies.* He adverted besides to the
coincidence of two of them with stellar " streams " in Eridanus
' Monthly Notiaif vol. liiv. p. 639. " Cap« Resiiita, p. IS7.
1 Monthiy N^aiat, tqL xxix. p. 340.
364
THS SYSTEM OF THE STAES
and Aquarius, and waa Htnick with a rignifioant dtAdeacj of
bright atan over the iuterv^ between nebular groups.
Ampler aoquiuixtanoe with tbia das4 of objects has, on tba
whole, served to r&tifj earlier conclusions relative to their
mad« of iiL'&tteriQg. Their overwhelmiiig teadeucy U* oon^
gate jibout the norUi galactic pole is accentuated by the nnllB
of Dr. Mai Wolfs photographic surrey ; ' while the preseooe of
« aecoudary focus of aggregation in Peiseus and Andromedi.
remarked by WaterSj' was rendered unmietokable hj the sah-
eequent investigations of StratonoE' M, £astoQ, diacaaiiig
the subject with his accustomed thoroughness in 1 904.
was especially struck with the disturbing influence of the
Magellanic Clouds. Hence possibly eo fundamental a diveiaity
m the modes of nebular difltribution on either eide of the
Milky Way, that he coogidera it as " very probable that the
structure of the southern galactic sky with regard to the
nebulae differs entirely from that of the northern g&lactic aky."^
The leading facte of nebular distribution were correctly
descrihod by Herbert Spencer in 1S54. "In that zone***
he wrote, " of celestial space where stars are exeeHsive^
abundantj nebuhe are rare ; while in the two opposite celeetul
spaces tliat are furthest removed from this zone nebulse are
abundant. Scarcely any nebulie lie near the g&Iactic cirde,
and the great mass of them He round the galactic poles. Can
thifi be mere coincidence I When to the fact that the generd
maaa of nebulfie are antithetical in position to the general mass
of stars^ we add the fact that local regions of nebulfc are regions
where stars ore scarce, and the further fact that single nebuhe
are habitually found in comparatively starless spots, does not
the proof of a physical connection become overwhelming?***
Accompauying, but considerably overlapping the Milky
Way aloug its entire round, is a " zone of nebular dispersion "
(as Proctor called it) — a wide track of denudation, ao far
as these objects are concerned. The nebular multitude shrinks,
aa it were, from association with the congregated galactic octars.
A relation of avoidance is strongly accentuated. But wjth-
' Jicpm-t of Kani^flmhl OhKrwaary for 1902 | AUr. N<uK Ktt. 3812.
* Monikly Noti^tf, vol. Im p. 527.
* RilteupiLrt, K J. S. Adr. Gta. Jfthrg. xxxrii. p. 3&S,
* Proc Aead. of Sdtme*, Am&Iord&tu, June 2£, 1901 ; Atir, Nach, Ko, SMft.
> TM* Nftntiar ffypctft*su (with Addend*), p. 113.
STATUS OF THE E'EBTTLjE
355
iwal implies recogaition. It implies Che Bubordination of
and nebulae alike to a single idea embodied in a single
Beme, The range of our possible acquaintance is aec^rd-
5I7 restricted to one " island universe " — that within whose
oundaries our temporal lot is cast, and from whose shores we
wistfully into infinitude.
Dismisaing, then, the grandiose but mi^eading notion that
nebulae are systems of equal rank with the galaiy, we may
turn our attention to the problems presented by the pecu-
liarities of their interior situation. When these are subjected
to a detailed examination, distinctions become evident between
the di£ferent classes of nebuhe. Distinctions so marked as to
lead almost to their separation.
The " relation of avoidance " to the Milky Way juat adverted
to prevaila on/y among the " unresolved " nebuhe. These, it
ia true, are the great majority of the entire, so that the con-
clusion of nebular crowding away from that zone remains
unimpeachable. For certain classes of minor numerical, but
high cosmical importance, the relation is precisely inverted.
Over gaseous nebulae and clusters, the Milky Way seems to
exercise an attractive infiuence equally strong with its repul-
sive effect upon nebulse of other kinds.
Forty out of one hundred and eleven globular cluBterg
belong to the galactic zone,^ which is hence twice as richly
furnished as the rest of the sky with these wonderful objects.
And the excess rises to twenty - five times for irregular
or nondescript clusters^ 434 out of 535 of which — that
is, 81 per cent — are located in, or close to, the Milky
Way. Many cluaters, indeed, obviously form an integral part
of the formation itself; of others, it is diffiexJt to decide
whether they should be ranked as distinct, or simply as
inteneifications of ortliaary galactic star-groupings. To the
latter categoi-y almost certainly belongs a collection (M 24)
visible to the naked eye as a dim cloudlet near /x Sagittarii,
and named by Father Secchi " Delle Caustiche/* from the
' Taken as of ttie unifonn width of thirty degre«4, nml coTering ^ of the
iphuTo. Mujor M*rk-wiolt {Joum. Lvv. Asir. ^Svc^ vol. Tii. ^. 182) Goda the pro-
portloD&te area of the Milkf Way in the uorthfro hemispbero to bo ^, iaiho
soutbcro i- Pickering (HaTWird Amials, yol. xlviil p. 165) ustisifttas Ibe
galactic area at 1&,&12 squan degrees, or ^ of the sphere.
356
THE SYSTEM OF THE STABS
peculiar armngemont of its staifl in t^jb^ arches^ caoaltt
GarTBB^ and initirlwiued Bpirals. This again is included ia t
great ovat condetiaution of galactic atars, obTioosly endoved
with some degree of Btructural iDdependeiice.
Oaseoufl aebuli^, like gaseous stara^ are nearly exdoai've in
their galactic affinities.' Very few planetaiies caa be foawl
at anj oonsidemble distance Irom the favoured xone; die
Bpectroacopic senroh for stellar ttebulfe is &mtless unless within
its borders ; and they embrace — with one exception all ibft
irregular nebula. This single exception is a most significant
one. It is that of the " great looped nebula " (see Pl^te XV.).
an important constituent of the greater Magellanic Cloud
PUiuly, then, the conditiona allowing primitive coemical
matter to remain uucondensed in galactic regions, prevail alwi
iu the nubecula. The individuality of its organisation has
been strongly accentuated by the discovery, lately made at
Harvard College, thut very many of the stars contaijied in it
fluctuate mpidly in light.* Misa Lea\'itt'B examination af the
Arequipa platea yielded at once a harvest of 152 variables;
and more doubtless a^ait recognition.
Gaseous and white nebulte meet on equal terms only in
this comprelieusive aaaemblage. The Milky Way is more
escclusive. It favours the former class largely at the expense
of the latter Within its precincts only one in sixteen of those
dim, often fautaatically-ahaped, objects is met with, the analysed
light of which gives no indication of gaaeity, while their even
texture, under the highest telescopic powers, suggests no
approach to the stage of breaking-up into 9tar& What then
is their nature I Is the difference separating them in appear-
ance from the resolvable aggregations of star-dust, crowding
the Milky Way, a difference of distance solely ? Are they
too clufltora beyond the reach, through remoteness, of effective
scrutiny ? There is nothing in their aspect to preclude this
BUppOflition. So far aa observation can tell, they may be of
stellar compoattiou. Only it is not easy to understand why
nebula situated near the galactic poles should be immensely
and consistently more distant than nebulas thronging the
vicinity of the galactic equator.
1 Bauacbinger, V. J, S. Aatr. QeM. Jahrg. xxlv. p. 4S.
3 ffarvard Circular, TUq. 89 ; Attr. l^ath. No. 3»0e.
STATUS OF THE NEBULA
357
Mr. CleveUnd Abbe* sought to overcome the difficulty
t>7 imagining the nebulie to be equably diatributed over the
rface of a " prolate ellipsoid," its loQger axis coinciding
^proximately with the axis of the llilky Way ; and thia
igetneut would undoubtedly give an appearance of crowd-
ig in the observed directions, since to an eye placed near the
Bnti-e of such an oval figure, objects imiformly scattered over
its Burfoce would produce^ by perspective, the effect of nmning
together near its pointed enda. But this highly artificial
contrivance was scarcely realisable. Our minds demand
from a theoiy not barely that it "cover the phenomena"
but also that it show itself congruous with the general plan
of operations upon which we can see that nature works. Be-
sides, the local distribution of nebula is ao far from uniform,
that antecedent probability is in favour of their general distri-
bution being also marked by striking irregularitiea. The
" canopy " of nebulee in Virgo is then, we may rest assured,
as genuine an accumulation in its own way aa the spherical
assemblage in the Magellanic Cloud.
But if there be no systematic difference of distance between
the nebular classes occupying contrasted situations as regards
the Hues of galactic structure, there must be a systematio
diffei-ence of constitution.^ The parts of those objects crowd-
ing towards the poles must be comparatively small and close
tc^ther. We have indeed already found reason to believe
that clusters do, in point of fact, merge insensibly into nebulae
— that groups of genuine suns at wide intervals stand at
the smnmit of an unbroken gradation of systems with
smaller and closer constituents, down to oocumulations of
what ia ahnost literally '^star-dust," Eesolvahility is hence
a question of constitution quite as much as of distance, and
we are brought to the conclusion that, while galactic nebulte
are of what we may roughly describe as stellar composition,
noQ -galactic nebulae are more or less pulverulent. We
cannot of course pretend to account for this remarkable
distinction. All that can be said is that it appears to be
actually existent. The irresolvable "polar" nebuhe perhaps
escaped influences powerful over the " equatorial " ones. Their
* Mi'nthly Noticts, vol, ixvii. p. 262.
* Proctor, Monthly Noiia^ vol. iriz. p. 342.
368 THE STSTKH OF THE STABS
&gniopmmA, U anj nte, oaems to hsTe Uken « di&nsl
eomxm.
The iftectmcope iofenni qb that nebnlK pocBUB Eft&t
wioGitJM of tbe MLine cHer «■ tbooe of eur&. And that
^»paRnt fixity to wiaaal tkBEmtian nimniwlkMiaUlj imlti,
in put from thor ei Lre uw nanoietteB, in {ivt finm tbitt^
fiT^WTnnmi of aoetumte nmsoremeoL Tbe fuogoUiitioi of
iMbular ilJUrfhntiwi mttatd boides indirect erideticse of
menL ** Streuninefli,' if it mean anjUiing^ implies that
hodiwi affected bj it adrmnoe in oommoai towarda a csoniiBoe
goaL Aggregatton at tbe end of a sboam pirompto tbe con-
jeotvre ^at a rootion of advance was at a oertaia point, hf
•ome aupervening attractioD, ewajed into a motaoo of feYolo-
tion. A bint aa to the origin of the WagiJlanw* Clonds maj
hence be derived. Thej represent in eome sort veaeets filled
througb long pipee from a vast reservoir. And slqco the pipes
are still there, the flow may he eoDCselred to be still in prognaa
Wore it to cease, tbe ooimection of the nubecula? with th«
main nebular bodj would eYentxiallj be interrupt^ and their
inaulation would become complete.
The fidelity with which gaseous nebula and clnsteis adhere
to the Milkj Way as seen projected upon tbe sphere, wazranta
the inference that their distribution in &pace is of a similar
character. It would be lui reasonable to disconnect them from
tt. forjuatton of which they ao closely follow the lines. We
can Bcorcoly err in supposing that they lie in general vif&tA,
not behind, or in front of it. Thus, the globular clusten
richly strewn over the branch of tbe Milky Way from Scorpio
to Opliiuchua, but withdrawn from tlie cotiterminoua dark rift,
plainly belong to the cloud-like stellar masses, owing to tbe
abaencti of which the fissure seema black, although den^y
Htocked with stars to the tenth magnitude. Other compressed
groups Btftud out from a curtain of apparently still more remote
8tar6, repreaentiug poasibly a divergent galactic ramification.
Such tamificatioufl must in many cases be greatly fore-
shortened as viewed from our nearly central poaition ; in £ome,
they may appear only as brilliant knots upon the " trunk " of
the Milky Way. Possibly, the double cluster in Perseus may
partake of this optical character. It may be the termination
of a branch spreading inward, and seen nearly end-on.
STATUS OF THE NEBULA
359
Like the Perseus clusteis, the OrioQ nebula gives indica-
tions of greater proximity than the main galactic accumulation^
to which it is nevertheless beyond doubt etructuially related.
For a winding nebuloius extension from the Milky Way can
be traced past a Orionia through the belt and sword, the
bright stars marking which are demonatrably associated with
the nebula. The inference then presents itself that the whole
mixed system, or series of systems, is placed upon an obliquely
directed oElset from the galactic zone. Keasoning of the same
kind may perhaps apply to the combined nebula and cluster
M 8, It occurs as a premonitory outlier of the leading division
of the fissured Milky Way, from which it Ilea a little apart ',
and it seemed to Sir John Herachel only an " intent exaggera-
tion " of the stellar collections in its neighbourhood.^
Summariaing our conclusions, we find the unity of the
stellar and nebular systems to be fully ascertained. They are
bound together by relations of agreement and contrast scarcely
less visibly intimate than those severally connecting individual
members of each order. The general plan of nebuW distribu-
tion is into two vast assemblages, one on either side of the
Milky Way ; but while this ia, comparatively speaking, avoided
by the unresolved crowd, it is densely thronged with eluaters
and gaseous nebuke. The conditions of aggregation witblu
the zone may hence be inferred to differ from those prevailing
outside it ; but how and why they differ remains inscrutable.
As to the distancea of the nebulEe, we know nothing positive ;
they no doubt vary extensively ; noi can either linenees of
giain, or faintness of light (both of which may be inherent
quahtiea) serve to distinguish between those nearest to, and
thcKe further away from us. We may, however, plausibly
conjecture that the Loodlike accumulation of nebulte in Coma
Berenices is of the same approximate remoteness with the
main galactic stream, and may thus be said to constitute the
' cap of a sphere equatorially girdled by the Milky Way.
'■ 0»p« MtntU&f p. 887.
CHAPTEB XXVU
Tin comnticTioN o» tue REMrwsa
Wmi^u HJCRiiClliCL cDuceired it to be the sapxeow object
'ei M lre uomy " to obtiUD ii knowledge of ihe ooortnictioik U
%h% ht^ttat "; and thia, in his view, would be aooomplubad hf
the " determination of the real place of evBzy oeiestial body
iu ■pftce.'* * Thus limited, the problem would be completely
Bolvdd oonld the abeolnte diatance bo aacertained of all Uie
objdctt teleBcopicdllj or photographicallj di^certiible in tbe
■ky. But even the attainment of this unattainable paint
would never have satisfied Hciachers restlesa spirit. The
imI loope of hifl inquiriee went far beyond it. They had oa
hUtorical as well aa a statistical aim. "Looking before and
after," thuy embraced the past and future, no lesa than tbe
prtMDt of the OoHmoa.
Modem inveatigators are of tbe same mind The heavens
UO TOgarded by them from a 'physiological, rather than from a
purely anatomical point of view. Mere knowledge of structure
however ui-curute, will not content them. Tbe -vital functiona
of the organiRm, the mutual dependence of its parts, the
balanoG of the intemul forces t^^Qding towards destruction
and preaervation, the dimly-apprehended aim of its divinely-
sustained activity, engage their eager attention. The heavens
livo luiil mov(\ mid t!ie laws of their life and motion involve
the material dtistiny of man. It is impossible that he should
be iudilTorent Uy them.
Kvon, however, if our instinctive interest in the working
of the machinB were less keen, we ghould be driven to search
out the dynamical rulationa of its parta by the impossibility of
' PML IVofH. voL cTiL p. 302.
Ma
THE COKSTRUCTION OF THE HEAVENS 361
aerwise arriving at a true knowledge of their egometrical
3.tton& Not only are these variable from one moment to
lother, but acquaintance with them at any single momeut ia
ot conceiTably acceeaible to us apart from previous acquaint-
ice with modes and laws of motion. For our view of eidereal
bjects iu not siinultaneous. Communication with them by
of light takes time, and post-dates the scnaiUe impres-
jas by which we are informed of their whereabouts, in the
'direct proportion of their distances. We see the stars not
where they are — not even where they were — at any one
instant^ but where they were on a eliding scale of InatantB,
The epoch corresponding to the apparent position of each
is different, and the range of difference extends over some
thousands of yeara The reduction of those poeitiona to a
common epoch so aa to get a survey of the genuinely con-
temporary relations in space of all sidereal objects — ideally
feasible at best — could not bo much aa be thought of as
pOBsible without a preliminary knowledge of their diaplace-
ments during the centuries, or millenmuma elapsed since the
ethereal vibrations they originate started ou their several
joiu-neys hither. Thus the study of configurations blends
with the study of movements and forces ; the reetiictiona
placed upon thought by the effort to exclude all but a single
aspect of phenomena fall away of themselves, and we are (con-
fronted, whether we will or no, by the stupendous problem of
be universe as a vital whole.
As a whole ; but not necessarily ae the whole. The
sidereal world presents us, to all appearance, with a finite
system. Human reason would, indeed, otherwise be totally
incompetent to deal with the subject of its organisation. There
would be notliing for it but to lay down the arms of our
underetauding before its transcendental and appalliug magni-
tude. But the probability amounts almost to certainty that
star-strewn spate is of measurable dimensions. For from
innumerable stars, a limitless 3um*total of radiations should
be derived, by which darkness would bo banished from our
skies i and the '* intense inane," glowing with the mingled
beams of suns individually indistinguishable, would bewilder
our feeble senses with its monotonous splendour. This laying
bare, so to speak, of the i-mpyrean would be the simple and
362
THE SYSTEM OF THE STARS
certain resiilt oi the ockntlauaKice txd injtnitum af any
ment of sktorasl objeote coiiip«mhUs with thAt prevailii^^
oar netghboorhood. Ualen, that is to say, light Boffer
degree of eofeeblement in npace. If this be the case, thai'
<rar raasooings are put to eikDce, and a reil ia drawn ia-
peOfllTable to ficrutiny. But there is not a particle of evid
tliAt any sncb toll is exacted *, contraij indications are
and the awertiou that its pajiuent is inevitable depends np
malogiee which may be wholly visioni^,^ Ethereal abmip*
tioo and the actual inte-rceptiaa of stellar radiance by opaque
mnnHTwi. &ti9 equally the creation of the speculative intellect
K^ther mode of action ia vouched for by experience. We arc
theiit for the present, entitled to disregard the problematioU
elTeot of a more than dubious causa. The sidereal systeai
cannot be regardtKl as in any true senae infinite. The scale
of its construction, it \& true, strikes im^ination impotent;
in the muUitudjnous splendour of ita component?, in the
number and variety of the subordinate groups constituted by
them, in the magnificenb play of forces it unfolds, in the dim
prooesses of developmeut it suggests, it bears glorious witness
to the power and wiadoin of the Almighty Designer ; yet it
has limits, and for that reason it is a fit subject for the
exercise of limited understandings. With further systems,
" pinnacled deep *' out of our sight for ever, we have, properly
speaking.no ecientific concern; we only know that "when a
man hath done, then shall he begin " to declare the wonderful
works of God.
liegurding the visible world of stara and nebulee as aa
isolated, though e^teeasively complei system, we may tiy to
give the beat order we can to our ideas respecting ita consti-
tution. Let us see what are the available data. The number
of stars actually registered, inoludiug those in the Cape
Photographic Durchmusterung, approaches a million, of which
three-fifths, or thereabouts, are of magnitudes between the
ninth and tenth, and the rest are brighter. Beyond the
limits of this great censug, minute stars abound ; but to how
many millions they would sum up if completely enumer-
ated, can only be guessed very much ad lihituvi. Sir John
Herschel estimated at five and a half millions the stars (to the
1 Hiru, Conatituiiw de VStpaee CilaU, p, 207.
rJbmteenth photometric magnitude) perceptible over the entire
arity with his twenty-foot reflector; Struve ctilculated them at
twenty millions; anJ it has been vaguely surmised that a
hyniireil millioas could he shown by the most powerful modern
r telescopes. The photographic International Chart should
I contain, by M. Loewy'a reckoning in 1900, thirty million stars
rto the fourteenth magnitude. Yet Urota the basis of the work
I done in preparing it at GresEwich down to 1904, the number
. was evaluated at only 13,880»000. Thus, we are still in great
I measure ignorant on the point. Different parts of the sky
vary extremely in richness. In some, telescopic stara literally
' BWarm ; in others, they occur hut scantily. It has been com-
puted by Mr. Qore,^ that if the whole heavens were ag thickly
atrewn as the region of the Fleiadea, the number of stars to
the seventeenth (nominal) magnitude, would be about thirty-
thrcB milhona. But the method of distribution within a
definite cluster evidently gives no clue to that prevailing out-
side it. A fair specimen-field is, indeed, all but impossible to
choose. Counts in the Milky Way, extended in the same
proportion over the sphere, would vastly exaggerate the
crowding of the stars; which would, in an equal degree, be
underrated by counts executed outaide it.
Reliable data on the subject might, one would have thought^
be collected with practical usefulness by the method of
*' photographic star-gauging." Eeckonings of the stars in their
light-ranks, upon plates exposed for various lengths of time,
ought to tell with certainty how far the ideal law of augment-
ing numbers holds good, and where " thinning-out " becomes
apparent. In an equable stratum the stars must nearly
quadruple at each descent of a magnitude, simply because the
cubical apaee holding them is quadrupled.^ Should this i-ule
be overthrown by excess^ a real crowding is indicated, at the
di^itTice corresponding to the altered rate of increase ; if by
defect, then obviously the supply of stars in the region
examined is becoming exhausted, their scattering is sparser
than in our nearer vicinity, and the termination of the aeries
is at hand, if not already reached. Photographic soundings
^P 1 Joitm, X«i. AstT. Soe. toL vii. p. 180.
' For some reasoD atill TiDezpUiued, tli« obaervod ratio fttllfl cotiaiiteatly
than of the theontickl ntiih
364
THE SYSTEM OF THE STARS
h&ve. nevertheless, some special drawbacj£&* Theiz oaa %
4bove all, hampered by wide disparities depending on subtle
variations in atmospheric transparencj, which incalculably
modify, from one night to the neit, the registering powers hi
perfectly similar plates*
But even Herschel'e Milkj Way gauges, although indis-
criminate as regards magnitude, afforded distinct evidence o( a
termmatlng series in the fact that the numbers of stais
recorded by him amounted to only one-third of what might
- g. * — * — ± — -It ^ - J.
O O ~ ^ 1^ H
^ — 3 — a — 3 — ■
, l<L--DI*tribu.aan of DM ataji within 1" of t^B Pols, uhowlDg tJw mOoof POmbew tt
flpftcfl for <Acb hjilf-TiujrniUid«.
have been anticipated from the penetrating power of his
instrument appUed to an indefinitely extended system. And
for a " mean sounding " at the northern galactic pole, M.
Celoria, witU a refractor showing, at the utmost, eleventh'
magnitude stars, obtained a number almost identical with that
given by Herachel's great reflector. The larger instrument
then here revealed no additional stars. Similar symptoms of
exhaustion in the star*supplies may be found in Profesaor
Pickering's photographic catalogue of 947 stars within one
degree of the celestial north pole»* A single glance at the
1 aftvib J, BuruB, Joum. £riL Ahr. Aa. toL xiL p. 75.
* Uarvard Aniiahf vol. xviii. p. 203.
THE CONSTRUCTION OF THE HEAVENS 365
eynoptical table giving the nmnbera for each hftlf-magnitude,
BUlBcea to show that the DumeTical i-epreBentation of the lower
ranks is inadequate. The small stars are overwhelmingly too
few for the apace they must occupy if of average hrighlneas ;
and they are too few in a constantly increasing ratio. The
accompanying diagram (Fig, 3S) represenbs graphically the
decrease outward of density (or the proportion of numbers to
epace), deducible from Professor Pickering's enumeration on
the Bole supposition of the equal average lustre of each class
of stars. Those of the ninth are the moat thickly strewn;
the intervals between star and Btar widen rapidly and con-
tinuously (for the sudden dip at 9 '5 magnitude in evidently
accidental) down to 11'5 magnitude, when a slight recovery,
lasting to the thirteenth magnitude, sets in. A result of a
different character was obtained by Professor Neweomb from
a count of 312 stars to the eleventh magnitude on plates
taken at Potsdam for the International Catalogue. Although
the region examined lay close to the galactic pole, he could
detect no manifeafc falliag-off in the proportionate inerease of
number with faintness-^ But until more comprehensive
surveys of the same kind have been executed, it will be
impossible to lay down any general rule for the thinning-out
of sidereal strata. Nor, even if it were BuccASsfully formu-
lated for the rest of the eky, could it apply to the Milky
Way, where, "with both bands fuU/' veritable star -dust ia
scattered.
A far-reaching influence is exercised by this great zone of
condensation oyer the scattering of the stara, taken in the
gross ; but it grow^ more marked with their diminishing bright-
ness. Seeliger'B ascription to it of infeiior efficacy in the
southern hemisphere^ may now be tested with the help of the
Cape DurchmuBterung. The prefei^ence of lucid stars for the
Milky Way is slight yet unequivocal ; it appears from some
careful statistics published by Mr. Gore," that even in them,
the galactic zone is once and a half times richer than other
parts of the sky. There is some evidence, however, that this
crowding is towards a plane of condensation distinct from,
though very close to that of the galaxy.
* The Stan, p. 284. ' SiisutigsUrkftU, Munich, 1884, p. B21 ; 1856, p. 220.
* Jovm. Liv. Astr, Stfc. voL rii. pp. 175, 1S2.
366
THE SYSTEM OF THE STABS
A girdle of Urge stara epftoning the southern hemisphere
WHS thought hj Sir John Hexscfael to be the projectioii of ' 4
subordinate Rhoet, or stratam, deviating some tventj degree
from paralleliKm to the Milky Waj." ^ The hint was
developed hy Dr, Gould. " Few celestial phenomeoa ** he
sidured to be " more pcUpable than th« existence of a stream or
belt of bright stars," traceable *" with tolerable distinctziiMi
through the entire circuit of the beaveoa, and formiag a gnat
oinsle as well defined as that of the galaxy itself,*^* which it
croflse« at an angle of about 20^ in Crux and Caseiopm
Traversing in the southern hemisphere Orion, Oanis Major,
Atgo, the Centaur, Lupus^ and Scorpio, it porsuee its way ia
the northern through Taurus, Perseus, Cassiopeia, Cepheus,
Cygnus, and Lyra, its line being lees obvioasly continued by
the stars of Hereules and Ophiuchufli* Like the Milkj' Way
it seema to bifurcate near a Gentauri, the branch there thrown
off reuniting with the pareot stem in Andromeda. That tbe
stars thus marked out, to the number of about five hundred,
constitute with tbe sun a cluster ''of a flattened and somewhat
bifid form," " distinct from the vaat organisation of the Milky
Way," grew into a conviction with the progress of Dr. Gould's
observations.
The grounds upon which it was baaed have, neverthele^
been gradually undermined by close and varied research.
Gould's star-belt continues to subsist; its reality is unquestioned;
but its leLationa are dlffereut &om those which ho assigned to
it. It has assuredly galactic, not solar proclivities. Mr.
J, H. Sutton pointed out in 1891 that the tracts where it
ooftleecea with the Milky Way are marked by profound dis-
turbance of the nebulous streauL* But this could only result
from an actual intermingling of the two formations. Again^
many^ perhaps most of the belt-stars give spectra of the
helium type ; and the chosen habitat of helium stars is — we
are led to believe — within the galactic aggregations. Nor is
there the least justification for holding the sun to be a member
of any specialised Btellar group. Some ostensible evidence
derived from proper motions, implying the genuine existence
^ Gap* SimitSj p. 9S5.
Amer. Joum. of S^nct, vol. viii. p. 333 (1874J.
' Uran, Argentina, p, 356. • XtuwUcigt, vol. xir, p. 121.
J
THE COIfSTEUCTION OF THE HKVVENS 367
£L Bo]ar duster, is now known to have been misleading.
rofessor Kapteju was justiSed, by the data placed at hia
[>sal, in concluding that stars of the solar type are crowded
the neighbourhood of our sun,^ bub he fully recognised later
le defective nature of those data, and withdrew the inference
ided on them.^
The wide separation of the belt-stars from our own
ace in the uaiverae adds incalculably to the importance
the phenomenon which they constitute. Their remoteness
nficessarily enhances our estimate of their size and luminosity;
the condensation of an extraneous stellar multitude towards
the plane they affect testifies to their attractive power ; while
their orderly arrangement, as if in a ring-like enclosure, still
further perplexes the enigma presented by this surprising
feature of the sidereal eyatem. Its natural effect in dis-
arranging the theoretical progression of photometric ranks
augments seriously the difficulty of searching out the laws of
stellar distribution. Into those ranks close upon five hundred
extra stars are intrudedj all above the seventh magnitude,
which have no proper status among the denizens of intra-
galactic space. There is accordingly an excess of bright stars
with small proper motions — -sentinel-atars, one might call
them, posted at the outskirts of the world, which might well
serve to arrest runaways on the verge of breaking bounds
through over -acceleration. Gould, in fact, showed that,
deduction having been made of five himdred belt-stars, the
remainder of those he had the means of enumerating, down to
9^ magnitude, form a tolerably regular series, increasing in
numbers nearly in the theoretical proportion of their diminish-
ing light.^ And the conclusion that these five hundred
superfiuous objects do in fact compose a group apart, is
strengthened by the symmetrical arrangement, with regard to
the " belt," of the bright gtai's outside it Their tendency
to collect towards its central plane was thought by Dr.
•Gould to be irrespective of the Milky Way, except in ao
' Pnte. Amsirrdam Acad. t>/ Sdeiuit, April 2% 1AS2 ; Janaary 28, 1893,
■ md, April 20, 1901, p, 6S9.
' TUti " eiripiri<!Al ratio" (tLat reaaltlRj; from Actu&l euumerDtion) of multi*
IpliuatioD of Qumbers per magijitud«, i^ Z'9\2 ; the theoretical ratio is 3'9&7. —
Uran. ArgetUma^ p. 367.
THE SYSTEM OF THE STABS
for AS the two farmatioDfl oomctde bj tbo projoeCioii
upon the other.
It is worth QOtioc, U>o» that the present dijmitiaii ol ^
aoUr movement agrees with the general " li« '* of the tcj
although other stars pve no sign of preference for ft&y I
inoDUil j>lH.ae of revolutioiL Yet^ quite obviooftlj. Utt
figuriLtiuD of moving bodies is the abrogate exproamoo otl
motte of mavetneut- A ring of stars can be a sul
reality oul^ if it be constructed on a dynamical fonDdatat
IbH mombora niust travel along the JxttiQ of their di^tiibutio.
Shoul*l they eventually be proved not to do so, thea G<itjl
bolt will stand revealed as un illusory appearance. V
question of eyatemiitic proper motions is evidently fundaisexi'
to the rtrchi tectonics of the universe, and we are still a l<»g
way from being able to answer it
In a long series of researches^ Mr. MaxweU Hall of Jamaicft.
attempted to fii the elements of the sidereal system, reganl*!
as an undivided whole.* The plan of structure attributed U>
it WiiA identical with that suggested as barely pos«ibIg to b«
realised in globular clusters. Nothing could be simpler.
There being no dominant central mass, attractive force and
velocity increaee progressively outward, and ail the movements
in the collection, in whatever plane pursued, and whether in
orbits nearly circular or highly eccentric, are governed hj ft
single period, or annus itiagnu^. But the scheme is practioally
unworkable aa failiug to accommodate itself to the irregularitiea
and veraatilibies of nature ; and its elaboration conveyed onI)r
a warning that the great problem was, by such means, Im-
pregnable.
The subject is one which, for the present, can only be
approached tentatively ; it would be highly undesirable that
investigators should, for that reason, be discouraged from
approaching it at all. The life of a science is in the thought
that binds together its facts \ decadence has already set in
when they come to be regarded as an end in themeelvea
" Man is the interpreter of nature ; ** to draw up an inventory.
i Mtmo'tTi R. AHt. Soeiity, vol. xliil. \k 1G7 ; MoKthl^ Notiets, vol. xxzix.
p, 33fi; xldl. p. 621 ; Ivii. p, S&7 ; IviiL p. 473. In the ooiialudiiig iJAper*
of the BWiea, Sir. Hall found it «dTi««ble to aubstitui* for a law of fot&i ruyiag
directly m tho dUtauce one cobstaut at a!l distaocua Trom the ceutre.
I
THE CONSTEUCTION OF THE HEAVENS 369
', is not to interpret. It is true that speculation is
i^MPOiie to waader into devious ways ; but then " truth emerges
.ore easily from error than from confuflion," And in sidereal
ience especially, there i& danger lest inveatigatorB, seduced
ty the wonderful facilities of novel methods, should eshaust
eir energies upon the accumulation of data, and leave none
Cor the higher work of marshalling them along the expanding
lines of adequate theory. Mr, Hall's efforts had thus a value
not to be measured by definite achievement.
It ia scarcely probable that indications as to the
general plan of the sidereal world euffidently definite for
purposes of numerical calculation, can be gathered during the
present era of human knowledge. A limitless field of fruitful
Teeearch, however^ lies open even now in the systema of various
^Leg^a of subordination, the federated combination of which
■we may reasonably suppose to constitute the supreme unity
of the coamoa. From double, triple, multiple groupings to
knots, drifts, clusters, clouds of stars, an ascending scale of
complex arrangement leads upwards to the unknown — perhaps
beyond it to the unknowable.
As the outcome of recent statistical inquiries, a distinction
has been set up between the stars arrayed into more or less
definite groups or masses, and the apparently incoherent
multitude forming the ordinary population of sidereal space.
Every cluster is strewn with interjtieenb stars, and projected
upon a background of disconnected stars. Even the great
■nlactic drifts are not only seen through a starry veil, but
^Sui? possibly (ProfesBor Newcomb thinks) have a starry curtain
drawn behind them.
Hence Newcomb's inference that, if we could remove from
the sky the swarms of stara constituting the cloud-forms of
the Milky Way, as well as all local aggregations, " we should
have left a scattered collection, constantly increasing in density
towards the galactic belt." ^ Sweeping away the cry stall isat ion -
products (to put it figuratively), wa should find remaining a
saturated solution of stars.
Again, Professor Pickering states that stellar distribution
within and outside the Milky Way is so far identical, that the
proportion of stars of a given magnitude to the total number
' The Stan, p. 27a,
TH£ SYSTEM OF THE SXAES
in ft&y singU region is ereryvrbere tbe same. But -wiikh j
the galactic oroa the numbt^rH ar« doubled Tben itr I
twice as many Btars of each consecutive photoiaetiic nu '
down to the twelfth ma^itude. " The Milky Way." be adj-
"coven about a third of the sky, aad contains about half tl^
BtatB. There ia no evidence of a liudt to thp faintneea of eti&
although the proportionate increase in numbers becomee In
for each auccesaiTe magnittide/' ^
These are remarkable facts; aud tbey acquire a dtept?
meaning from their aaaociation with physical diveraitaa
The varjuua spectral daasea are not alike in their mode U
Bcatteriug. Each obeys laws and tendencies proper to it^
Thus, Sirian stars, which form the majority of the entL'
are drawn towards the plane of the Milky Way. and sup^^
the material of its lucent thronga Solar and Antarian star?,
on the other hand, display no galactic preferences ; they occur
with equal profusion in all sections of the sphere. "Tbr
Universe is thus ehown," Profesaor Pickering writes,* " to coo-
siat of two portions ; first, the stars of ibe first type which,
although frequent in all parts of the sky, predomicmte along t
oertaiu plane^ thus forming the Milky Way. The aeoood
portion conaiats of stars whose spectra are of the second and
third types. They show no concentration in the Milky Way,
but are, in general, uniformly distributed in all parts (^
the sky. These two portions should be treated separately
in all discussions of the structure of the Universe, such
as studies of piH^per motion, parallax, motion of the Sun
in space, eto. The proportion of stars of the first type to
the total number increases when fainter Btars aie included.
while with the Orion stars the opposite seems to be the
case,"
Our own sun, so far as present knowledge acquaints
ua, belongs to the class of what HerscheJ called "inter*
systematical stara"— stars, that iSj exempt from particular
ties, and exhibiting in their moyements the net result of
OOflmioal compulsion* How many of them there may be, we
have no means of judging ; but it is easily seen that epecJAl
association becomes more prevalent with increasing remoteneos
from our pout of observation. For tkb. among other
^ Sarwrd Annalt, roL xlviii. p. 166. ' Ibid. val. Ivl [x 36.
THE CONSTRUCTION OF THE HEAVENS 371
Baplacementa among the membera of the several groupa evade
otice. When their nature develops, as it must with the efflui
>ff time, it will perhaps occiision embarrassment The sub-
OJBteace of a dyaamical equilibrium may not always be implied
yj it Companionship, which on the sidereal time-acale might
called transient, is even conceivable. One set of t-om-
binations may be dissolved to give place to others ; a single
itar may pass from one vast confederacy to the next, seeking
its fortune, as it were, through space ; or, breaking away from
the entire congeries of fiysfceins, rush out into the ethereal
desert, to find itself, after milliards of ages, withiu the precincts
of a strange galaxy beyond terrestrial ken with telescope or
camera.
The more attentively the configuration of the stars is
studied, the more clearly do special phenomena of grouping
come iuto view. Among the minute stars of the Milky Way,
above all, a tendency towards the display of typical patterns
is, in certain parts of the sky, almost as uiimielakahle as it
would be in a ball-room crowded with dancers suddenly arrested
in threading their way through the figures of a quadrille
or a minuet Yet in the heavens, methodical distribution
muflt always l>e to some extent masked by the projection upon
the same surface of objects at totally different distances.
That, under these circumstances, it should often be effaced is
less remarkable than that it should occasionally become
apparent.
One of the " typical forms " in which stars seem to collect, is
that of an ellipse, or circle seen in perspective.' Radiated struc-
tures also occur; and Father Secchi, who early drew attention
to this curious subject, regarded the presence of a large red star
in a commanding situation among minor objects, as a common
trait of physical arrangements,* The spectral r«lationB of the
objects composing them was made the subject of a suggestive
study by J. Maclair Boraston in 1893.' As specimens of
a class of objects to which the " persevering student " coadd
make large additions " with an increasing conviction as to
the mutual interdependence '* of their constituents, Webb
1 Century Magazine, Sept. 1889, p. 787.
* Mti delV Acctid, Pont. t. vii p. 67.
' Attr, and AArephys\e$y toL xiL p. 98.
•r M
U-' I&e pn*
W*
ff
It mm^ JBifcrrl. be wiMttBd ktet tfe wn
gif«A tei^ cv b* p«t together by a rvrj otigfat stntch i
fMf . II «M iton «<nwii ii wun y by Udy Hqggm
tbe Ei^oai dh tf i btttMD of dote of ladiBB ink does
mcladff the poaribility, to a |»edispoeed ere. of fanning
Mo atBMSrt ftoj doind figanit- Ba( Ui« illastzntMm
not^ nor «u it rinwgnmt to leod ns to set down w
fnwginT7 tbe viidlile peenliaritieB of stellar
Tldi mmld be an wlawnft qiute aa nuacfaieToiu as
naqotlifled csednli^, flfnee there 15 camaUtiv« erideoeo^
the peculiarities in qoattiiMi aie, in m&nj cases, zeal
algnificaot.*
Mr Froctor expnaed hia conTiction that "star 1
will eventually prore themflelvee genuine by the mxammlty
* P^iMnUmt Wat fftndm Ohttrsat^rf, Tob. t iL
THE CONSTItUCTlON OF THE HEAVENS 373
."their proper motions.* AnU it is obvious that they can only
Bubeist upon this condition. Their order would otherwise
r bo a merely passing coincidence. Stars marching " in
5 Indian file," are presumably swayed by an identical force
jiactin,]^ upon Lbem from a very great distance. The group
J that they form is not self-centred, but makes only a part of a
larger organisation. Segregation, on the other hand« is the
diatitiguishing " note " of true dusters. They might be
described as autonomous demoeracies, each of their members
obeying the united commands of all, while outside influences,
although exerted upon them collectively, are without effect
upon their internal regimen.
A " streaming " can then be discriminated (at least
ideally) from a " clustering " collection of stars, by the circum-
Btance that the centre of movement of the one is external^
of the other internal It may possibly be found that the two
plans of oi^nisation prevail respectively in different sections
of the Milky Way; there is some appearance that they not
unfifequently compete or combine within the same cluster, the
streaming tendency working towards the diaaolution, the
clustering tendency for the preservation of the system. This
is not the only feature of sidereal construction which conveys
a hint to us that the world of stars and nebxilse is in a state
of transition. We see it in only one phase of its long develop-
ment. To regard its condition as settled upon an uaalterable
basis, would be to miaconetrue signe everywhere legible to
attentive scnitiny.
Since stars and nebula are undeniably united into a
single scheme, our view of the universe must embrace both
clashes. The distribution of nebulae is in fact complementary
to the distribution of stars. Assemblages of the one kind fill
in the outlinea left blank by the asaemblagea of the other.
The Milky Way, so far as can be immediately discerned, is a
rifted and irregular ring, furnished with innumerable tenta^
cular appendagea, and composed of stars in every stage of
aggregation. This ring, however, has obvious geometrical
relations with the rest of the sidereal etnicture. It marks the
equator of a vast globe, of which the poles are canopied by
le nebulae. Necessarily, too. of a rotating globe, since axial
* UhiPtrie of Start, p. 84.
374
THB SYSTEM OF THE SXAJK8
aovemaDt aione gms rise to the dwtmctjon bcl w mu poltti
Iha opinicfti that the ab^te of the viable miiTas 1 1
■pbericai^ or spbetoitkl. eatber than lenticular, wu fixprni i
bj Rftdau/ Kkin, and F^b.' The poUr reUUoM a< di >
ocbuhe to the pUne of the Milkj Waj admit indeed d m
other iDterpretatioiL And Lheee rolfttums can ecaiteljWT*
been determined otherwise than bj the rotation on ad txii d
the coloaaal, uDdirided volnma The oooditioQ tliiis fratwHil
aa primitivel/ existing m&y have become modified with tine; '
ftod. even if still prevalent, should be imreoogiiisftble bjr i&
Hince the relative Bituatioua of the heavenlj bodies WQc]d«ii
Falb remarked, be absolutely unaffected b^ it.
All that we can see clearl/ is that an uniTersal moveaiMft
of rotation had much to do with the present dis&ibatMii if
matter ia sidereal space. Whether the forces which hiit
brought it about axe 8till active, must remain an open queetiM-
The opposite tendencies of Btars to gather in the ^quatoriil
pkne^ and of nebnlse to stream towards the poles of the
s^Btcui, may not even jet be exhausted ; but the decision of
this point must be left to a dim futurity. The efficacy, in
the past or at present, of contrnxy drifta would apparentlj
imply an inherent diSerence in the qualities of the objects
TOBpoL'tively swayed by them ; and would, so far, contribute to
iuvaUdate the con;3ecrated hypotheaia of stellar developinent
from nebulsG.
Wti can, indeed^ heaitate to admit neither the fundamtf'nul
identity of the material elementn of the universe, nor the
Otfbuloufl origLD of stars. The transition from one to the
other of tht) two great families of the sidereal kingdom is so
gradual us to aifard a rational conviction that what we sae
contemporaneously in dififerent objects haa been exhibited
Buccassiyely by the same objects. Planetary nebuhe pass into
gaseous stars on one side, into nebulous stars on the other ;
the greater nebulEe into clusters. The present state of the
Pleiades refers us inevitably to an antecedent condition closely
resembling that of the Oriou nebula ; the Andromeda nebula
^ Bitll AttT. t, il, p, as.
■ Bandbueh der HimrMlftrtchHnungefi^ Tb. ii. p. 313; Sir(*ti, Biiude tu.
p.. iO, nil. p. 19H.
THE CONSTRUCTIOK OF THE HEAVENS 376
may TepresecC the nascent stage of a splendid collection of suns.
But even though stara without exception have Bprirng from
nebuliK, it does not follow that nebulaa without exception
grow into etara. The requisite conditions need not invariably
fiubeist. Other ends than that of star production are
perhaps met and promoted by the chief part of the present
nebulous conteuts of the heavens. The contrast between
stellar and nebular d^tribution is intelligible only as express-
^ ing a definitive separation of the life-histories of the two
L classes — a divergence destined to be perpetual between their
lines of growth.
Progress, then, is the law of the universe. From its
present state we can obscurely argue a " has been " and a
,flball be." The face of the skies is not cast in stereotype.
a vesture Thou shalt change them, and they shall be
.ged.'* They shall change, by no caprice of hazard, but
subjection to laws unalterable in their essence although
finitely various in their applications, divinely directed
towards the continually more perfect embodiment of the
unfolding Eternal Thought.
But the glory of the heavenly bodies, it is asserted, must
come to an end. It results from a merely transitory state of
things. The radiations, by virtue of which they shine, are
the outcome of what may be figuratively termed the effort of
nature to establish a universal thermal equilibrium. This
condition will be attained when the frigid " temperature of
space " reigns in all the millions of bodies which once were
suns, and will thenceforward revolvCj amid " darkness that
may be felt," the mechanism of their movements unimpaired,
but inert, lifeless, and invisible. Is this then the pre-
destined end ? Science replies in the affirmative. That is to
say, it knows no better. Yet there is much as to which it is
ignorant. Matter rests upon a subsensible basis, into the
arcana of which no inquiry has penetrated. The observation
of phenomena leads, it may be said, to the shore of an all-
ditfoaivo ocean of force, the existence of which is implicated
in their occurrence. That is all we know ; at the brink of
the ocean we pause, helpless to sound its depths, or number
the modes of its manifestations, or predict the tasks of re-
novation or preservation committed to it. We can only
Sj«
'-like •
ft ■
D
■
1
■
^^H
^^^ APPENDIX
^^^^H
^^H
IP TABLE
I
^^^H
^M Tne 40
BRiaHTEST Stars in
ORDER OF Magnitude^ ^H
P
THE 8UN. BTELLAR MAGNITUDE
-26-6
^^H Diialipii.tlon.
IHKk
M^-
SpecCmiEL
Rdnturlu.
1 SiriuB
h. m.
6 40-7
-16' 35'
-1-58
Sirian
DtuuT ; iAtp)ltt<3 af vm.
1 CdDOpilS ,
6 21-3
-hTZV
-o-se
Sma,u-aDUr
IrmnAlhlKi parHll^s.
a OiitAUi-j
14 32'a
- 60" 25'
+ 0-06
SoUr
Ciaia^liaiit»OfO'3i^Ulil I'CliA.
Vega
18 33-6
+ 38M1'
0-14
Siriftn
Ca]iclta
6 &-3
+ 45" 54'
0-21
Solar
Spwtmcoi^cally eompCKmd..
ArctnruB .
14 11-1
+ 19' 42'
0^24
Solar
Rig«l
6 0'7
- 8"!9'
0-34
Helium .
PTocyofl .
7*4'1
+ S"29'
0'4S
SirtAD-SDlftr
Ql&uy ; utftllftfl of ISn.
^_
Aclienual.
l$4-0
-57' 44'
0*80
HuliLin
RaH brlghtDSM 'SS tlm«i wUr.
l^^^l
y? Ceutauii
13 Gfi'6
-69" 53'
0-86
Heiiiun .
^^H
AlUir
19 46 -d
+ 8' 36'
0-89
Slnas
BpKtmin hAxy.
Bctelgeux
5 ifl-e
+ 7' 23'
I'Oto 1-4
AotariftD .
Imguliriy TOTtoble.
a Criicin .
12 21-0
- 62* 38'
105
Helium
Otnnt^Jnei two tf\VMX starK.
Aldeljwftrj
4S0-2
+ 16' 1»'
1-00
SoUr
Pollux
7 39-2
+ 28" IS'
1-21
Solar
Spica
VA 19-9
-lO'SS'
1*21
Uel ium .
BpActTOftCople blniiry.
Auures .
16 'J&Z
-26' 13'
1-22
Antarisn .
Ccnnpanloa glvci t SIHaIi
Fonmlhant
22 52-1
-30° 9*
1-29
SLrian
a Cygnd .
20 38-0
+ 44° 65'
1-S3
Sirian
InsenKlblB puvllax.
10 3-0
+ 12° 27'
1-34
Helium .
CruoiB .
12 41-9
-6ft' »'
1-60
Helium .
linClcui't "oxjKiin itu."
OftStOT
7 2S-2
+ 83* 6'
1-5S
Sirian
CompoDADtB '9'flk kwl X^afiB.
1 y Cruoia .
12 2&-d
- B6' 83'
1*60
AtiturUo .
^1
e CAais Mnjaris
6 54*7
- 28° BO"
1-es
Helium
^^^H
* Urate Mnjoria
12 4fi-6
+ 66' 30'
l-fiS
diTiau.
^H
BeU^triz .
6 19-8
+ e'lfl'
1-70
Heliuia
1 \ Rcorph .
17 20-8
-87' 2'
t-71
Hfllium
4 Carina! .
8 20'fi
-5»"ir
T74
Solaf
Spectrum cou]]iQ«ilA
* Orianjfi .
S8in
' rw
1-76
Haliaiu
■ ^ Tfturi
&20-0
+ 28' 31'
1-78
Helium
^ Catwet .
12-1
-69' 18'
1-80
Sirtui
A Triaaguli
Ifl a8-i
-68' 51'
1^88
SoUr
Australia
' See ^arrartf A%luiU,
ToL xlviii. t
ro, <t
^
377
^
HPUP
^^m^^^^^^^^^
^^H
378
THE SYSTEM OF THE STAES ^H
^^H
^^V
DwUeuttoo,
1900.
IHH.
1U«,
Qpsctm^k
1
BivrkL ,
Or P^rani .
t OriootB. t
q Ur«e Mftjoria
7 Oeminnrmn ,
0. VtBob Maoris
r Sftgittuii
£ Qaais Majona
j9 CflDifl Majoris
h.. 1A.
$17 -a
fiae-7
6 31'fi
len-s
7 4-3
8 18-S
+49* 80'
- 2" Q'
+49' 49'
+ 16" 29'
+ «a:^17'
- 26' U'
'17°54'
1*90
1-ei
I'Bfi
l-«9
3oUr
HflHoffi .
Helium
SoliLt
Sirian
Solar
HaliuiQ ,
TABLE II
i
EEPaESKNTATTVK ViBIi^LK STABS 1
X. LOKO^PERIOD VARIABLES '
Nune,
H.A.
Mai-.
P«r)«d la
Pa/i.
VtrA Oati
h. m.
- 3'*2«'
1-7- e'6
SS2
J
of rally- -20^ from t
H
V OrioniB
5 40-9
+20" 10''
ee-ia^s
a75
Symctrnta tbird tf
brigh:^ H-Unu at □
S Qmna^,
9 29-7
-arai'
4-5-10
310
Koberti liude aa ii
Ij) th« periot] com
■bQut Ss yean.
H Kornue
16 28-S
- 49" 10'
7 -11*6
471
Bi>coadu7 maxliiiia «
nik 9b«ej-v«d by In
X Cygni .
V Del phi Ei
19 46-7
20 -13-2
+ 32" 40'
+ 18°58'
45-18 &
T-a-17'3
404
G40
Period slowly leuKtb
Bant?^ ol magnitude t
lutQ<rD.
2. IRRKOULAS VARIABLES
SDoradOs
6 18-9
-69' 21'
8-2- 9-8
In cluster N.O.C. 191
tnun first typo wi
H-Usea.
i;Gariiua .
10 41-2
-69^10'
-1-0- +7-7
At a constant minin
IBM.
R Goronffi
Borealis
16 44*4
+28" 28'
6 •6-10-1
...
8add«Q tUlorsB of U
this star at nnoe
tMTvala.
u HercnliA
1718-6
+ 83" 12'
4-6- 6-4
...
Helium apaetram ;
lines. Badialraloc
Tsriable.
RScttti .
18 42-2
- 6° 49'
4-8- 7-8
...
Spectnun aolar vlt
Unea. Radial T«k
stant at +42 1
seootuL
EWCygni
20 26 2
+ 39" 89'
7-7-10-6
...
Spoctram probably
of IbQXta tTps
(BiplnX
f^\.^
■ 4-:>^'
^M
^m APFEKDIX
^^^ 379 1
^■^
8. CEPHBID VARIABLES
•
^^H NuDfi.
R, A.
1 000,
1H».
Banga In
PSTiDdlD
WevuTkat
^^V
II m.
^H Lepam
4 53-0
- 2r22'
9-040'0
13-9
Rite very nplA, P«irlo4
^"
It Muacn .
12 30-0
-ea"52'
6-5- 7 -a
0-8
SpMtrtua voUr typo.
1? Bagittui «
17 68-8
- ar S5'
4-8' 6-1
7-6
i[ntii"ltli1iH!it-chuiR&r Sub-
*liliiiry [H-nijil of a84 linliv
If Aquilie .
19 47-4
+ 0M6'
3-7- 4-6
71
Diioyvvnd by Plgott, 17B1.
T Vulpecolfe .
20 47-2
+ 27* 62'
5-5' 6*6
4-4
SpHitnMOOfiic biBMxy (rniat}.
i Cephfl) .
22 25-4
+ 57" 64'
3-7- 4 8
C-3
BpaotroHoplG binarr. N'od-
ecllptilDg. SpHUum wlmr
type.
^
4. GEMmiD VAEIABLES
1
{" Oemiuonun .
6 68 -S
+ 20*" 43*
sa. 4-8
10-2
Non-eoUptttiig bUunr. Doable
perlodlclliy indlutod (Ctatop.
V Puppla .
7 fi6-4
- 46" 68'
I'l- 4-8
1'4
8 AntUie
a 27 -e
-28Mr
e-3- 6-8
0-3
SirlAii-HDlar spectrum.
'W UrsFE Majoris
36-7
+ 68' 25'
7 -ft- a-a
0-17
irim (UUllor Hid KMipf,
^ Lyre .
18 48-4
+38-16'
3-4- 4-L
12-9
BnliiuD BpecLnim witli nui&blD
brltfbt llD«. Dottble pAHo-
dliJty.
V Valpeculm .
20 32-3
+28' IB'
a -3- 9-7
767
UEbt-dlKU« uulogoui to
5. CLXT9TER VAHIABLES
•
Ko. 8 td Gentami
ia20-8
-48' 67*
12*8.14 -3
0'S2
oftbQ^natwiit'berDcltistar.
of Qh duraliun.
J
Ko. 7 Meui^r 5
!ft l»-fi
+ a'27'
lS-6-U'»
0-60
Bltuat^v) In Uie globolAT cinih
^InLibn. UtnimatulMta
0-4 of iLotii parioi.
4
S Arffi
17 61 -6
-49" 26'
9^6-lO-8
0-45
RLtu to iDftilmam In 1 h. lOm.
^
YLyne ,
18 34-2
+ 13' 62'
11 -3-12 -3
0-&1
Incraufl qf ]fgbt 6ff<«U)<l In
1
'
1 h, BOm-
1
14. 1904 Cygai
20 1-3
+ fi3* 4'
10-7.11 -B
13
DfaOi:>V9r«d by kailima
1
CertHk! La IVOi.
I
Iprrcygm
20 62'3
+ 30° 3'
9-6.10-4 0'5
IUb« coDipleled In t b. 53 ut.
1
L
i
^^
i^^i^ni
^^^880
THE SYSTEM OF THE STABS ^M
TABI.E
III
■
List of Ecupszng Stabs ^^B
XkiMoratu-.
K.X.
L90a
Ttw.
Dv*.
Fluaein
—
1l nk
UOephet.
0*3-4
+81* «r
a-fi
7-0- »-2
Daia«|gb «f itn
2INfM4 . .
sss*?
+ 4I'8«*
81
9-4-12
Al«ol
a 17
+ 40' 34'
3-8
21. 8-2
RTF^rmi
sie-7
+*rir
OSS
9-5-11 D
in 1»4.
\ TADii
S65*l
+ia*iar
a-«
a-a- 4-2
FliM* IhU 10 Ik I
R C«ni« Uigorii
7 11-9
-wiy
11
6*7- 6*8
Df*ii«tt7 euoKA «i
tlMt D^ lit* flS
RuweII> ^J
TOuidopudftH
7 27'fl
+7e' 17'
3-3
»*a-u-9
C*iukl Id liOoTf
R* Papitti
7 48-5
-41' a*
«-4
I0-O.11-0
QMtlt^ or «TsUm i
1
XCaruuc.
a as 'I
-6a'63'
05
7-9- 8-7
Two tcfcht Hwn, 1
Id l*% DtidKXQ 1
SQufiri .
999-2
4i»'a4'
0'4
8-0-10-3
Ptimtkra or tihu* llA
mj-(hOae«i)ar(l
1
S Valorom
S39-4
-ii'M^
5-9
7 '8- 911
Ftan (KcajplM UK
>0^ •oLu- (Ttoa^
1
R» Veloram
10 17 a
-41*61'
I '8
lO-O-lO-ft
Dnrmtion of pSum s|
t Dnoatiis
11 398
*73°iS'
1-4
9'4-13'S
'
GwumiDiaoft.
1
fllabne .
14 6S-6
- »• 7'
2-3
CO. «-a
V GoroiUB Bo-
IC 14-1
+ fi2' 1'
3-4
7-t- t-7
DUBtflon of ph«ae
r«&|u
^0-1 wUe (RiiMll]
R Am
IB 81*4
-M'48'
4-4
a -9- 8-0
U Opbittobi
17U-4
+ \*W
0-8
a-0. 67
jean (Ctwndiec).
1
RV Ophiofihj .
ITM-a
+ 7'W
»
9-0.11 '2
i
'
EHarouUk
17 »^
+ 16* S'
a-»
71- 7-9
Two UD«qnftl *^4B
1
ptaoe la Hch pH
■
RflSftgitUiii .
18 11-0
-34' 8'
3^4
57- a-B
PMCfOd osBqwUT dir
« HOOtodazT mlnJiiiui
p
[
L,
^
^
•« est 3 c4
? ?
THE SYSTEM OF THE STABS
111
5ii£i
P
fe
^ 'b ^ *»
S
w »«
is SB
^»2 g^ SB
I.
5
g
-c -9 «
d
^
o
APPEKDIX
383 ^^M
'
TABT.E
V
H
List of Stars with sensible PAEAU.AXKa'
^
014 flf fit^r.
a. A.
Dm.
1900.
M«ff.
FimllftT,
AaUiotitr.
1
mbndge 34
3-3
+ 68' 36'
2^4
0"-l6
Piitdhord. Photogrsphy,
An were. DiffBrences of R, A.
127
+ 43*27'
s-o
0*-39
Dcaai
U-&
-e6"2S'
4-3
0*-138
Elkin. HeliomettT.
^^H
^dri .
20-5
-77*49'
SB
0'*134
OilL HelioiQQt«r,
^^H
eHiafwue
34-8
+ 55*fi9'
3-6
0''-04
ft-itchard. Photography.
^^1
wiopeue .
43-0
+ 57" 17'
3^
0*'1S
Peter. HBliotnettr^
^^^^H
sfiiopeUe .
1 re
+ E-l*2«'
6-3
0-*l3
Peter. Heliometer.
^^H
ria
1 22-e
+ S8' le'
21
a"*05
Pritchard, Photogr»phy,
ftlhaat
I 31
-57 '46'
0-8
ifm
Oill Heliomcter.
^^^^^1
tt
1 39-4
-l»*28'
3^0
(T-Sl
Flint. Diffprencea ofRA.
LdjiQi .
3 IS'B
^ 4r 27'
4*8
o*-ifi
Ellcin, Heliometer.
ridAni
4 107
+ 17' 48'
4-5
o'-ies
Gill. Heliomt'tff.
^^H
^bt^ul
4 30-2
+ 18" 19'
I'l
0*'i07
ElkiCL Holiomfltcr.
^^1
&bS4S
B 6-7
-46" 3'
8-6
0*-312
Db Sitter. Helioiueter.
^^H
bUi .
5 9*3
+ 46' S4'
0*2
o"'oa
ElkiD. Helioinetor.
^^H
»lgeux
6 49-8
+ 7' 23'
1*0±
C'OSS
ElkiD. HoHomttiir.
^^1
mrigae
39-5
+ 43' 41'
fi-S
o"-n
Schur. Micrometer.
^^1
Lia
8 407
-l6'aV
-1*0
0'-37
Giil. Heliometer.
^^^
ler. Oephei
6 537
+ 37" 12*
0-2
0''027
Wagner. MeridiAa o!j»r-
TatlQUS.
fM .
7 28-2
+32" e'
1-6
o*-o&
CnrtisE. Bpeotraacopic mea'
syoa .
7*34 -1
+ 5'29'
0-6
0"'335
ElkiD. Heliotndter.
11X
7 3ft-2
+ 2SM6'
1-a
0--066
Elkin. Heliometer,
iadel&290 -
7 47-2
+ao"53'
8-2
o'-oa
P*ter. Heliometer.
tmt! Unjoris
SM-a
+ 42*11'
4-1
0"'02
Wagner. Meridian ob«fir-
TstiDns,
mde 18116 .
B 7-6
+ 53" 7'
7-B
o^-ia
Peter. Holiotneter.
rsfe Maoris
9 2S'2
+53* 8'
3-3
0*'09
Peter. Heliaineter.
uide 19022 .
fi 37 1
+43no'
8-0
0"-06
Kavt<^y^> DitfereDC&B of
R,A,
K4i't«ya. Difierenooa of
E.A.
Elkin. Heliometer.
lOoBii Minoria
9&&'S
+82" 26'
5-6
0--06
fllus .
10 3
+ 12" 27'
1-3
0^-022
pmbridge .
S13
Dinbridf^ .
340
10 fi-3
+ 49"S8'
6-8
0*'17
Peter. Heliometer.
10 21 -9
+ 49' 19'
6*5
r-ii
K&i>^yn. DilToTSDcaa of
B.A.
ombiidge .
867
uide 2118^ .
10 277
+ 49" 42'
7-8
0*-04S
Eapteyu. Diflie rebcea of
10 67-9
+ 36*38'
7-6
0'-344
H. N. RiuselL Pboto-
gTApbiu measurea.
utdt 21268 .
11 0-6
+ 44" t
8'6
0*24
K*pt9yn, Auwen, and
Kriiutir.
D» B«ri. Uiarodeter.
51« .
11 S-fl
+H' 1'
7*0
c-io
In pTeparittg
tliis liiit recourse h
IS been ha
d to BflV'QI
'§,1 unthorities, MpociAlly to the
MX colli'ctiaiu
pubfished by Net
rcomb ftn
d KapU]
n, in The Sian uad Oroninggn
i&Uiong, So,
9, r«ajJ>4ctively.
_
_
-^
-^
SM
TEX STBIXM OF XEK 8ZAB8
Nimfr of staff.
[t.A. t>«c
«»
PnriliBp
Aothoiltf,
A-Ofciim .
11 14-8 j+e6'28'
0-0
O'-IO
Franz. H«Uoiuettt
nradWI&M .
U2»a -ana'
6-0
(TilS
niui DitfereooH
ZlMl
liaS'fl +*5M0'
6-7
c-oi
E»pt«yii. Diffm
B.A.
ORHNnbridgo .
1B2S
iiio-a i+*aM4'
BS>
(T'OS
Orooiu bridge .
1S30
Qroamfarid|^ .
1S5A
UiT-a +3S*2fl'
0^
<r-i48
EApteyn «ad othen
13 4^
+40* 49'
7-*
y-fl?
KaptayiL. Diffot
a Crueu .
13 31D
-arss'
1-0
(T-flfi
Oiil. Htliraneter.
7 Vtrginia
12 30*8
- 0^66'
2-9
<r-(i7i
H.N.Ibifoell. Phot
j9 ComiQ
13 7^2
+ as* 2a'
4'&
or^ii
P«tot. Heliametsi
§ Ceqtann
13 fie -s
-69^63'
09
C-03
GUI HHliometer.
Arcturut .
14 U 1
+19^42'
0-24
(Toai
Elkio, Heliometv
a CentiuH
14 S2-8
-«0"25'
0-OS
O'^fi
Om. Heliometpr.
Pinnil XIV. 212
14 dl -G
-20" 68'
0-3
O"'107
Do Sitter, Bclitm
Uluida 3739S .
14 G2-S
+ 54' 4'
7'fi
O"-088
F«ter. Heliometiei
AnUree ,
leas-s
-2fl*ia'
1*2
0*^121
Fiolay. HelioDiQb
If HernnliB
le S9'6
+89" r
3-0
ff'tO
Wognar. Mcridui
i Herculifl
17 lO-i
+ai'57'
3-a
0*106
LoATflDWDlth. MIc
T HerculiB
17 11
+ 3«*M'
»'4
o*-ii
W^oer. UeridJu
r' DncQiiia
I7ft0'3
+ M*16'
4*9
0--82
Wagbsr. Meridiu
A. Ob. 171 1£ .
usz-o
+66' ae'
«*«
0--35
Kr^BT. H«Uoi&at
70 Ophiucfai ,
18 0-4
+ 2" 81'
4-2
0"-168
Kr^ii. Hftliomet
Teg»
13 33 -e
+38*41'
O'U
(T'osa
Blkin. HQliometei
Z 3398 .
18 41-7
+69"3»'
8-2
0--36
livmy. Differences 1
AttOD.
SI AqnUe
10 20*2
+ ir44'
5-3
0*-O68
Pet«r. Helioimeter
r Draoouis
IQ 32-41
+ 69^29^
4-8
0''176
Fater. HBHometer.
Altur
1$4£-!>
+ s'se'
0-9
er-oai
Glkin. HeliameteT
61 Cygni .
21 2':t
+38' IB'
0-1
0^-37
Mv&n of photograpl
3 Equukl
21 9-6
+ 9^38'
4'7
0'07
■ Ibdi
31 W7
-57' 12-
4^8
0^-273
GilUodElkin, Hel
a Omia
22 1-9
-47" 27'
2-2
0"-0]5
Gill, Ri^UDmetar.
Kriiger (tO
22 24'G
+ 57^2'
9-0
0*278
SchlcsingeT, Phot
FoinalbAUt
22 52-1
-30' 9'
1-3
0'-130
GUJL HeliotJietcr.
Lftcailla 9353 .
22 50-4
- 36* 2fl'
7-1
€•■283
GilL H^^liometet.
Bradley 3077 .
23 3-6
+ 66" 37'
a-0
o"-isa
Fflter. Heliometer
85 Pegwi.
2S67-a
+ 26" 33'
5-8
0*'0H
Briinnow. Microm
■
1
APPENDIX
385
1
1
TABT.R
VI
c OF Stars with Peopse Motions oi V''9 ako Upwards
H of Stv.
190O.
Dm,
1»Q.
Hag.
Anookl
liDtJOO.
jLtnuukt,
1^243
ta. m.
5 7-7
-46" 3'
8-5
r-7
1>lieoY«T«d by RaptcTD uid Ihqob
Ar]{Hl&&(lHri« "kfitif; star "
i^dgelSSO
11 47-2
+ 38' 28'
6-B
T^-O
lU 93&a ,
23 50-4
- 36" 28'
7-1
r*-o
DUUncMs:!!} Ilght^jttra.
f»jts4ie .
23 59-5
-37*38'
8-2
a* -3
" OouH-* rtkr " in Sculptor.
de 21185 .
SI 2-4
+ 38M5'
6-1
6' -a
CobtKNiuitA 31** n|Mrt.
10 67fl
+ ar 38'
3-6
4'-8
21 557
-&7M2'
4 -a
4' -7
d« 31298 ^
11 O'fi
+44' 2'
8-6
4" -4
dftni
4 107
- 7" 48'
47
4'!
CMiif of ■. trIpLft nfibCQ.
■lopcin
1 1*6
+54" 28'
5-4
3" -8
taori
U 32*8
- 60' 25'
0-6
3^7
CompDDfwiU SS'Apftrt.
. U31S .
16 47
-15*5fl'
9-3
|3''6J
BUn Cf' aput.
. 14320
IB 47
-15" 64'
9-2
IdonUcBl moliOD.
lie 8760 .
21 11*4
- 39" IB'
6-8
3" -4
l«Di.
3 1S'»
-43" 27'
4-4
a-i
, 11677 .
1! 14-»
+ 86" 23'
9
S'-O
i*iii.
3 23-2
" 9^48'
88
S-'O
^^1
:i bridge Si
127
+ 43' 27'
7-9
2" -8
Duubia at 40* lubninj.
^^1
II. 123 .
2 30-ti
+ 0'25'
6
2" -4
^^1
de 25372 .
la 407
+ 15*28'
8-6
2" -3
^^1
nis ,
14 ll-l
+ l»-42'
0-2
2* -3
^^1
8 . .
18 417
+59*29'
8-2
2* -3
Com^QPSBti lA* ilArL
^^1
M .
20-5
-6F.*2S'
27
2" -2
^^1
de 7443 .
3 56-5
+35* 2'
8-B
y-2
^^1
B V. bn ,
5 20 4
- 3" 42'
9-0
r-2
^^1
)y 8077 .
23 3*5
+ 6^37'
6>0
ri
^^1
am .
14-S
-85"^ 28'
4-1
r-Q
^^1
ie 15290 .
7 47-2
+ 30*56'
8 2
m
^^1
XIV, aia
14 Bi ^a
-20-53'
e-0
2*-0
DDtlbtr atu lit 13". A ■Inubtft
pdoBA t obtWTvv4 by ItinOi,
■
^ ^
1 30-4
-13*28'
37
I'^es
^^H
le 681
2 S-4
^&1*19'
a-5
r-B
^^1
MinLH
39 32-6
+ 69" 29'
4-8
l*-9
^^H
-a A.G.C.
13 40-2
+ 19" 20'
9-0
r-9
^^1
9
■
t
u%
TABU Tn
8C&1B SI Swnt JjXMMM JfOVBUlB I
L RADIAL TXLOOmiB
#kOliODta
GnMBund^
«Cluiii]li4<>ri>
<L«porU
If Crohei .
« AnoTomeda .
a Phoemeia
fi Sagittarii
1 Pegui .
61 Gygni .
AldebftT&n
Capella .
7 Leonis .
X Draoonis
44
S-9
4-0
4-6
2-4
4-0
4*2
8-0
6-1
1-1
0-2
2-8
87
Sokv
Antarfanj
Solar
Heiiam
Probably
solar
Solar
-«1
-W
-fM
+69
-54
-62
+48*6
-48
-48
-44
-34-6
+ 34
+ 21
-20
+ 20
O iB| l J.Jl><|ik*
Dotannlned hj Om, 1
OunpbeU, loo. ett. Tb
of UiB ftw hdiui
known to be In i^iid
aunpbelI.Ibe.oU.
Btiopcdaky. innMlli
., Total ▼el>
latiTe to nut a c
(TOQDlO.
Vogel and OunpbaD.
H. C. Lord. Aitrofk.
zzl SIS.
H. a Lewd. TUDalb
Spectroeeopie biuuT
WrightX
APPENDIX
387
2. TANGENTUL VELOCITIES
Nuna ot Stja.
X>0.
PanUax.
VeLoclt:; in mUe*
per HCODd.
Kflii]ju'k&
ArotaruB .
0-3
QTim
267
BaHiil nlDcity = -1 &iUh *
HCODd (N«waU]|t
lAUnde 1&29Q .
8-3
ff^'Oas
30«
Gmombridgfl
laao
6-6
(f^ii
IGO
Total Tulodly in spau IM
luileA a •ootHid.
fi Cusiop«ia9
5-4
(T'loa
108
A. Oe. 11877 .
9*0
tf-'lO
S8
Z.C.V\243
8fi
a*-3i3
82
LftuillB 2B&7 '
6-0
(T-Ofli
78
Ucaille 93^3 ,
7 1
tr-asB
73
Ag Brid&tii
4-5
r-lflB
72
Groombridge
a-0
(T-oaa
71
1822
e Gridani .
4-4
tf'-ug
61
Ulude 21266 .
a-fi
0"-23S
64
£ 15S1 .
67
(T'oas
50
j9 Hjdri .
Bradley 3077 .
2-7
(r-134
49
6-0
tf'-isa
44
j* TUUOK .
4-1
(rise
43
^ UrstR MajoriB
3-*
0*'078
41
A 15-5BI cooiai at C, klLana
it9 proper niOtlo^a of l'''ia
(Ilumliiaai).
31 A{|Uil»
fi-3
(f'OflS
41
61 Cy^ni ,
a Omu
6-1
(r-37
41
2-1
(T-OIB
40
Tbiff etar gives ninrlT M4
tiiuMi tlit> ll^ht of 0T)r vmi.
HallDm spflctnim.
UUDde2I1S5.
7-5
0*-35l
40
Latande 27SeS .
7-5
o*"08a
36
La]&tid6 ISllfi .
7-5
o-'ias
36
PiiZKiXIVbaia
6-3
(r-id7
3&
Lalande 1S022.
8-1
0*-Clfl8
S&
PoUui
1-2
(r-066
34
aOLconiaHiiioiU
1-3
(f'oa*
33
5-a
(r-o»8
SO
^ ConuQ
4-5
(T-llB
£B
Groombridge 34
7-9
(T-aw
28
INDEX
hbbo, diEtribnlioD of nebuIsB, 357
AbemiliDii of llg-bt, Anmiul, 284, 911 ;
Hcular, 311-312
Abiponw, Pltlad-aaoestry, 218
Atmcj, Sir Wniiani, iolnl KiarVighi, 7 \
photagixyhic exposures, 23
AbHorptioD^ atmaipheric, 21 ; in Stftnt,
47, SO. 62» &7, 75, 136
Aduns, detection of speotroecopic
biiiirifls, IBS, 198, 222
Airy* Sir (Jeorge, 5t*Uar pumllajt, 284 ;
investigftttoii of (be aim'4 moTeotent,
306, 307
Airy, MJu, discflmnieiit a( twelra
Plf^iades, 218
AjtkflH, doublu j(at«]liU of Ktgtl, 195 ;
(letneisU of f HydtK, 197 ; nvalution
of » nebulous biiury, 204
Alcor, compuuaiLilnp with MIzbt, 201,
213, 328
Alcyone, spectrum, 59 ; mpdeni cim-
«pieQot]RneM, S17 ; ieuter of tb«
Pleiwlea, 217, 218, 219, 222» 227 ;
prop«r ERoUon, 219, 220, 221 1 actuii
brilllBncr, 221 i adJKeat avbuJie, 224,
226
Aldfltujim, brighlii^Aft, S, 22 ; ipectra]
type, 41, 4i; calonr, 51, 1 35» 140;
■«t«lliK», 150 I puraUai, 2fl7
Al«xiikt]derj ipital theory of Milky Way,
343
Al^l, A helium star, S7 ; ecUpeea, 117,
127-128; nature of ayjitem, 125-130 ;
pertuT^tiDQS, 129, 132 ^ pirolliu:,
133 ; colour, 13G
Al^l roriablea, 82, 126 ; perltjdH, 132 ;
mean dfluoitj^ 133 ; di^tribotioQ, 134 ;
npid biuriefl, 18Q; tvrO'foMeclLpsu,
191
Al SM, redncei of Algol, 136 ; of n
HydKE, 136, HO; mngnitade of #
BridEni, 130; lDngbliii:n of the
I'teiidea, 217 ; ti6ti£« of Audroiiieda
nebula, 257
itair, duifiiatloii, 2; ma^iiailej 22^
cpectmnk 41 ; panllai^ 297
America nebula, photofrraphed by Wolf,
270 ; vicinity drained of ittare, 862
Ames, bydrog«u-liuen in solar BptK:trui|i|
44
ADtlerRoa, diaooTQilea of tctnpaTary
stiLra, 90, 92; fudiug of Eridaui,
180
Andromeds, >, co1citi7% HC ; triple
ayatein, 195, 256
Andromeda uebula, early obHrratioiu,
lOi 257 ; Hpectnim, 69-70, 260 ■ star-
blaw in, 88-30, 361 ; Btructnrff, 268-
259 ; linked with the Milky Way,
259, 337 ; conatitiition, 260 ; oliliqaa
poaitionj 260-261 ; intra ynlactjc, 360-
351
AbtAjQS, third-type tipectrum, 60 ; doIout,
57, 137, 140; grwn iiat«mte, 144,
146. 169
ADtariaa siaiB^ 35, 50 ; clieialatryf 50-
61 ; vMintillity, 54 ; nou -galiutic,
347, 370
AbthelmuH^ dlAQOvery of a temporary
star, 85
AntliiF, 8, «har4£t«r of It^ht • cbaagei,
121, 126, 127
Autonladl, viflw of a pUmetary nebula^
248
Apex, of the Ann's way, 1ndicB.t*d by
Blellar rmpkcenianta, 303, 304, SOS;
by radial ireio^ititMi, 310; uhigoed
poaitiotia, 305, 303, 307, 308, S09
Aquiloe, t), n variable «pcctrC4C0pia
biuary. US
Arn, K, an ei;llp«iii« Rtar, 124, 120
Ane, S, a cluster'TariabK 120
Arctnrua, oacient idflntificatiffD, 2 ;
magnitude, 3, 22 ; Bi>ectral t-Jjw, 41 ;
titauiDm Rb^rptiOD, 45, 327; a^nitifs,
51 ; tberraal ftlKcacy, 72, 74, 80 ;
cnlmir, 135. 136, 140 ; parallax. 397 -,
linuar velocity, 326
Argelaoder, utar entimentlons, 1, 6, U,
34fl ; identity of Tycho's Not*. 84 ;
periodicity of Mitil, 101 ; li^bt-cban;^
of ff Lyns. 1^ ; of S Cancri, 180 ;
889
SftO
THE SYSTEM OF THE STABS
ealov flf Aietan^ IM ; bri^towi of
•obr kpM. M6; uirthod of IsMt
1—im SM^ S07 ; ■ — toi of viMt
otUI. lis ; MDtIm of 1830 Omm-
teUfi^ttt
AiMK % aiRDTCrr M A dMbk atar,
ISO; alowvaii of rrralBtiawi, 1£6.
171 ; T»ri«hmty, ISO
Ajrbaua^ lottiboaity of B ebnla, 380
Atla^ taalwttiv WufctMM, 219 ; pa».
itU* daplkftr. m
Allfin> «b l—lfcwii" thMX^Om of
viiWMiiiy, io». in
AaTCHk iMiottoii of Ncvn Soprpii, 8S ;
flrWii ftf Srlm «v«l Procjon, IfiQ,
1A7 ; star-pwtlLuM, iSS^ £91 ; »-
dneUoQ of BrKd]«y't dhMmtMBS, 907
BtHvy, itiscQTwj of dutv - TariiUflo,
118 ; tb«ir Uglkt-ciima, 119 ; gnrapod
Btiljr. uitlqn* rvoordt of t^a FIcUdM,
lU; daoRptioo of * itar-cltuOert
3SB
BOl, Sir RobHV ^zallat of Nota
C>vm. 99 ; of ei CjfKi, ass ; MKtch
for lar;^ ptnlUni^ MO
Balnatt. kw of hj^if wria, M
biiriQW, 4i*ciip«i« of r Orlo^ «•
UvMid. obMmttou of Som^ Sft. S8,
«», HS; of olwtoMvtaUi^ 119;
««u* iHlhln tn[iciim» 906 ; BeibvfeK
ta And JTuuati ifa« FkfadM, Si6 ;
I^Mtognpht of e1iist*n> fiS^ ISO ; of
Mbolou itux 2U, 244 ; of diffiwd
utelotUte. 271 ; of ■ p e iJmA B d
gilutfo cknd, iS7 ; dMnctiar of
^otnkr cilutant,, SMO ; d i wawiy cf *
i^nl Bobok., 251 ; « nm » te d tow**
BUnt o5 jiaig^mhaiM, 970 ; obnrrstiDa
of ■ TuiAblfl Debuik, 277 ; r*"'**^ '"^
61 Cygm*£SS
Bajrw, iiomQucliitQn of Matt, 3 ; de-
^gnaltiiiiH, 90, lOS, 196y SSfl -, Aodra-
Difldb nebolk usBotiosd bj^ 357
IMlAtnj:, ■dlleoa ■ MbaarpHdaot 37 ; on-
modLfied rmdiatiraig, 48 ; abHuioe of
iTDO^IiiHB from ipeobma, 47
B^opohky, TBnable tpfetxaaoopAc
hiB$nea^ US, 131, 131 ; nnwoo vfm-
puioa Of Cufeor, 190 ; apectroaeopk
ponllu, SM
Bcaaal, Bppt^ci^oa ofBradloj, IS ; ^0-
tntbvd motioQ of Srioi. 1&0 ; vtoftr
Aotioii of 61 Cygiil, IKS ; mMmna of
Ui« Pl«i»ltti, 219, :^, 3S1 ; Lnniti-
gatioM of ftoUMr pNiOlu. 2S4. 887-
988, 239 : dtteetioD of * pArtul
syitom, 329
BetaJgvox, dowgp*tiott> 3 ; napHak
23 : tpoctnutt. &l i caXvar, $7, 1*1,
136, 140; nrlabiltty, 10» ^ pcnlht
397; liffht.ponr, S96
Binuj lUis, daOaed. 1£2. At Dfilk
Sum.
Birmnekwii, Qittlapio of IM 9ub,B,
139; diaoovvry of Not* Odw^tt:
olmrrMinu of red otna, llOi Id:
th«ir Aggiv^tioQ bvtween Aqnikal
Cy^n^ 142
BoeddickBr, ■'■SradMHifin of ItiDc}' V»,
337
BolUnmn, Tmlidity cf Stabs'l I'*,
72
Bond, 0. P^ nl»tin lulxv of Srinnl
the cBtL. as ; Flio«ogmpliy of ddiUi
it«% 165 ; rifts im AmdromedA tuM fc
2S8-S59;azt<Btofth«farAiAtioii.Ma;
textatsftf Qrioa aeba]U,^S; catalCBV
of inclndod itan, 368
BonstoD, «p«^n] eliAnsteiutJcf of ittf •
groups, 371
Bcw, dct^rrnirtatioa of tDlar apex, 907
BoudUnd, period of Mirm, 99 ; notiw «I
AndroQinlfr btbtilm, 2fiT
BojB, mdkmwtHral eip«rimeiita cm itw-
boat, 73
Bnd]«7, sludjud ol»emtiaiu» 12, 307,
317; aotie«B gf donbla atan, ]£0 ; ol
Caxtor, 153, of 61 Cygni, IS-I, of 7
Aiutia, 1S8; ttallar panllaz, 968,
364 ; diacOTBTT' <tf tha AbamtiqB of
light, 384
Bnho^, Tydio, tempotaiT- stof, S3-&4;
raoord of Orioiuj, ?05 ; lu^fatDflal
ai Akjontt 21 7 ; Andromada QaMa
ignored by, 2fi7 ; atollir pa^OvcSSSL
283
BtMiklune, partUai oif Dnoa pUocttf;,
347
Bnabana, nugnJtadB of ^ CminB, 106 ;
Df AOntwri, 133
Braoe apactzograph, S3, 45, 321
Bnica talaioope, 34
BrflDnoWt panllaj: of Dnco xilanatwj.
347 ; nawLTt^M in ataUiir pafaUu*
293
Bnffham, dark laaia in HarctUoi di
asa
Bll^c^heIl. bn^tonlog 9f v Caring H
BartoQ, !ip«<tnim of Looped nalnla,
Bamhuo, i::htomi.tifl donbl* stan, 1 45 ;
rejectloa of wida pain. 151 ; di^
coT«ri«^ 151 169, 171. 181. 192. 195,
19S, 203, 204 ; moTtffia&ta of 61
CjT)^ 1S5 ; obaervatian of ^rixa,
wtaUitOf 1A6; critioianu of stellar
ortHtal compwUtioUk 168, 169, 900 i
qttjdmple atan, 203 ; oonataoGy in
light gf tispaihuD atan^ SOfi ; doaa
INDEX
zn
pairs in the Pleiades, S22 ; nebulotu
double htMT, 244 ; msumrea of Elng
nebala, 27ti -, vsjuhl* oebuls, 27*
ilciam, in nan aad atara, 42-44, &2, G3,
npbelJ, bydragen-linei in Mira, &Z\
ia ^ Centtturi and y Velomm, 61, fl3 j
bydiviigcn-tiiivelope of a star, 64 ; spec-
trum of Orion nebula, Q^^ 7'9 ; spoctro-
Bcopic binarieidisftoven^l \iy, 121, 13^
l&i, 196; tt)«Lr prop>[>rtioDate number,
1S8 ; tolar LrauilatioQ from iteUar
radial velocitiM, 3t0 ; jnaport of remit,
313 ; 5wlftni!»a of faidt lUrh 321
Caoori, 3, Mgol-viiriabltj, l;]0 ; llgbt-
eurvfi at mtnLmom, iSl
Cancri. f, calonra, H7 ; qttftternary
■j-stem. 19S-200
C«m;oti» IdiiH, liiacaamau. of stalljar «peG-
trogTanis, 2(^
Canapiifl, mognitadt, 3; ipMtnuiL, 41,
41, 2&3 ; inseiLStble pftnlUx, 293, 297 ;
nat brilliaocy, 293-294
CapslU, apparent brightneaaj 3, 7 ;
photometTic rauk, 22 ; spectral typa,
41, 4% 44, 75 \ bibary cbatacter, ii,
189 ; Qltn - riolpt apectrum, 77 ;
panllnx, 190, 211 ; stage af deT«bp-
loeitt, 212
CarboQ, in aim and stars, 42, 51, fi4, &5
Carbon atars, 35 ; character ot spectra^
M, 55 ; aSluitiea, 56 ; aamber ngu-
t<red, 67
CariiuEi, X, uatore of light-chaaga, 124,
126
Carime, ij, spectrum, &2, 96. 109 ; light-
chADgaa, 103408 *, aitoAtioQ, 269
Oarringtan, ditwAruiaenl of PUiduies, SIS
OauiopeiB, B, 84. Set Nova Coasiopflite
CauiopfliB, 7, gaspou.1 .tpflctpim, 69, 62^
87 J variability af Wight lities, flO
Camiopein, 17, colours, 146 ; orbit, 16'6 ;
masaas and light>pow«rDf compnaantB,
176, ne, aio
spactrftl type, a27
Caslor, apectmm, 41 ; a doubJa star,
160 : i>eriod of reTolntion, U3, 167 ;
diaURt attecdaiit. \&9. 197 ; lumi-
ncnitjr, 176 ; a double Kpectmaoopic
binary, IftO; ^pectKWWplc parallax,
1»0. 236
Oeloria, doublis annoJar tbeory of Milky
Way, 345; star-souadm^, 364
Cantnuri, R", a ibort-period nri«M«,
126
Centatiri, a, mM^gtiituilti^ 3^ 22 ; fluo-like
apdctmtiL, 46 ; obiHerred aa a dodblfl
star, 15Q ; orbit, l&S, 174 ; joiut masi^
, 164 I Quu and luiumosity of com-
paaents, 175, 210 ; «p«ctTO»opio
parallaT, 137, 236 ; aQDual [Mrallax,
287, 292 I pfoper motion, 322
Cfinlauii, fL, HpfflGtragraro showing bright
lino*. 60
C«nt»nrij hi, pftTiAbilityfif dustered cnm-
poaenta, 110. 120, 236, 237
Cephei, Ui nature of eoUpsBS, ISl ; tima-
ineqnalitiftt, 132
Oephei, 9, abort period variable, 82, 117 ;
a spectrDBcopic biuuy, 118 ; blue
attendant, 146, 169
Ceph^id Tariablas, 117, 118
Ceroski, v»rtabilitf of U Cepbd, 131
Curaaki, Madame, diacovery of variablvs
ataris 121
Cb&mberlin, Diigiu of spiral nebuls, 278
Chamberfl, catalogue of red ttan, 159
Cbondlar, catalogue of Toriahle atani, 97 ;
perioda, 99 ; relation to Dolonr, 114 ;
inequalities nf Algol, 129 ; raiiatiouj
of Y Cygni, 132
Chase, ponillaz nf Algol, 133 ; paraUactic
Hurv»y, 30O
Ci{»ro, Qolour of Sinus, 135
Clark, AlvAUr relative Ittatre of Biriufl and
the aun, 22
Clark, AWan G., Bruce teleacope, 24 ;
discovery of Sirian Mtellite, 166; staia
TFtthln tlie trapezinm, SOS
ClnattiTB, Drganio unity, 215, 233 ; mode
of origin, 240 ; spectra,, 241 ; crowded
in Milky Way, 356
Clusters, globular, lystemlo constitutlut,
233-235 ', raria'bLlity ot component
atius, ^36-237 ; diRtribution of itara in,
234 ; trariou^ty oi^uuMd, 236-238 ;
bou-ndbnlQua, 240
Ctiiat«ri, b-rv^liir, tnotlaa of confbrma-
tlon, 227-^26 i blfld and perforated,
229-230 : diTerelfled ahapefl, 231 ; no
evidflncn of Intemal mobility, 232-233 ;
aebulfir relatioDH, 240, 241, 26S, 350
ClMt^jr-TAriablM, 117, 1 18-121, 23fl-237 j
in ChrioD nebula, 268
Coal-oaek in Milky Way, 336 ; photo-
graphed, 337 ; hypothosU In explana-
tion. 347
Cocoou bebula, aitoatad in a Btar-laeuais
363
ColDur^ pbotogiapbic afFeets, 26 ; of
tantporaTT itara, 84, 86, &7. 03, 96,
141-142 ; of Incid star^ 135-136, 138,
14{1 ; of double Stan, 143-Ha, 160;
allc^gcd changM, 147-H3 ; of neibalAf
249, 364
Comaa Soli, Tariabllity of trapedum-
atan, 206
Camnion, ptiotograplia of ntbulEe, 28,
31, &9, 252 ; nebnbv io the Plaiadoa,
224
m
i» THK 8XAB3
«<K1
K»;
^t
, Z3i
S»:tfi
tatty <tf
0|^ Ci; m i%J Miilihi. ISriBS
QF^ T, fcfi rrt i rBi i ^ IM; W
■< ii|iiiBUl4»-ll»; ■mwiry h
> p«fa; IW ; 1^ rial iiiiBMiliM, 1» ;
Omi. X. •!»£«»», HI 104 ; M^H.
&BVm, lOS-lOft, 111
0|S»1» M, dilMttM •• • pH^ 1«B;
pnpv wOo^ IM, lU. SS; flffUMl
tiMlaa^ lift ; iMdu. 387-SBak 3M;
Dnqslv* dlHVfWT of Bii« be^K 2M
I/jfciniC ilifcMUltirtll a( * iwi lUr, 141 ;
tamianamtiim of " pdd dart" clBstar,
^9 ; qMctram of a hIpbI^ 24fi ;
|M^«r ibotlda of Dnw fTwuUiy,
347 : nriilife iMboiab 377. 37B. 279
DKTwfaB. Bcvma^aqsfllliriBaf 129^3(M;
eutb noon tjsttn^ 20S. 212
CrgDi. SS8
DAwea, donbla OcsultAtioD of AnUro,
1i4 ; colonn of double utmn, liJt
lift ■ ol-MrrfttioD of 44 Bootift, I7ft
Dmibawiki, coloitni of doable vtmn, 147,
144 ; obMrTRtiotu of pfttn mfabl« in
tlcbt.lS0*181
.an
■».■< ■ ■Ifc rtK% t»-tM; tf
Ml mmm mm, «7. M7. S7V; rf
jq. !«, i*iL in, iM
^•Wi-^'
IW
rtf^Maltcrel^
DB^tentef^eDiaai, 143-1 4«, l$9-1«e:
*■■ lii iwtafcifii^, 14«-ia ; «d7
UO; rtrfrifw, l&li
m, U3, 1S»>1«0 ; nWMi
U6; fiw|MAi m ■■■■ itj ,
1C1 ; ■■■■■■ I rti, 192 I QMpvte-
tMH. ICS-1C5 ; ffcnfc»ip1ih RMrii,
1M-1S7 ; ortibd nJBtirM, 1C7-172»
173-174; mmmm, I70>17»; te»^
S0» : variaUitr in l«hW ITft-lM ;
vtolntion. aM-111 ; pnpv ■otigi,
322
t>Dable nebalB, Bnnmw oa imn mm,
276
Downing iiiiiiniiiwli of tlta ByxJes, 337
Ih-aoo plsaHuT uhnla^ tiMiibl* pmxtd.-
lAx. 347 ; IwUc*! coaftknutMo. ftM,
25« ; rwlulTvladtr, 275
Draper cKtala^e of jitell&r «pertn, 21
Dreyer, obserratioa of V HydiK. 140 ;
allef^ chto^jts in ii«bat*, 276, 27d
Dumt'-bell deba]^, Lnd^tennuiftte cliarae-
tei, m ; ■na.togoqi objwtk, S&6, S5l
Ptm^i dmnn^ of fooitlk-typa speetn,
H ; i&cqvAlitiet of T Cygni, 132^ ;
obaarvAtianH of rod sUn, 140, 141 ;
of doabia lUn, 179, 163
INDEX
unlop, obKrvbliDiu at doable eUn,
autmuig, Hoan, d» 7, 11, Stf ;
photomfltric, 21 ; Cap« Pboto^rapliic,
2€, 126, 322.362.36^
jBoa and Tli«i:keray, ilatenniDiitioti of
the ffiiu'i! ap«E from Slrias und solar
Btai^ 308
Bkston, iRophotjJ cnrres in MUky W*y)
337 ; 9pur»l g«laxy> Si4, 34:i ; relation
r of brigbt st&rs to gdactlc BtrDcttim,
310 ; □ebiilBr<lutxibTitioD, S54
arhArd, «po3trogT»phic atndy of x
Cygnj, 54 ; movctiifitila vitliln Orida
QebuJa, A& ; binuy aitnre of c Auri-
gw.% 105
Bberhsri! and Hartiaum, origin of cpark
»p«utruu, 76
Ebert, uLamiLlDUl dUpeniOU ia «t«Iliu:
■.tmoflpheres, 62
Bcosutiioity of stallar orbita, 170. 173,
177t UB, l&b- QTolutioDArj sigoiQ.
cuice, 209
Ecli}i8es, o^vAn&^^le Ht&rs, ItS, 123, 125-
133 ; duplJHizate, 125, 13!^
Elduon, experirucntfl od steHiLr beat, 73
Etutn. flitctuftling bjightne^ 21 S ; rtal
ipl«fiidoDr, 221 ; nebulous counectiaai,
224
ICt'uctric&l conditioDfi in st^ar atmD->
jipbvrefl, 41, 47-48, 75-76, 78 ; indi-
cated by butded spBctn, 4fi ; Id
nebtilje, 70» 280
ElflmtliU of stflUar Dt-^it», 170, noU
RLkin, hclioitieter employed b^, IQ^ S94 ;
meMuremetitu of the Pleindw, a20,
221 : pnrall[iXe» of sOlltlicra etam, 292-
293, 297 i of utn-them itare, 294, 3i97-
29& ; meiDi panllax, 2H, 307
Ellartnann, «yftDog«i tiatuig^ io Antariui
s\as«t 51 ; apectroji^rapbic iovesti^tloD
i>f t:arbou star:!, 5b
EIlipticAl iiebiiliij, 243, 257 ; foresliorteTi-
iag, 254, 260 ; examples, 257-261 ;
rirtod, 261-262
Engelmauit, Ntm Aadromedse, 89 ;
colour ot 3 Cygni, 143
Enhanced llnw, 41, 47, 76
EqaatoresJ tfll»ao|n, ifeacribed, 15
£!qiiul«i, 3, period of rerolutioD, 16>8 ;
■pCctTascapic puraUix, 16«, 1S7, 2&4;
Bweutricity of ofbit, 177 ; opticftl
coiDpAuion, 201
E>]aal«i, e, triplo system, 107
Eridaoi, o^ mau onA ImQinosity, I75«
176 i triple BTttttn, 196 ; rapid ototion,
293
Kipin, detHtion of carbon ilars. 57 ;
Bpwtrnjn of X Cygnit 104 ; Ught-
period of 33 Cygui, 108 ; vamMllty
of a red star, 110 ; of U E*uppifl^ 181 ;
Birmingliwn'B Ited SUra, 139 ; red
«Un ib Porutti cluster, 23?
Evershed, titabiubi In dolflr promliienciM,
45
GvoktioD, of aUn, 36-37, 40-41, 46-47,
51, 56 ; coEirlittoned liy tempenitar^
77>73 ; of BtfiUar syBtcina, 208^214 ;
of rtar clusters, 220, 240, 267
Extinctions, method of, 20
Fabricias, discovery of Mira C<!Li, 90
Falb, nhape of Ibe viiiible uuivcne, 374
Fallows, magnitmie of 7 Cftriqim lOG
Farley, colour of BCuphei, 110
Feu«tr map of ^lars in M«8si«r II, 230
Feiiillcf, obHerTation of a Cflataurl, lEiS
Finlay, magnitude of 1} Carinas, 107
Fizcuu, iDoUon^tbifta of apMtral Uuw,
135
FlammarioQ, colonn of 70 OpliLucbi,
147 ; Tftriflbllity of 7 Arietis, 180 ;
anomalotis Bjovemant of f Cancri,
1^9 ; star eysteiii ia CygnuB, 329
FlaniHtecd, aIu- dcKignntiotis, 196, 201 ;
aberrationaJ ghifting of tbe pole atATj
233, 284
Fleming, Mn., BpectTograpbto dlicoreriM^
29, 52, 57, 62, 64 ; of Nan, 90, 02 ;
of M! ec)ip*Lng star, 182
Flint, rcHArcbeHi in «teUiu' pArallnx, 800
Komalbnut, Apectrmii, 4l ; p«rflp«ctira
FqwI^t, tit&uium^flutingB in AntarUo
Htars, 51
Prankf, colonrs of 70 OpbiutiUL, J47
Franz, pBrallaX of Noirtl AudrODiedl^
SO
Fraunhoftir, O'bjective piisni, 2$ ; in-
stntmeotal refmenient*, U66 ; S«nigi-
b«rg beliometer, 239
Frost, »peatrograKt of Nova Geminorum,
05 ; bctium it&rs. aa clote bfniulM,
169 ; radial 7Tiotion of f Cancri, 200
Froal and Adanj?, sp«clrngT*m of
Arctiima, 4Q ; Bp«cLroaCopic fiOtD'
poneut of 8 Orionia. 264 ; low
TQloatiea of helium ut&rs, 321
Galilflo, observation of Nova Serpentarii,
84 ; BtflUar parallax, 232 ; coiiipaaitiou
of the Milky Way, 333, 341
UsMcns BtATs, triple ippatrs. 58 ; (Irrt
reeD^itiotis, 5B ; iipectral rariability,
60 ; nature of AtmoAphero, 01 ;
eETecta in, of dispernion and aoomalous
refi-acU&ft, 61-02 ; priatqaLic ffwwepa
ffir, 64
Geminid variablefl, 117, 121, 125, 12fl
GemiTjomm, f, a apeetroacoplc binary,
121 ; dlaturbuu of motum-canre, 1(12
Eaw
THE SYSTEM OF THE STAES
OwniaannB, % leng- period inulkl>l* wiil
■pw Uw uo p to biuur, ISiaaa. 103,
1»7
QUI, sir DtTid, pbotogT^pMc n^tra-
tioB of «lan, fi ; tb4 auo'^ ttellw
mignftniffi S^ ; n model wjIat «Ur,
4fi i •p«c|jiua of ■^ CiHdb. 83, 10S :
lM«tngism o{ ft Pfaoniiiru, IBS ;
[Motognpli of 47 Toooui, 337 ; eiu
plormiat df Uie hAliouiBlftr, 289 :
pumUftUi of ■oaibara sUn, S02-£»4,
tt7 ; ftTsnga pftTnUax, 294 ; roUUoa
of bright vtan, 391
tifllu*. rnloar of fl Curins, 107
(lla>i!Dapp, compatation q( iteUar orbits,
107
Ooldiohmid^ nobnloas oonditira of
FlviadM, 224
OcoilndEe, vsmbilitjr of p Ljms, 122 :
edipffc tLeoo' of M^l, 127
Qmv, ihe mn's fltdtar mx^itadct SS ;
•tellftT orl^its, 147, 182; up«ot of
8& P«irui, 171 ; iiiuibi%btD«tf of
titiurles, 176 ; ealiiii&t«d number of
Uw cUiH, S63, US
Guthudf tp«ctr^ni of 7 Ciusiop«i4i^ 60 ;
pbol^npb* of ucbulie, 250, 2&3
Qoalil, UruiDiiicLry, 1 ; viLria.liiltt]r of
R NoruuB, 104 ; obaerratioiu of nA
Bian, 140,141 ; pbotogrApbicmttunre-
mput of Ibfl Pleiades, 219 ; iirift
Roathem ttmn, Z2'i ; luperpoaod
gftluitB, 547 ; belt of bright it*rs.
36S
Oroombridge, ctnumpoUr catalogiui,
308,817
Groombrif^ 1S30. proper motion, 322;
ft nuMWAj ffUr, 325 ; spectral type,
«a7
QtiWj, roocrd of Not* Audntmed*, 89
Gutholck, periodicity of Mir», 100, 101
Hkbn, central itftr in ring nebula^ 2&1
Hale, double'slit mfttbod in soIat photO'
g^^phy, 4? ; hoIa? flocculi^ 43 ; cyABO-
gBD in Antwian rtini M ; tp«ctro-
gnpblo izinftti^tdoti ol cubaii Btom,
CS; their ftffltittl«o^ 6ft; r*v«rtaif; in
metallic spettm, 59
Hikll, A., pontltx of Nova A&idroiiitdiJL',
89 ; cntalognH of Htars In Pmaape, SSd
H»ll, Maxw^l, sprwd of Meropfl uebulu,
S24 1 blemuto of ftideruJ eyit«m, 308-
S89
^lley, absorrrtiona of wbol*. 10; of
ctufton, 230, 239 ; niiignitqd« of if
Canoit, lOa
Harding, biigbt and fuut aectloDj of
ring n«bii)at 25A
Hbrtung, outburst of Not* AndromfldjB,
«9 ; callpwu Of UZ Cygni, 1S2
Hamrd FhotoaMtriMt 31; ■paoBo-
sr*phi« MumyA, 2S^29
Hois, flAr-fittuni«tmUoti, 1 ; higb ni Iw
tnvKUBB of Mir*. 100
BeU«al Debnlo. '2i8
HftltoiMter, Yal« Oollf«eb »0, SHW;
*d&pt*UMi to phvUmUo iiih
289, 296 i Kooigsbcfs, M(^ »l:
Cap?, 293
Helicm, ft terresttul cletnuu, X ; a^
jorptiou in Btsn, S7, 47 i tmjmm
66 ; variaUo bright line, W ; io*
nfrHti«9 power, 63 ; pi—il s
DcbslK, 67
Hethllii-slar& jreceoi diBcrtminitioiw 8C :
Dflbalar affinities, 3«, 46, $& £0;
mbvorptiria feAtima, 37 ; gmUcCic «»■
d«ti»tioii, 37, 347 ; eubanettd sptctat
Uneft* 47 ; emiasiw spectrm, £9, 80 : «
taaporary appmritioii^ 9ti a* fchfrn-
Tftriablo9,I83; ■■apectratoopie bovrti^
1S9; TcmotmMB, 299, SW; omit
linoar TvlocLties, 321 ; gBUeUfi em-
dwuatioa. 347
Hfttmert, catalo^e of stars In U 11. tSQ
Hettdenob, phrtllax of a C«iUaH, 287
H«lu7, Faal and Prosper, photcfn^it
tdoHope, 25 : photography of doabli
•tan, 18€; of tbe Fldadtt^ S19;
dLscorery of Pleiades oebuke, 2H
Herenlo^ cluster in, eentr^ eoiidjSUft-
tiOD, 9^i ; dtBtnbiition arul ntimbtf of
COCDpOOOIlt*, £3^ 2^9 ; Sulraiiaed dic-
tancc, 210 ; spectruiu, 241
HercuUa, a, flated ■peetnuo, iBS;
TariabiUty in lii^bt, 109 ; gptoi oooi*
pmuon, 145, 178 ; their fflwt*™
proper motlob, \6B ; ftpuriooa ptmllia,
S9S
Hvrcvlia, 95; colour obim^ 147; ft
physical piur, IfiS ; nlatlTo fijd^,
171
Hfirachel, Corolinft, atteadant to Aiulm-
mflcla Dtibula, 35^, 259
Htjnscbel, &iJF JobTn^ stfUftr DomeiHslatart*
1 ; oatbunt of 11 Cikriii^ 107 ; rvAaam
of stftt*. IS7, 143 ; coloum ofy Leonifc
148 ; of dfi HnculiA, 147 ; disturbed
uiotioQ oF 70 OphJacbi, 155 ; re-
rctatiolu of t Cuicri, 199 i nebolom
doubJe Htara, 304 ; deteoitoQ of dxtb
trftp<BimQ-»tar, 305 ; coafonnition of
clQst«n, 229, 231, 235i, 337^ de-
scriptions of clusten, 330, 2M ;
mejuiurentcnt of jvirBtled cloftter, 332 ;
laiimbct And dyntmieftl MUkditioo of
gLobubu- cluat«r«, 233-235 ; varietiei
of nebubB, 24&, 249. 251, 252, 2fil.
262 ; aatelUt«-st«r«, 2^0, 278 ; Wbiri-
pool nebula, 253 ; doublfr nebul*.
2&4 : dumb-bell, 2S8 ; ecpoct of
INDEX
395
Orion uebulii, 264 ; nebula in Ai^,
S68, 279 ; Omega nebula, 2€D ; ligbt-
cbacge in nobulae, 218, 2^0 ; stuUar
pftrallikZ, 2SS ;. iiyBteniatic movements
of star*, 331 ; the MiJky Way is
Argo, 33.^ ; gDJoctic Ktrudure, 336,
833, 3S£^, 34'i ^ nebular distribution,
SftS ; galactic relations of a claQter,
Sfi9 ^ nuetbt-r of tUe aUra, 362 ; belt
of bright aUia, see
HflrftcLel, Sir William, observation!) of
naliulB, 11 ; iiUnetary aebulie, ti5,
24S, 24fi I maxlDiam of Mira, 99 ;
variability of a HsrculiA, IQO ; coloufH
o( Htars, 137. U3, 145, 148, 1-17 ;
diACoveriei of dopM« •tare, 151, JCfl,
196. 1&7, 193 : t^triori of Cantor. 1^7 ;
lnagnituiJ«y of 44 BooIlb, 179 ; donbU*
trtSle star, 203 ; arrundteoeiit of stars
in diuton, 229, 230, 23& ; cluster in
Fenea^ 2S1 ', components of Her-
cules cl'usber, 2i^ ; ntibnloua Btar»,
24S, 244. 245; riBg-Behyfw, 262;
diffuMd DBbBloi^tit^. 267, 270 ; Omegn
nebula, 261) ', touiBta and. Dtibulte, 27'2;
Variable uflbulte, 278, 279 ; mv«it)-
g:!Ltbn of the bqu's moTeoient, 304,
»05. 306 : syBt«liiintLc parallax. 313 ;
atmctim of tbe Millcy Way, SAfl. 13S.
340; due-theory, 340-341; '^hole"
in BoorpiOi 342 ; replAceiueut of stara
by nibulie, 352 ; conatmction of the
hMTBDs, 300 ; atar-j^augBS, S&4 ; Inter-
iiyntematicAl Htars, 370
HeTeliiia, d&iignation of Mira Ctti, 99 ;
rccorii of R Cepliei, 110; abHrratioD
of 9 Ortooia, 205
Eliggena, coili]ur-i;hanga of 95 Euvolia^
147
fiind, erlnuon tint of R Iieporia, 67,
140; obHrratlanB of effati Norss, 84,
S& ; diacovery of Nova Ophiuohi, 65 ;
variationa of 8 CAnerU 130 j ohserva-
tiDD of a colour- vnrtaliln, 141 ; de-
tection of n varial>la nebula, 277
Eipparehnsj star deterraisatifjia, 12 ;
Mw btar, 62 ; duster in Persuu% 231 ;
ao uDtkii of Antlmmeda oebula, 2&7
Bp^Qt, diatauve of Atar-vytftem in Ursa
MlJQT, 32S
Hold«Ttr atudj of Orioa nebula, ZS ;
■MloDftt oif double Btara, 144 ; atellar
^roup in irifid nebulai, 207 ; beUcal
bebulK, 243 i stmctura of Satum
nebula, 250 ; stars in Orioti nebultt
268; type-uurve of nebuliBt 2/4;
tt*inil<iafl effetta in Milky Way, 339 ;
atiLr pwtterDB, 372
Holwarda, light-chnnge of Mira, 93
^odke, twinkliug of «tars, 4 ; duplicity
of y Arietiat 160 ; obserration of fifth
trapeziDm-atar, 20& ; ccuut of tbe
Fleiadesi, 218
nniigh, (luatemary atettar HyAteuiA, 203
Iloiizeaii, visual cnuuieratioi}, cratjkra, 1 ;
dtudy or galactic Umiiitwity, 337
Hug^ina, Lady, Bxtthcial i<tu-palt«rBS,
372
Huggina, Sir WiUiani, nieaaurement of
radiai inotiDn, 18, 29, 194 ; q«« of
dry pliit«.l, 23 ; Jaiutueas of bebulru,
27 ; apoctTogTaphiti mbthoda^ 29 ; dis-
covery of hydiogBD - Miiea Id wbit*
fftars, 3S, 39, 40 ; spacti^nuu of
Aldebaj-au, 45 » Apactra of AiidraUJifida
n«bula, 70 ; of Nova Coroimi, 8& : of
Kove AnilromedK, 90 ; of ilercul&s
dtttter, 241 ; of Draco plmctAry,
247 ; eiperinjent^j on Btelliu- faiJAt, 72 ;
inventiou of ntiectmg elit, 148
Elugginih Sir William &ttd Lady, Alluof
Stellar Spectra, 29 ; calcittlQ In the
iiun» 44, 76 ; deteiraiuatidn of Qhicf
nebuLor lincj 6fi ; spectra of Orion
and Andl-ooieila uelmliB, 67, 260, 264 ;
nltra-TiuletstHllaripectra,??; apectro-
grama of fi Cygui, 1 id ; spectroflopi'U
oompoaent of 9 Orionin, 206 ; wolu-
tioiLAry oS'ectB df gravity, 211
Hnmboldl, first view of 47 ToucanJ, 237
Hiitney, period and maas of S Equulei,
166, 169 ; elementa of the AyKtoni,
177 r apectroscopic paralbix, 137> £83
Hnygenn, obaervation of B Orionia, IGO ;
(leliaeation of Orion nebula, 864
Hy&dea, diaKction Into driiliit^ giDUpi,
327; rsHcbud by a galactic aide-itream
S37
Bydfogen, abeorptiTe actioD to atarii
36, 37, 38,,4Q, 41, 42, 43, 44, 47, 68 ;
In tbfl sun, 44 ; cosmic, 37, S9, 47,
03 ; rliytlipjicftl Jipectral series, 38-39 ;
eini!»ioi] iu vftriable^j, &2-5a, 79, 102,
104 ; in helium stars, 59, 60*01 ; in
Wolf-Baypt etara, 63 ; in nebulaj, B6,
67, 79 : in Novffi. 85, 67, 9i, 9&. 109 ;
low refracUvity, 62
Innes, invi^tigatioD of variable itan,
104, 105. 120, 126; del«ctkio of
quntemwy eyatems, 20^ 203, 3A0 ;
variabiltty of a nebula, 279 ; a swiftly
uioviQ^ ntar, 322
Iron, absjirption in aun, 47 ; in Amtmiiin
and earbou stnrt, 52, SG ; emleiiaii ta
Him Cet), Ui
Irre^ilar nuhalw, 243, 2!i7, 270 ;
capriciouA romut, 2132-264, 2G9
Jacob, mnrementa of 61 Cygnl, I6G;
apurioua parallax of « HenvIWi 39S
396
THE SYSTEM OF THE STARS
Jtooby, photop«]dUc oomptilnoi of iht
PlolailM. 210
Jummh, daoMa-sIit incUiod Is photo-
JubtlMD, BUgDitUcl« of q GuiuB* lOA
KtlMT, ooltTOZMiliBiig* of Anitnnu; 196
Kjqjiajn, qiutitr of gnUctio stara^ S6 ;
D«liulMlty rcund Nov% pBrwt^ 91 ;
datMlJon of T«mbte sUn, 126 ;
meridlui obaarriHoiaa foi «te!lu'
pumlliuc, !Z98 ; pftnLllAZ KnA migiii-
tude, 290 ; tnaitiDeiit of proper
itiQlioaa. 806k XS3 ; JioUr Telocity,
309 i ■*'■**""— aiwl proper motioiLS,
^VK i2X ; k Awift lUr. 322 i tatan
KajHT, waTfl4eDgtlu of bydrogwi-luies,
S9
Kaiwlai, dMorltiSm of the r]ekd«s,SlS
KavIflTi pltolofn^jliic nebuUr sorrey,, 11 ;
photcgnphjc Df uebiil»,. 31 : thetr
eblc^ RjxictnLl linciik 6& ; Iholr cleotriiml
glow, 70 : prevJent splnUity, 2M,
844; thtir rAduU maveiueutfi, &7fi< ;
j^wiagrmph of Hlnd'a nebutu, 277
SkiIb^ Lord, trrartutivfl power of tbe
Odfltttl world. 3fl&
Hepler, iUj of 1604, SS, 84 ; diflUnca
of tli« ■tui, S32, 3^5
100, 209 ; CDDrorniAtJaQ, U€3-26f^ ;
•Mming; ch&Q^ '27^
Klreh, TMlAblHty of x CyB^i ^^'-^ J
obMrr&tiou of M 1 Iv 2*29
Eirchbori Law, 61
Eleln, clircinuitic period of a T7m
H^otLa, 136 ; ahap« of «dcre*3 vorld,
374
Klinkerftiea, rtellaf tiriAbillty^ 111
Knorre, ■colour-peiueptinn, 137
Knott. vambilUy of U C>-giii, 183
Konboly, ip«H3trat flactUAtloos of y
CauiopoiK, 60
K'tivosligethy, colonr-chuiifi or a Ume
Majoris, 136
KnlgBT, cmUIo^a of »d at&m. 13I» ;
pRraUues of raf^dly - mOTicg start,
n
Qle, Kutliem DfibtiliB, 10; tnaguL^
tode of q CiTUUB. 306 ; of ct Centauri,
1£3 ; at&r osUlogue, 817
LiUodB, list of red slara, 13B ; notica
of tho Draco planeUry, 217 ; itm
obffflrrod by, 317
Umbflrt, UUky Way, 331
Ltwt, Irw of qoolinff for gBawiiJ bodies 77
LongeDbkob, teiDpoTature* relatiotu of
liaO'SpactrA, 70
iMH^Djr intUtip>l« atb m trifid a^bak.
207
Laplrbos, tUrk atan. Iff A
LMeell, cluster in GeniiBi, 228 ; obMCi^
tiou of Dflbobc, 2<fi, 349, 398
l^a and Wirtz, ooltmr-cfeiuiee of s V^
Hvoiix, 1S6
Least iq^tana, principlfl of, 3D5-S46
LuvitS, HIis. detoetioii of nrUble lAm
e7» sea, am
Ejb Qea tfl, Lttfrndut to AadiOBiit
nebula, 253
Ijeowitz, apocryi^ial apparttioDa of Ibfa
CassiopouB, 34
[jeiris, nlatrra mjiiuM of binary iln^
I7fi
Ugbt-9qutioo In itaUmr orUta, ISS^SSI
Light-pTounn, effect on Nora IVn^ M
Ligbt-rmlio deSned, 19
liindianr, obflerr^tioD of Novft fTjHiopiin
8i
livuingADdDewu, l£biper«tarecif tlcetik
spark, 76
LockyoTt 8tr Nonnon^ bellTun ia Stan*
36 ; ea1iHic«d liset, 41, 74 ; Aataria
stan, &0 ; nebulai' ^lectram, 45;
nltn-virilAt Rtallar spaetK*, 7S;
temperatares of th« sfaus; 78 ; nd-
ablca n^ardod u Hiuuiei, 111, 1^;
conititatjioik of Andromeda. Dcbnla,
260 ; coTOAtUT aflbiltua of ncbnlsf
272
Ijixrwj^ estimatad moniber of djiartad
stars, Zm
LoliBS, J. G,, ttiap of Btttw nui Koti
Cygni. 88
LobacOHelamBntsof SirUnsyBtem, 156;
uiTesttgation of clufitcr in Pfli-Beai^ 2Si
Loomii» period tttnbat«d to ^ Oaiinjt,
107
Looped uebala, apectmm, 69, 363 ;
upect, 262-263
Lodendorff, poriodicity of « AuHgKv lOB,
jn
LauL, spectrogTani tit a. Fbcexiieta, 1S4
LynB,^ vjmible bright lines in apectram,
G9, 60. 87 ; ligbtcbangis, a2, 116,
122-123, 126 ; aaalc^us ol^Vfa. 123
Lyrm,€, qundmpleflliu', 201*203 ; origiBf
214
M<:Clutt, distribution «f belium itan,
36 ; oiyg^xi in stars, 87, 64 j apwlw-
gr&pbic appamtDS, 109
MaJler, disturbed ciwulaticn of 70
0]ibiuebJ, lEi5 ; l)ypoth«tLi»l ptLtatUz,
172
Haaitlin, oli«ierTn.tion of Notr Serpvn-
tKrli 84 : duceniincrit of Flaindea, 21S
Ma^ljuiic douda, Wolf>RAyet stitn oot-
l»Ct«d io, 64 t v&rUbU $tu% 119, 134,
INDEX
397
Bystemic unity, 351-S52, 3C7 ;
ab'itlM' connectLDna, ^63 ; couditi'Oiu
neflium, ■ caoatitaect of iUra, 38, 10,
[C2, 60 ; gnben. flutiog ol, 65
Bitude, of atan, 2^3, 19, 22
ougnituilfl, 218 ; rul brlUiiuiCT,
F'S!21 ; apoctroacopic untallite, 222 ;
■ttftchMl UflbnLe, 224, 225, 2&2
HaIb, pwnUlH of €1 Cygni, 2SS ; wlu
Mariotte, blae itara, 143
MArtua, hrst telescopic obserfAtioii of
AtnLrooitd* ncbalK, 2&7
Marktirick, iukxuua of UItk Oti, 100
MuioD onrl Smith, obaervAtioua at tlm
trtfld nebula, 250
MftS^'brightaesSt of biimTiea, 178
Mvsaas,, of binary tUra, bov detericinAd,
170 ; ns-aita obtakted, 171-172 ; rela-
tive, 1712-176; cpnditioDBof ucertain-
Baout for spectroscopic pairs, 190-lBl
Maimder, galactic clui^tcrisg, S36
HAarolfA^a, obserratiQiu of Nova Caasio*
peiffi, 81
Maarjr, Mi^, iJUdlvioo of tteUv «pH-
trograois, 29 ; «volat)onu7 aeritit, 97 ;
couipofiito spfctrs, 148 i Apdctniacopic
duplicity of ^ Aurigsa, 189
Mayer >, C.^ colours of double sthis^ 1*3 ;
debectlDa of atolUf uOtiplM, 106, 106,
1»5, 202
May»r, Tobia*, di™ion of fCancri, 198
Me^lowi. parallax of a Cectauri, 237
Meridi&u photometer, priuciple of, 20
M^Tope, magattnde, 213 ; ailJ&uKttt
nebulic, 223, 224. 225, 226, 265
Mcuisr, obaerratioiu of uebtilns, 10, 291,
26B
Moteofitic bypotkenifs U, 111, 184
UiisUelL, rod etm, 136 ; Dumber of tb«
Pkiivlm, 318
Micrometer, described, 15
Milky Wny, a collectiau of stir-gronpi,
9, 340-341, 351 ; qunlJty of liglit, 26,
347; conceDtratioD io, of bt>liuin st«TB,
37, 347 ', of carbon stw, 60 ; of
Wolf'Kayet aUrs, M ; of gaaeoQu
nebalK, 65, 3fi6, 35S, 359; of t«m-
poraiy atara, 63, 90 ; of sbort-period
rarUblfiH, 133-134 ; of cliuUre, 228,
231.3G&,9S8-3&fl; unrelated todoubie-
Btor orbits, 177 : proloo^ed towaidi]
gnat nebulffi, 2£i9, 359 ; Btmctiire,
2€8,835>33S,373; inflneucsupoDHUn's
coorwi 312, 313 ; iipou Atellar proffer
tnotiotH, 331^33!^; aspwt, 333 ; folk-
Ion, 334 ; track acrou tbo sky, 334>
335; dolineations, 337 ; irresolvability,
33d-33&; strAtuni-tbeory,3S9-34l ; ftat
ikg theory, 343 ', ■pinl theoma.
343-344, 343 ; cotdpQUad fortaatioiit
345, 347 i distance, ZA$ i relation to
QAbiilar (iisttibutioQ, 353 357 ; tttar-
doiLjity in, 364, 365, 369-370
MiucUlo, iaeaflurt<m«ut of HteUar beat, 73
Mini Oti, bydrog¥U-li»u.4 bright io, £2,
102 ; specLrograpliiu inreatiigaticai^
S3-54, ]l>2; a typiual i-artable, A2,
99; pericidicity. ^9-102, 112; propar
tcotLou, 133, iS3
Hitohel, divisLan of y Scotptir 202
Mitchell, Hpectrani of Sirius. 38
MizftT {£" Ursn MiJ"'^^^ ^^^ leader of
Alcor, 201, 213. 328
Moack, masfi-brightnefla of liinoritid, 17& ;
remotcue&s of whito stant, 299
Mi::tTiti^uy, acint illation of Hie at&ix, 4, tV
MiiU«r Aud Kempf, photometrio obaerra-
tious 21
Multiple starn, varietlea of oomliUiatioii,
194-195. 197, 213 ; iaviMiblii comiioi]-
enta, 197^^00 ; ^lenipecUTiu attaodantci,
AOl ; i]UAttiniar7 ^oupA. 201-203;
214 ; aebulouarelaljonsliipfl, ^04-207 ;
«Tdutioii, 208-2i4
Nobuln, early obserrnttoiia, 10, 267 ;
number, 11, 2&4 ; usociatloii vritU
bc'Iiitm'.ilarH, 36, 46 ; gaseooa tp«c-
truiP. 66-67, 245, '^47, 256, 273;
aobtiiiuoiiit, ^7, 70, 263, 281 ; strati'
acatiou, eS ; etieeiftd, 69, 243 ; t«m-
pcrfttuw, 79^ 2S0-2S1 ; fttrnotuw. 242,
246, 'l&i, 2S1, 344; colour, 249,
204 ; GomotaryjLffluitiea, 272-274, 276 ;
Hoemiag immobility^ 275-270 ; rndLat
%'elocitle«, 275, 3S8 ; variability in
liRbt, 277-2S0 ; toauity, 280 ; llitra-
gataclic atatua, 349, 362-^53, 36^ i
atellar relations, 350, 352-353, 369 ;
dlatribation, 353^367, 359 ; variety In
comitltntiou, 357
Xebulie ill the Pleiadtts, 223-220 ; fomii.
274 ; drift through space, 275
Ndbulium, a goaeoua conatitnetit of
nBbul;e, 65. 08, 245 ; jpectnim, 66,
67 ', amission by taBiporory start, 87,
92
Neboloaity, roaod Nova Perwif, 93*90,
241 ; aUut the Fletadaa, 226 ; diffuaed,
270-271
NebiiloUHi stars, flnft notice of, 243 J
aUinitl^ji, -244
NewoU, apectram of Kara Oncminonuu,
95
N^wcomlj, total light of the atafs, 7 ;
nature of tlie pebuloaity rouod Nova
Paraei, 95 ; cotnploiity of Btvlliir
ayattms, 199 ; proper motion of
Alcyone. 219 ; invMligatjoa of aclar
motioD, SOd ; ATeragtt st«llu- relooitlei,
iS96
TllE SYSTEM OF THE STARS
mi, 334 : runaway it«Uv«pw*i 3S& ;
■ur <lrift LQ UrM Mijor, 328 ; mcdid
lint of lbs Ullk; W*;, 334 : ptnlkt
of pUAcLle lUn, 844 ; t«if* 4f gilHtic
nufaitndw, S47 ; itistribnttoB c€ tlin,
3«A, 369
N*wUMi'* Uw, nnlTerul ralltUty, 170
Kiohohi, hMt of Um sCani, 7^-7-1
Kotfel* obwrvALian ^<f it Ckrtiw. 100 ; rvd-
MB of 'r CniotK, 1 40
Mow AndmuttUbk oatbnr^t. 83, sei ;
■pKCrum, 8ft, 00 ; colour, 142 ; tdtn-
giatictic (Litoatioi), 3&0-S51
Hon, AurtgiBt epectnl nlstiouibips* 02,
91, lOlf I discovery, tiO ; tKbolu
tnuuformation, dl-92
Kora OunopaiKt 83-91 ; soloar-cluuiga,
l«l
Von OukUati, 90
Kera Ooro&Bv ^^-Sft; oolobr-chaugih 141
Korlt GTfBi, SO-!)S ; coMr-ehange, 142
Kova Oeamomtn^ #5 ; colour* 143
Jivrt, Potaeli luminoua Jlucluatiau^, 92-
9^ ; ooaiiHt«il i)«buLo«ity, 03-06 ;
ooloar-chuign, 142
Olben, period of x Cypai. lOS
Omega nebula, piacemaiU dUt^crunieiit,
260 ; photogmpti, 270 ; fuajHUctod
lamtBoiu eluiD^cMi, 279
Ophiuchi, 70^ tiulour-chaogB, 147 ; per-
turbed revolution, 156 ; inasiu anil
lJght-pow«T of companieDtA, 17^, iJ'Sf,
210
Ortiibi of binary ttan, apparent, 1 &3- 165,
167 ; actual, 163 ; number computed,
l$7i 160 ;, methods of [jfltermjniag
dimaiui'Oti^ ltj& ;. elvmenta, 170, tiote ;
nlativa and nparata at Dompanauta,
lTS-174; floceatricity, 177
Orion nebula, inophotal contouw, 27 ;
pliotographa, 28, 25^, 267; i|iettrm»,
66, <17, flS ; ftit«i-iinl niavamsiits, dfi,
276 ; variable Ktwt in, 134, 268 ;
"Fi»h-mouth" aipwt, 242; ^occn-
loiit teittiire, 264 ; plnn ot ^trueton,
2«5-26t] ; » d«velopin^ cltuti^r, 267,
360 ; recesHion from tbe iim, 275 ;
ateadridt lights 279 ; gtilactic coii-
ufKUons, 337, 369 ; paucity of aur-
roujidin^f stara, 352
OtioD Stan, :36. See HaliQio-etara
OrioDLB, e, Bpectrum, 36, 37, 40
OrioDii, 0, early apectral type, 37, 6S ;
eWtiufs bright Une«, 67-SJ3 ; multiple
cbaraoter, 1£>0; relation to ann-ound-
tog nebula, 205, 264 ; aucceasive
datactioiL or conipoTieuta, 305'206 ;
genetio AtBuitiu, 213
Orionlfl, ir« lnultipt« star, 143, 203
Orthochromatic pUtaa, 2S, 30, 50
Oitkoff, ntdDMB of atara, 100
OEford UmBomatry. 20
Osygva ui tUra, 37, 47, M, M ; te I
■tm, 42, 4»
Fklm^r, ■pectTOBimni of Nora pRtili, I
spectfrwcopic parsliaz of s
187 ; binary cliarftctvT ot «
192 ; compom-nts of Hvrcnka dailB,
236. 239 ; Debalax apcctroiiv 381
Paialluu uitLtul, mode of ^SetensiMtlak
14. IS, 266-i«7 ; pliotiYnphi^ A
S»a-S0O • of KoTK* SO, 04 ; of iwMk
9tu*, 133 : apHfavoDoplc. 169, 197.
190, 286 '28ft : hfpoCbeticaloffaiauiM,
172 ; of the Platadea. S31 ; of anebak
217 ; vmallnosa, 282 ; B«»oc)at«d tflarti^
S33-2S4 ; by llglit-*q nation in ftcDu
orbita, 285 ; reiulls of maaMajma^tUt
287-ZOa ; of ^actic atwa^ S44
Parallax, sMular, SOS
Pegajni, ^&, ralatire maaaea of cob-
ponanta, 175 ; optical attendant, 201
Pegaai, k, p«rio4, 160 ; ajMctsivoiae
and Tiyoal system, 201
PtfguL V, analogy vlth j9 Lym, 12S
ppjTiter, Bcintillatioa of Sirius^ 5
IVrrlDEi, Bpectrogram of Nora Aurtfv,
92 ; rpcctmin and nebula o! S<m
Perset, 93
PaiaeuB, doufcio oloatcEr |q, SSl-SSSj
aaeamed centre of »:un'« orbity 311
galactic relationship, 358
Prrsotml «quatioii, d«Qiied, 14 ; iu do*t)|
star nieasnreiueDt, 16fi
Peters C. A. F., rtdlftr parallw, 290, !
PbuaQidiv et, radial 'v«]wit]F, 186
Phdio^raphlo pl&tai, 2S, 2d, 30, SO, 6B ;
Ulaacopea. 24-26. aO-31 ; lBt«nuti«al
cbart, 26, 863 ; irradiatton, 3& ; aUltar
magnitudai, 26 ; c«talt9^M> S«% Mi,
365 i Btar-gaugiitg, 363
Photographs, of Dabola;!, 28, 81, 03-0
224-226, 251, 25S, 256, 25»-260» ! "
266, 267, 289, 270-271, 377; _
Btellar spectra, 39, 40. 41, 42, 43, 44,
45, 52, 53, 54, 60, 6S, 136 ; of Debular
a)vec<tra, 67, 70. 260 : of double atais
165-167; of UiB Fleladaa, 319. 2^4-
2£6 ; at varioua duHtort, 238, 230.
sae, 236, SI I; of nebulons BtV7,
241, 244 ; in the MUky Way, S37,
347
Plintograpljiy, etnploymeDt la lideiBal ra-
March, 22-26, 31-33 ; photometric,
26-27 1 apeetrofloopjc, 2S-20 ; radial
motioa dete^m!nl^d by, 29, 1S6, 323^
discoFerieaby, 29, S3, 52,90.92. OS-!'
97. 236, 266 ; rt«llAr parultu by,
293 ^2»e; rapidity and treraatilit;
32 ; investigation by, of nobalo
INDEX
399
ntatiDnibips, 207, 234, 242, S&0-2fil,
, 254, 308^67
' olaiueter, poUrigiDg, SO i vedge, 20
hotoinetry, stellar, liin and loape, 19 ;
; metbotii. 20 ; resultA, 21-22 ; photo*
graphiK. 2;5-27 ; nebular^ 27
>ipili«f«, AID «sKntuU f«»tare al nm-
riik« bodieA. 34
i, fltar-cBtiilogui.% 317
kerin^, E. C, Harrard photoiratryf
I ; mtXaO^phtFK |.bsorpt.iDn, SI : atiu'i
iialtaj- miigiiLtiuk, 22 ; iiLd<2r«Al photo-
grat'ti j» 24 ; dintrihatian of the BtarH,
25 ; in the Milky Way, 3fl9.370 ; atellar
'fpectrogfftiliB, 3ft, C3 ; discovery of
coflmic hydrogao, 37, 30, 66 i sweeps
for g4««oqH itara, 64, St, 246 ; clouiii-
utiOD of variflhJea, 82, 10&, 116. 126 ;
datflc Lion of «p«ctTD«copic binnrifs,
12S, 189 ■■, invutigatioa of Algol's
eeiipMfi^ 1147, 12S; colours of 96
Hercidis, 147 ; ouua - brightnaM of
binarleu, 17B, 201 ; tlie lost Fleiid,
218; paucity of tnia Plaiados, 220;
their spectro, 223 ; countg of fltara
la globular c1uf.ter«, 234 ; utatns of
Looped DcbQls^ 263 ; photognphiQ
catalogae, SAi, U6
Pitlttriagt W, H., netralar photomatry,
27 ; photoprapliic dSEtiloRurv of gTBit
Biuke ucbulh £67
PEctor, flying Bt&f in. 322
Pigott, discovery of R CorOluB, 109
PLaticki Stefan's law of ndlati^iD, 72
Planetary nebulK, apectraui, 6&, 6& ;
Btraiiture, 66^ 246, S&d, 274 ; dimiff-
iut«d by HOTBchel, 24& ; Bpeciiuens,
217 ■ 2G0 ; imwn^ible parAllax^ 247,
aOO; ndial velouitie^, 275
FlasaniantiH, tidal tlieory of Rtellu: varia-
bility, 111 ; oecondar)' naininiBm of ^
Tanri, 131 ; iTregalaritiea of U Cephei,
132 ; galactic isqairiea, 345
Fifliadled, mythological foniu, 215-217 ;
DUiQbtir visible, 218 ; cotnmou nDOVQ-
ment, Sl£^ 220 ; ficale of ny^tem, 221-
222; nebuloufi coaditian, 223-220,
8fiO ; a typical invgtiLar claiter, 227,
247 ; forma of induded nebulte, 274 \.
connwatjon with the Milky Way, 337
Fleione, bright-lme spectrum, 69 ; the
but Pleiad, 213
Plamnifr, eiitimates of star-liiglit, 7 ;
ohMirvaCioua of Nova CaMiopetie, 81
PogHon, DbftOTTattoQ of Nova Bcorpil, 88 ;
periodicity of It Cephei, 10&, ItO
Poincar^, QgureH of rotating caaaiiefl, 209
Fol«-«tar, the " cyDOflur*," 2 ; niagnitiide,
B, 22 i ataiidard brtghlben^ 20 ; spec-
tnim, 41 ; tberratioui^ diftplacemanta,
383,284
Pond. Btellar paraUai, 28S, 294 ; wcolor
abamsLtioa, 311
FosltloD -angle of coap]e<l etam, IBS
PhEsepe, meaaarea of componvtiL atar^
233
Prey, nlatiTe maAaei of biaary stara, 175
Pritchard, photometTic inrestigaltoiw^
20 ^ sballai' parallax by photography,
30, 298 ; surFcy of the PleiadcB, 220
Proctor, Htar-drift, 327-328 ; theory of
Milky Way, 343 ; siellnr o'utbuTBts in
uebule, 350 ; nebnlnr diatribnUoUt
353. 354 ; star-alreoni^ 372
Procyon, magnlLude, 22; ^peutral type,
41, 293; iatellite, lf^7 ; liiminoitity,
158, 175; ij*rallaa:, 297; propee
mol^gii, 322
P^per motioiui, defined, 14, 316 ; of Tori-
«bka, 133 ; of double ^tars, 164, 1C8,
160, 174, 322; diiiturl>t^l, 1&6, 157,
1&8 ; of the FleiadM, 219. 220 ; a
criterion of ricinity, 290-291, 317-318;
common perspective elemtni, 304,
SOS, 322-323 ; non-tn^tUodical cbar-
actter, 305, 314-315; aacertainnient,
307. 308, ai6-3l7; aiiomalie% 318-
820 ; TsrifctioD with •pectnU type,
321 -, Bwifieift kaowD, 322 ; unwu-
troUabla rates, B24-327 ; concerted,
327-330; snraii&ed harmoniM, 331-
332
Ptolemy, Htar-inagnitiidtiiB, 2 ; ncbttlofi«,
10 ; ignor^ tf CariniE, 100 ; ni&gnltuda
of Eridaal, 180 5 Pleiad quaitatta,
217
Fnppis, U, variable doable star, t81
Pappis, V, Boppoaeil eclipses, 123
Puppia, ^. ooscnio hydrogen - litiH in
ipectrum, 38
EUdan, form of fdilereal uniTerae, 372
I^dial motion, of dtara, apetitroBcopleally
dBtemiiued, IB, 185-186 ; variabloj
66, 121, 128, 1S7. 182 ; of Novte. 91,
93 ; in binary orbits, 285 ; indicative
of Bolar translation, 310 ; of nebula^
275. 358
Radio-activity, coarnical effocta^ 80
Kaocken, galactic rotation of itan, 9^%
Ramyatil, itructufea in Odoo nebnla, 265}
266 ; tenuity of nehulic, 2S0 ; com-
poflittau of galactic duaters, 347
Red Btars, jpeotral vartfttwa, 49 ; itropg
Mir-ab«^tIon, GO, 62, 57, 140;
catiJt^iiss, 55, 138, 13d ; variability
in light, no, 140 ; in colpnr, Ul ;
eiampleg, 140 ; dUtri button, 142 j
ocoumncQ in pain, ICO ; in Persvas
oluBtor, 2S2 ; in (galactic grqupinga^
S71
Keflecting telescopes, adTaotagM and
400
THE SYSTEM OF THE STARS
•oloanilM
Bmla^ Bi^Blltiik, 3 ; aatoUtt*, 146.
1S8
ftMplcH prfaHtk dbeto of MtptiUft.
tto*. « ; tfiMtnuB of T V«tormiii. 63
JttoaML dkvMab of f Un» BUJarim IM
Btpb*Mt Am ftbaomtlm cf « Owttjori,
150
tut, %7 ; t|H)otnuD ■ai^Ml by inw'
■fanrpliA, 47 ; onitit gf ultn-riokt
ndlBtMCM, 7& : bltta atlMdnt, 14£,
lU; pu*Uu.2»7
Blag iMbalA, iiMctnin, 47 ; vfini con
ronuUom, Sfi^ fi61. *JI^A ; juiilc^oos
otijcato, 2&1-3A^ 256 ; kuhiwcUU move
Bltchey, twbtilA photogTupbiS, 31, 380
aipuLUOD of Harm Pwsei ticbdUi, 94
BoberU. A. W., itclUr e«U[)Mlv ISS
ISA ; iD«ui deiiiitx of AJgo) ttan,
12S ; ctntrv of grtvUf of b CstiUtui.
174 ; periodicity of x PiToiits, l^H
Eoberbk Unftc, mulUpl« €ip««ores, 33 \.
photognipbJ of bebulXt 31^ 253, 25S,
2C0, 2«1, 262, 205. 266, 270 ; of tfae
PlaiulB^ 224 ; of nrioiu cliuten,
SSO, 232, 23S, 241 ; of a nbaLoiu
■tv, 244 ; of ilifftued DAfaoloutia^
S« 1 ; arTVL^ement of «tui to. eliutari,
229, 231 ; v»TiaU« gtus Jn Onon
nebala, 269
Bijwu. tidrd Ear]^ colour of ■. nUr, 141 ;
■tneton of HUr-cltuten, 23B» ^0,
SS5, aaS ; Anm of Sahun netiid*, 250
Bo«Bv fonitb Etfl, double ubuU, 254
Roaidt H. C.t ta«Bfli«ia«bt of eliutir
&boat s Cracis, 232 ; cbimgo k K«y-
bolfl bobula, ^9 ; pboto^nph of tfa«
OoKl'Uck, 387 ; of Atin in Crnx, S4T
BwkII, H. N., tcDait; of Algol TorubltjB,
133
Rnlberfonlt pbotogrspbt of the FleUdeo,
219 ; of pTBKpe, 233
K^dberg, principaJ sehu of bf drogea In
8ul]or, double sttelUte of RI^I, 195
Hftfjuiki identity of Nora Cassiopaie,
S4 ; Unctiutiona of rtd stan, 110;
micettaiRtied £□ oolour-pctveptioll, 137
SfttTor^, satellite of Siriaa, 1G6 ; tvxton
of OrioD iiebulau 2fl5
Bfttara uebuln, colonr, 249 ; mibr, 2&0 ;
r&dloJ velocity, 275
Bavary, Gnt cooipntatioa of a itellar
orbit, 169 ; ponllkiu of biiuunr stuv^
28&
Sftwyarr miBimildi of R Corons, 110
Sdbtebarle, diAcovery of Pnxfon'j ooni-
puioii, IS7 : halioLl B*b4b M;
pfaoUigrsplii of Ring tnl Thimli Ml
tiebul«, 251, 256
Bcbcibcr, apvctnuB flf CkpilH 44;
rmtioaale of fan^rt-ISBB atautK ^mut.
61; >p«aibqgr^of AAdfaiBabMkilfc
70, t«0
Schupftralli, dapUcity of « Bj4i^ 117;
Mercpft setmbL. 224
Scl^*U*>ru[i, c»ulGgrtt* of ml ttm, A
13d, 140 : obaemtldfi o€ * ealio>
Tkriftblt, lil
SoMtBTiw, pufelUxaB of fiitet i4m^
Schnidl, dteonxT of Ndn Cygni 16;
nduMa uul periods of Tmn«iile ote^
314 ; minituum of S C^ocri, IM;
ootoar of AlffoU 136 ; hittory ctf T
Vlrglid^ Ifti ; &*bQlar nrubOity, S79
Sn^DfiMil, teixad of T Pnriw. M;
oolottr of K Obphn. 110 ; obHrvatlffa
of 3 C^Mri, 130; nxiafala aatofe
278 ; eoDBioii drift of ■ ttn-pm^
3S9 i pTDpar QotiiKu rrftgw i to 4h
Milky Way, 330
Schal«r, botke of Tycbo's stw, 84
Scbiir, flxJSy of itan in PnBU|Mv Stt;
paimllmx of ■ comp&iiKiB'ftu'* SSO
Sebofter, dispfnira-bypoibwa of
bri^t Unw, 61
Scbnb, pnriodidty of Mira^ 101
Scintilljition, of white iwd ted «(««»
of None, 4, 84
Sdjitillonifrtt'r, 4
Scorpii^ V, m qiut^maiy ajsloB, 203
Skorpii, {, a tr{pl« aysleB. IVT ; ooa*
plu iHRliMUsm, 21 S
Swle, oebulooitj abouX AJteytti^ £B4
8«o«hl, objMtlivB prion, 26 ; culUr
typM» 35, 36, 49 ; cwbon fttn, £4,
65, 67 ; gawooa itu«, 69 ; auu-
colomv. 141, 143, 147, 146 ; niniity
In H closter, 229 i raotralidUty of •
Debali^ 24V ; TwtecB of intentdUi
ipuo, 301 ; Kilaotio doadlat, 3SS ;
fttsr-pittenia, 371
Sea, uii^ient redn«M of Siriiu^ 13& ; dti'
tarbuce of 70 Optuncfal, I££ ; pvth
of 17 Cusiopcile, 1&6 ; comput^iazi of
rtaUar orbJU, 163, 167, 197 ; oeoafi-
triciticff, 177 ; qaiatuple stv, 195 ;
tiddl fricdoti ib fit«]liir syiteou^ 206,
209, 213
Sediger, oebtLbi round Ifork Pond^ 94 ;
lytfbem of f" Caocrit 3O0 ; gidaotk
reHUCha, 345, 365
Senoca, colour of Slrins^ 136
Sideival aitronomy, canditioii« for pro i> »
cutioQ, 13, 14, 81 ; owtbodi* 13-14 ;
ftTiLil&bility of tbe camen, 22-23, 26,
Sl-33 ; muliabla ot lifbt, S3
INDEX
401
Sidereal phy&iu, origia, 14 ; takan pro-
gress 1&
SiderenJ ny&tem, graviUtiTi power, 325,
325 ; periBUieiice, 330, 331 ; spectral
relatiotuhipB, 332, 370 ; tioite dimcm-
Biono, 361-362; org&niHation, 363-
369, 371 ; comprebeiiii'ive ^^f stats and
iicbuUt, 373 ; primitive rotation, 371
SidgresTes, fipectrum of Nota ikurigK<,
91 - of Xava rorui, 93
SUicDo, in stars, 37, 41| &i ; in the iiui,
Ftiri&n JitarB, 35, 40 ; nature of Hp^ctra,
S7, 47t 48 ; pbotograpliic iuiuftiga-
tion. 36 ; brtlTogeu -absorption is, 33,
41 ; nffinitieA, 46 ; Absence at emu&ive
fiymptoiQH, £8 ; tlfht-vaTiaLiork.s 117,
133 ; tnteQa^lmiiliiDaity, 17S ; ivninte-
DUft, 29&» 320 ; aioaU pr&per motjopp.
831 ; guJActii: cQbdetiaatiaii;, 347, 370
Sirtua, bright&«M, 3, ^2 ; twinkling, 3,
6 ; jpectrDgrami, 33, 4Q ; hydrogen
Ebaarptioo, 41 ; ultra-violet spectrum,
75 ; aaciant TOflnaBS, 135 ; binary
iyst«in, 156-167. 16$ > ma«» rolationt^,
17fi ; p&rallax. 293 \ pmpcr motion,
322
Smyth, Admiral, dlNcriinliiatloii of atar
eoloun, 137 ; UnU of y lfOoui» and
116, 147 ; Qlnator in
95 UercnliA,
QoniiDL, 22S
Smyth. Piazzi,
HercuLin, 147
Solar lUra, 3i
colODT'cliaDge of 9&
relativQ Qiimbara, 41 ;
spactrm, 42-45, 48; relation shiju, 46,
!^^ fifl ; brIgLt liiiBa nliaent from,
68; l)gbt*varifttJon.s 117 ; comparative
viciiitty, 299, 320 ; diiUclied I'rom
galactk fonuations, 332, S47, 370
^onth, colours of doublet Btan, 144) 147 ;
observation of ^ nancri, 198
^^IKutra. nehiilur, G'j-JQ, 79, 24fi, 247,
253, 256, '2m, 264, 281
Spwtn, stellar, typ«g) 36 ; of luelium-
ftan, 36-37 ; of Sirlim stars, 37-41 ;
t>{ solar lUrs, 41-45 i fluted, 49-QQ i
of Antarian jtirt, 60-64 ; ot carbon-
(itars, Dl-r;? : of goMoys staiw, &S-61 ;
of Wolf-Eayet stars, 62-6S ; of loug-
period yariablwi^ 52, 79, 102, U3 ; of
■bort- period variableB, 116; of tero-
pomry atan, 62 ; a]t«ratiotiB In, 60 i
niatiObB to tomperature, 74-77, 78-
70; at double atnrfi, 14S, 161, 17$,
ISO, 181, 183, 210, 211 ; of the
Pleiades, 223 ; of elustera, 241 ; eon.
nection with proper niotioa, SOS
Sp«ctrogTkphJc methods, 2S - 29, 3S *,
application to stara, 38, 53-54, &&-56 ;
to nsbulc, €6-67, 70, 260 ; to Nmm,
91
Bpectroccopic bioarias, diBcoYBries, 80,
105, lis, 121, 128, 131, 139-1&2,
J97» 203, 206-207. 222 ; relations to
telcMcopIc binariei, 168, 209 ; condi-
tions of movement, 187-188; abunilauL
oocurreccft, I8S-1S9 ; dims detennina-
tinna^ Idl -, nebulous, 207, 270
SyBctruiu analyBi?, principlia, 16 ;
method^ 17^1S ', Applied to tho stan,
35
Spnacflr, distribittion of neWlie, 351
Spies, a »p«Gtroacopk bjniry, 190 ; nuuu
of aysteiD, 191 ; panUlox, 297
t^jiirol DebuliB, ilbcovetod at Fatsoiu-
tovrn, 252; two-brwicbed, 253 ; fore-
ahortened iuto '^'«piQdJ4»," HSi ;
copious oeciUTcnce, 344
Star-dria, 327-328 ; cbankcteriseH partial
aysteniH, 323-330
^tan, Dumber viHiblor 1 *, de^giiatloD^,
1-2; magiiituil«L5, 2-3; aointiUaUon.
3-6 ; t«lsuopio multitude, 6, 362 ;
toUl light, 7-S, 361 ; individaal rtndy»
S, 16; comViiiutioDB, 9; catblogU««,
IS, 317^ 364 ; detemiLnalioii ofplaoBS,
13; EuoTement^ 14, 303-304, 305,
308, 314, 3I&*332; paraUojtes, 14,
15, 282-360; faintuoM of ligbt, 17,
33; aim -like bodias, 34; spectral
typM. 3&-&7 ; gMWJUH, 68-65 ;
cbfloiifltiy, 37. 40-41. 47, Sl-Sa, 55 ;
tejapsratiiraH, 71-80 ; tclipses, 126-
133; colour-thangw, 135-136, 141-
142, 146-148 ; naturo and variety of
tinU, 136-149; pliotognplifo chut^
Saa, 365 ; distribution, 363-365, 36»-
370 ; belt-foTmatioa, 366-368 ; coUec-
llon iuto riags and ttreoms, 371-378
Ht«bl>iii8, KpcctTitm of Mira, 63, 54 ;
llRht-cbange. 100
Stefan'g law of cooling, 71, 73
Stellar bftbuliB, nionoL:liromAtic ligbt,
64 ; collated in Milky Way, 66 j «-
moteDess, 66, ^46 ; imdlal T«loctty,
S76
Btokea, 3lr Oeorge, temperdture-mUtioui
of Une-Bpectra, 78
StoDe, mea8iiruni6ut of ^lUr hfiat, 72 ;
CBotra of ^rarity of a Cestsuri, 174
StrntoQoff, coastitntJOD of tba Pleinden,
220 ; pbotograpliH of PLciadeR nehnliR,
225 ; dliitribatlcJii of uebuln. 354
Strove, F. O. W., observatiou of 4 ired
itar^ 141 ; colours of iioiib|« atart,
143, 144, 147, 148, 182 ; Msigued
limit of Apparent diatancc, 151, Ib^ ;
detections, 164, 181, 197: otwrrva^
tionSf 193, A'iB ; colour- ptroaption,
146; mognitudea of 44 BoiltiS;, 179;
fifth star in trnpezfum, 205 ; ntcllar
paraUai, 284 ; criterU of wtflUar
jMlillf»nfatirMl.»M
•irlfU M bd— I •!«, 344; Mhn UM
Mbote, 347 i Mr*ttM mM% 3M ;
iUlUr ud mMw «alM,9U; d*-
UU la Omtm wnkmh, m
TufI, X, w ■■llpiiM biwr, 1>0-1»
T«libatt» Ckdlag of ■ nd «tar. 141 1
wliHU dovbto ftar, IM
Ttlawppw, ■^^towd ittOMrt l at, IS,3S;
Tmp*!, dUm In AadraiB*!* lub^ 89 ;
dtaeavvy of lUvopa babuta, 223
T«ni|i«ralan, of tlia no, 71 | ^ «Uri.
7S-U, 77-7*. flO; of »bol». 79.
3M-U1
TmporHT itaim «i|fa ol apaBin, 03,
SC M ; faullridtua ontbtuiti^ »S-«5 ;
dlftrLbtiUoR, M-BO; aui of thoM
utlu'^ 184 ; wttour-chftogw, Ul*143
Ttaulty. uf mILimIiix «l«n^ ISA ; of
lUtla^ ■tmcUri of flatod ipta^ IM);
poled of Outor, 147
Thoma, Cordotw Durchtauttcrniu, t
of fUlUr gyiUma, 306-200
'i'liHruict Hatoxy of AIrqI'm laaqtullUM,
13B. lau
TlUnliiiiu afadiorptloa-lliiM In t^lur m^
mU\\n.x HpvotrE. iA» (3, &£ i HutingB in
JuiUrlu itAn, Al
▼■Udt mM^ I iiMilii. X77-:
y«i>life ita>^ ndMi^ 6S, 1 U ; dSi^lir
df Uriffcl Ham ■• Bsiin^ fil. U^
lit : aivd ipvclnl typtb M ;
vuiteBMi^ TVs illiHilBia I
«l ; Av« «Imv eS :
psiodii, ftMOS; bngvlw, 10&-U0:
•r •kort tMrfosU 07, lltf-iSd ; <&sixi-
fatillgni< pviodfl, 96s H' ; cxptuMatr
trpotht— , 110-115; «eliiiiM^ Ifd-
iMi mllKtod ID cnMpa, IM:
MapUd. IM. 17a-184
V«^ iippwBl brUbkH)}; 3, 23; kf-
dn|;ai-Hri« In cp«tnm, 81^ it;
fcR&pentare, 74 ; ii]t»>Tioi«t taSxk-
Uoiu, 77
Vfllonuii, R', nittqre of «djp««, iSIt, 181
VilonzM. &, frclitMtt tmdergoae by, ISS
VelonuD, r, bdinif of coloor, 141
Yfltoram, 7, cnuadoo-spectram^ fi8» 07 •
oxfgieD^bHrptioD, 01
Tsry, ncbaloiitj roand Norm Psvd, 9£
ViJluKwui, pianJlAX of binarieiH 2S5
Viigiiii», -y. duplicity, 1*0; o^\, 17*-
174; reltUve muaos, 17S; Inmiiioii^,
176; vn-UhLlily, 178; jpectrnjo. !?•;
flpectroHcapic p&rallAX, 26S
of mlial velticity, 29, U6, 833 i
dwortiuiDBtioii ot belium-MlOs, Sd ;
iDor«menti! within Oiioii iwbiili, 60,
INDEX
403
I STS ; obuTvation of Kova Corosa, 86 ;
I spectroscopic binnrit:!, 105, 190, 102 ;
ecljp!«s of Algnl, 117). 12S ; spectra nf
, 06 Herculip, 117 ; iiiveeligEition* <jf
, elaalers, 232, 341 ; peculiruilies of
plinetary nebtilm, 246. 249. 256 ;
mi&bla nebula, 278
liogvl, H. W., spBctrum of bydro^eiii
87
■Vatrd, Nova Androinc^ia:, 89
Waters^ rliiitributlDii ^f nobuln!, 351
j^^Wftbb, colour of U Cygni, 183 ; arrange-
^K meDL of ctiutertiig BtaiK, 237, 233 ;
^^P pljinetaxy nebula, 3Q0 ; st&T-pHttertLn,
I 871
W«ber, twinkling t>r tUn, 6
WMnmA, mt^vAJuflots of the Hyiidi^ 3Q7
I We(lQ7, pbotogTftphi of the PUijuiei,
225 ; diti^^iQB of Andromeda and
OHoD uebulrti, 25S, 259, 26S
WliHwell, interBtflUar aitnatjan of nebulKi,
361
Whirlpool nebulft, typical of spiral clua,
243, 25i ; 'ItfliKtinb at bratichcs, 2^5,
250 ; repiiLiive actioTi l>etokoiieil, 374
WiedeuiiDii, liiroinesecnM, 77
Wiea'a law of spectral energy. 79
WlUiamfi, investigatioiiB o( variable dtara,
120
WllslDiff, stellar Mpectrograma, 36 ; phajie*
curve of Algol, 121^ ; perlurballDTif of
61 Cjgni, IfiS
Wilson, nebulosity round Nova Perseij
04; photographof nn irregul&r nebnla,
283 ; repulsive affucts in Whiripool
nebula, '274
Winloek, double wtellite of itepdiw, 16&
WinnKlce, light-change of S Monocerotif^
ISl ; m^aBUrumeut of PneMpe, 333 ;
Tariability uf a nebula^ 276 ; parallax
nf a faint star, 290
Wolf, C.t catalogue of tha Pleiades. 318,
220 : uebuloua condition, 221 ; map
of itars in Preaepe, 233
WolC, Idax, diacovBriea of ucbulsi, 11 ;
observation of Andromeda nebula,
89; nebalcwity rmmil Nova Peraai,
93; photf>gTaphB of D«bTile, 253, 259,
270, 271, 362-353 ; "inakB" nebula,
267 ; replac«inent of ntan by nebuLc,
352-363 I nebulflT survey, Sfi4
Wolf, B., period *ttributfld to t) Carina,
107 ; solar auil fitdlftr p«riod)oity, 113
Wolf-RAyet Btan, emiMloa Ihuuh, 56,
62-fiS; amuitip.'', 56, 64, M, 9fi ;
Bum'tier and dintribution, 64 ; Id-
Beiiai>!le p[iJikllax«.H, 300
WoodB, detection of a variable atar, 136
Wright, lliomas, disc-lh&ory of MUkj
Way, 359
WriKbt, W. H^ ipectrograniR of Mir*.
53 ; apectrosoopic panUlax of a Caa-
tauri, S6€
Ye&[d(!ll, colour uid period* of vftrtLblee,
114 ; ccUpsea of U Cepbei, 131
Yoonp, oolcium-vaponr iu aun, 42, 4S ;
diagniQ of auD'a path in spuiQ, 812
Zaeh, red stsrs, 138
Zeemati ttttct impercepUhlit id Dnted
K].)ectra, 49
Zodiac, tiigns of the, 2
Zollner, polamlng photome'ter, 2]
THB WXTD
PrtHUtt i^ it. & k. U.AM]t, Umitsd, £diMimtg/L
^':
t
JAN 15 1941