Meteorite studies

=

H225

4
ey

322:
petted

4 tele:
Ricietaan bs hes ite
hh ia mat

| aot

of

But

5
“

+04 cud : 2s
atin

ze + of
ae ecEe SES

oe

enyere
preter in tt?) SE ;
roo

LS otete}

i
mt

Vihshy yr *
erent SEA nt
Wilts ot belied Werte hry
eee

ene yh)
Nae ip nie: :
“

is

;
ae
$2 ale i" J

th BERD oe) Pes
Hk rape h

san

=

ta

viaiyter

isin

tit i}
we iil
Ban ate at
vee a ?
me * rt

Utes

ae

Ly heh
Cab rrs

=e

seve

oS

Sere
ees ©

1

Kh ised
2 f
pin

Ly y
%

‘
poke

enlad +
»

He

ata?
tev oo we

Big ;
i i peer bhatt
sree: 8h: tae ies ; i ;
Poo eet Mea eat SU evea
hy + wy ‘J i (> - pee y 6
Whabeest 1) Q ehh
ket i ; ;

yp

S3

are e ae
pels

=

x

=

Hj NB TS
tte
A, pains

esate Mea TER Pha ine

=

aS ea
== S25.
ris yt tet
nes <3
=

ath

i ie

Lt
SP ellsamats ae
Mb tit
rat tat
wis bend
ioleian!

righ ci Meyer BT

Bait tot
ea

+ ba beg
ee 4
fst

ey

ay
Pintre
Sate

it t
nad “
Tt aboy Eines ;
Livahiakerea tales
; Hat
ryert uh

; iat
eats s404 Ft ho a ert f}
Riccar te art edt ad

het As ny f
H,)

sarees

Ate

aes: Seach
43

atat>

7
Tomeeieg ©:

ove

ny
Mt \
4 peolyrasiet
welt A: |

Stee
34

Peseta

Anions te Hl
Lhoteteveu

cheat Teed

” ot
be 4 +4
rot ft eh ‘4
ine Ee
FY!
ity ee
oni?
)

AT
ai hguber oe
Peoraits peer pt
mene h 4 Ween, pee
Hbrsctoa ter tea settee fortes
i Maseaes ah
a teys ? tal

PLO O90 004040004
$ ILLINOIS STATE ;

: LABORATORY :
OF NATURAL HISTORY

é LIBRARY ;

POL OP OOD. 1-05-85 OOS 6

rpawery 3 505 Ay eH
s/n > f
E | jae)

wa
DN IUNe ONE:

¥ Ni
H{tape
ae
j ul
RAS

A Sie

MOEN SH > iy ata : Se ) Rete soruce 2 % 5 4 an 2 ; em : Z BAN

Grnten OG

et a : sxe

ERPS SERP A) ; ay, ; = <j.

bol a PN eeRy Sey
2. vas ca’ NA

a
s

SOHN CO IE any eee

VPS : Ber acer

ae

SY CAGe AD)

Eo

Safth

Ign

(esl Ti MpsSarauc®, ie eR: AYA ENB LN fp thy f 18-4)

~~

a

> &

one :
Manoa. he

ta

hy, pees. Gz * ¥ * WRaeAy ©

Vavs

13
onal g

Fietp Museum or NaTuRAL History.
PUBLICATION 145.

GEOLOGICAL SERIES. VoL. III, No. 8.

METEORITE STUDIES III

BY

OLIVER CUMMINGS FARRINGTON.

Curator, Department of Geology.

Cuicaco, U. S. A.

June 1, Igto.

a

aT ie
Pat fe
se

METEORITE STUDIES. III.
BY OLIVER CUMMINGS FARRINGTON.

LEIGHTON.

This meteorite fell at 8 p. M., Sunday, January 12, 1907, eight
miles south of Leighton, Colbert County, Alabama. The exact place
of fall was near the old Bethel church in township 5, range 10, west
of the Huntsville meridian. So far as is known to the writer only a
single stone of the fall is preserved. To Dr. A. Graves of Leighton
and Professor E. A. Smith of the University of Alabama the Museum
is indebted for such information as it possesses regarding the fall.
According to Dr. Graves the meteor which produced the meteorite
passed over the region with a mighty roar which ended in a report
something like pistol-firing in rapid succession and from which “ par-
ticles flew like sparks from a coal of fire.’”’ A stone from this meteor
struck in the yard of the residence of Mrs. M. D. Allen. Mrs. Allen
and her daughter Mattie were standing on their front porch and saw
the meteor, heard the explosion, then heard a whizzing in the air and
the striking of a stone in the yard. On going to the place they found
the stone which is now preserved, sunken to the depth of about 12
inches. This stone weighed one pound and fifteen ounces (877 grams).
About one ounce was chipped off from one corner by the parties who
found the stone, in order to examine its interior. Accordingly the
weight of the stone as received by the Museum was one pound and
fourteen ounces (850 grams). The shape and size of the stone may
be roughly described as like that. of a man’s fist. It is shown in
Fig. 1, Plate LV. The greatest length is 4 inches (10 cm.), the
height 2% inches (6 cm.). About three-fourths of the surface is
covered with crust, the remainder has a rough, irregular, fractured
appearance. The lack of crust on part of the uncrusted surface is
probably due to the breaking done by the finders, the remainder per-
haps represents a fracture of the stonein the air. The large fractured
surface is roughly triangular in shape with sides about 3 inches (7.5

em.) in length. The encrusted surfaces of the stone are all smoothed
165

166 FreLpD Museum or NATURAL History — GEo.oGy, VoL. III.

and rounded. They are either convex or concave. The convex sur-
faces are of comparatively uniform slope, the concave, irregular and
showing depressions resembling pittings, though these are rarely as
well-defined as is usual in meteorites. Five of these pits which occur
together in one concavity are approximately circular in outline,
shallow, and have a diameter of about one centimeter each. On
another portion of the stone two similar but smaller pits may be
seen and on another portion a larger, crescent-shaped pit. Nothing
in the shape or markings of the stone indicates orientation during
flight. The general shape of the stone is, as already noted, irregular
and the crust remarkably uniform in appearance. In color the crust
is dull black with occasionally an inclination to a reddish shade.
Seen under the lens it presents a porous, slaggy appearance with no
indications of flow. The indications are that the surface fused in
place. The pores of the slag are very minute and the crust strongly
adherent.’ Grains of nickel-iron rounded by fusion can be seen here
and there and occasionally spots from one to three millimeters in
diameter having smoother crust appear. These doubtless indicate
portions which for some reason fused somewhat more readily. The
color of the interior of the stone is in general brownish-black resem-
bling the black chondrites. A marked feature (shown in Fig. 2,
Plate LV.) is that of large spots of a much lighter color scattered over
the dark ground. These are best seen on polished sections. The
color of these spots is a light gray, and so much lighter than the mass
of the meteorite as to be very prominent. The spots vary in size, the
largest seen covering nearly one square inch of surface. The outline of
the spots is irregular but not strongly so, and tends to be curved rather
than straight. There seems to be no indication megascopically of any
separation other than that of color, of the substance of these spots
from the remainder of the mass. The section in which they are best
exhibited and that illustrated in Fig. 2, Plate LV, was made near
one end of the meteorite. On a section parallel to this made about

one centimeter nearer the interior, the larger spots while retaining |
their relative position were found to be much smaller, less than half
the size of those on the outer section. They do not, therefore, extend.
uniformly through the meteorite. As solid bodies their shape is
probably somewhat lens-like or flat-pyramidal. One spot which
was small on the outer section was about twice as large on the inner
section. Hence the spots are probably to be found scattered irregu-
larly through the meteorite. The structure of the meteorite on the
whole in respect to these spots is the same as that designated by Bre-

JuNE, 1910. Meteorite Stupies II] — Farrincron. 167

zina as breccia-like. This term should be understood however, in the
same sense in which Brezina uses it, i. e., as an imitation of brecciated
structure, without an actual clastic origin being assumed.* The writer
knows of no meteorite in which this structure is so strongly marked
as in Leighton. Besides the spotting already referred to, the dark
mass of the meteorite is also speckled by numerous chondri of various
sizes and shapes but in general more or less circular in outline and
ranging from 2 mm. in diameter down. The color of these closely
resembles that of the light-colored spots just referred to. There
is also a thick sprinkling of metallic grains. These are as a rule
small, independent of each other and very irregular in outline.
Some of the larger ones are elongated, one seen being 4mm. long
and 7 mm. wide. The distribution of the metallic grains as a whole
is comparatively uniform, except that they tend to encircle the
chondri. Troilite is to be seen in the form of grains, but is much
less abundant than nickel-iron. At one point, however, a large
nodule of a somewhat crescentic form occurs which has a length of
11 millimeters and a width of 5 millimeters. This troilite is of bronze-
yellow color, brittle, and slightly magnetic.

The texture of the stone is firm and compact so that it breaks with
difficulty and takes an excellent polish. The specific gravity obtained
by weighing the whole stone was 3.604.

Under the microscope, chondri appear to be pa more numerous
in the dark-colored than in the light-colored portions of the sections.
This difference is doubtless in part due to the greater contrast in
which the chondri are thrown by the dark-colored background, but
there is also a real relative scarcity of chondri in the light-colored por-
tions. The line of demarcation between the light and dark-colored
portions is as sharply distinguished under the microscope as to the
naked eye. Leighton in this respect, therefore, forms an exception
to other brecciated chondrites, if Cohen’s statement in regard to the
latter is accepted, for he states that the megascopically sharp-appear-
ing boundaries of the differently colored areas of such meteorites dis-
appear under the microscope.t Yet the difference in appearance of
the two portions of Leighton as seen under the microscope is not
sufficient to establish the existence of a true brecciated structure in
the sense that it is certain that the mass was at one time broken up
and recemented or that fragments of different origin are here seen
cemented together. The appearance rather suggests that a dark-

* Jahrb. K. K. Geol. Reichsanstalt, Wien, 1885, xxxv, 172.
} Meteoritenkunde, Heft II. p. 63.

168 Fretp Museum or NaturaL History — GEo.oey, VoL. III.

colored liquid has been infused into the mass and affected certain por-
tions. This infusion appears to have taken place subsequent to the
cooling of the original magma. The siliceous minerals seen under
the microscope are chrysolite and bronzite, apparently in about
equal proportions. They occur as chondri, as fragments of chondri
and of crystals, and as more or less completely formed crystals. The
chrysolite chondri tend to be of small size, circular in form and mono-
somatic. One such chondrus measures .45 mm. in one diameter and
.52 mm. in the other. Its border is composed of a series of grains
more or less circular in outline and .o6 mm. in diameter. A series of
parallel alternate rods of chrysolite and glass averaging .o3 mm. in
width fills the interior. All these and the border extinguish simul-
taneously. Some of the other chrysolite chondri are characterized by
a porphyritic structure. All the chrysolite is highly fissured, as is
characteristic of meteoritic chrysolite. The bronzite chondri areas a
rule less regular in outline than the chrysolite chondri and vary greatly
in size. The largest seen is nearly 3 mm. in diameter, though of
irregular boundary. It ismade up of minute parallel fibers of bronz-
ite .0075 mm. in width and 2-3 mm. in length. Other chondri show
eccentric-radiated, parallel or irregular arrangement of fibers. One
conspicuous chondrus is of oval outline, 6 mm. in its longest
diameter and is composed of seven fan-shaped rays of bronzite set
in an opaque background. The rays radiate from a point near
the circumference of the chondrus and widen as they pass toward
the opposite periphery. Each ray is divided into two longitudinally
and there is a more or less sharply marked border of bronzite. The
chondrus as a whole has circular polarization. Another chondrus of
somewhat rectangular outline is about half composed of well-crystal-
lized bronzite and the remainder passes into a series of half-glassy
fibers. Narrow black veins evidently subsequent in origin to the
chondri cut through the sections. The nickel-iron occasionally exhibits
a tendency to follow these veins. The nickel-iron and troilite grains
are megascopically of amoeba-like outlines and evidently formed
subsequent to the chondri. The crust when seen in section on the
darker portions of the meteorite appears as a black, opaque band about
.4 mm. in width. Owing to the dark color of the interior the crust
is not easily distinguished from it. It is certain, however, that it
does not exhibit the zones usually characterizing the crust of chon-
dritic meteorites. As none of the sections prepared for study showed
crust bordering the light-colored portions, no study of this could be
made.

June, 1910. Meteorite Stupres III — FarrincTon. 169

A partial analysis of the meteorite was made by Mr. H. W. Nichols
with results as follows:

ENS aN aha oi eae Vs © aes Wg ge Bie os are a een ee Bikers nd 35.69
PET ae eo ae Se rere Micra Cate tga oe heals eave SRS el aoe tes 1.03
Cre O; Sh ee eC, Sa ea a eee ee RAPE RPO ST ay ee ore ee Ree ie aaa 0.12
bE gS RES pea Aa iene tt RARER PES ee RR he ied CNR? RO RE 1.04
MR a ery aloe pa eng rd oe eA ag, « arg cue Lela se wd-piese 0.08
hic cag sae a EO a Sa ox cea cata a oe SAE De 1.93
RR se ae SAN Re wlaca an A SEAS kad 5 Sma e eee 0.95
eo APR meee ote h cick SS yan iy ee Me Se Paneth AD eg Sry 0.47
Pe ah ers Be ren ean ee ce felt oo on ograaphote oy Gags Ae aterw S ©.40
Fie car bs Re ee pales ae Cael dices ANS ee ea pears 2.11
Me sta Praleg nal d atone ooh SOUS Se Adee alghias Brokat mre Sietan ded nadie aay 10.48
PR go oe Cia NG el gta er MONA ee Sri alace feelin «erie ia tees ae re das 1.59
alee ee ORE RP ANY EE are Eng enc ek oe A ey aN si 0.21

56.10

The remaining 44% is almost wholly Fe O and Mg O in approxi-
mately equal proportions, with probably a little water and some minor
ingredients. The composition is that usual to the chondritic meteor-
ites.

QUINN CANYON.

This meteorite was found, according to Mr. Walter P. Jenney,* at
the above locality in Nevada, in the latter part of August, 1908, by a
prospector looking for borax. Mr. Jenney further states that the
prospector cut off a few small pieces from the meteorite with a cold
chisel and took them to Tonopah, Nevada, for identification. Soon
after he sold out his interest in the find and left the country. The pur-
chaser of the prospector’s interest placed such information as he had in
the hands of Mr. Jenney with a view to rediscovering the meteorite. As
a very imperfect description of the locality where the meteorite was
situated had been obtained from the original discoverer, it was nec-
essary for him to make two trips to the region before the mass could
be relocated. These trips, made by automobile, required 430 miles
of travel. The place of find was in the foothills of the Quinn Canyon
range of mountains, Nye County, Nevada. These mountains are
marked on some maps as the Grant Mountains. The locality is go
miles east from Tonopah, 18 miles north from the Mt. Diablo base
line, and roo miles west of the Utah boundary. The meteorite was
found on the western slope of the range and on the northern slope of
a low hill of andesite. The slope was a gentle one and the contour

* Mining & Scientific Press, Jan. 9, 1909, p. 93.

170 Fretp Museum or Natura History — Geotoecy, Vor. III.

of the surrounding hills was such that the meteorite in falling may
have come at a low angle from the west, north, or northeast. The
area is treeless but bears a sparse growth of grass and sage brush.
It is uninhabited except for a few sheep herders and occasional wander-
ing prospectors. The meteorite was found with its flat side down
and its arched side projecting above the ground. It lay with its long-
est dimensions in an east and west direction and was imbedded in the
mantle of soil covering the hill to a depth of 10 or r2 inches. Mr.
Jenney states that the contour of the surface of the ground had evi-
dently resulted from extremely slow erosion and there was no indi- |
cation that the meteorite had ever been buried deeper and exposed
by the wearing away of the hillside. Under Mr. Jenney’s direction
a freight wagon drawn by a team of six horses and provided with a
crew of three men, and with derrick and chain pulleys, went to Quinn
Canyon and hauled the meteorite to Tonopah, the nearest railroad
point. The round trip consumed eight days.

Through the generosity of Messrs. Stanley Field, R. T. Crane, Jr.,
Cyrus H. McCormick, and George F. Porter of the Board of Trustees
of the Museum, the meteorite was acquired by this Museum in April,
1909. It wasshipped from Tonopah under the direction of Mr. Jenney
and reached the Museum in good condition. It is the largest specimen
in the Museum collection and one of the large iron meteorites of the
world. :

In form the meteorite shows considerable shaping from its passage
through the air and hence, as is typical with such meteorites, is a low
cone. This form is due doubtless to the excessive action of the heat
and erosion of atmospheric resistance about the periphery of the
front side of the meteorite. Here the meteorite is worn away most
rapidly and thus acquires a slope toward the center. Another effect
of the atmospheric resistance is seen in the production of deep chan-
nelings, furrowings, pittings, and numerous cylindrical holes on the
front side. All these, while very irregularly distributed, have a
generally radial arrangement from the center outward. The outline
of the meteorite in the direction of its greatest length is essentially
oval though somewhatirregular. The contours may be seen by referring
to Plates LVI-LVIII. The longest diameter of the oval is 47 inches;
the diameter at right angles to this is 35 inches, and the circumfer-
ence 132 inches. The height of the cone is 2oinches. The weight of
the meteorite as determined by two careful weighings is 3,275 lbs.
(1,450 kilog.). The front or conical side of the meteorite and the rear
or basal side present very different appearances both in contour

JUNE, 1910. MeErTEORITE StupiEs II] — FarrincTon. 171

and relief of the surface.. The front side is highly corrugated by
deep and irregular channelings, pittings, and furrowings. The rear
side is relatively smooth but with broad, shallow pittings. The
features of the front side of the meteorite while very irregular may be
classed as knobs, furrows, large and small pits and cylindrical holes.
Of these the knobs lie between irregularly coursing furrows which
leave the metal standing out in prominences, ranging in size
from that of a man’s fist down. These knobs are especially notice-
able toward the apex of the cone, so that this has none of the smooth-
ness which is often observed in meteorites of this form. The furrows
are very irregular in their course but in a general way may be said
to radiate outward from the center. They are shallow and sinuous,
with the ridges between them usually broad and rounded. An
average width for the furrows is one-half inch (1 cm.). Interspersed
with and interrupting the furrows are shallow, shell-shaped pits from
1 to 3 inches (2.5 to 7.5 cm.) in diameter. These are the small pits
referred to. The large pits differ in shape and character from the
small pits, since they penetrate deeply into the mass of the meteorite.
The largest of these pits is a bowl-like depression about nine inches
(23 cm.) in diameter and four inches (1ocm.) deep. On Plate LVII it
may be seen near the base of the meteorite. The contour and sur-
face of this pit are irregular but it is much the deepest and largest
depression observed. Perhaps the most interesting feature in regard
to it is the occurrence, spread over the bottom in two places covering
about one squareinch each, of a crust of black, magnetic iron oxide.
This adheres very firmly to the metal which it covers so that it can
only be removed by blows with a hammer and chisel. It is con-
tinuous as a broad patch in the two places where it occurs but the
two patches, while situated near together, do not join. The thick-
ness of one of these patches is about 2 mm., that of the other is much
less at the thickest point and dwindles away to nothing. The sur-
face of the thicker patch is rough and corrugated.

The cylindrical holes referred to occur irregularly over the surface,
not being grouped or lineally arranged so far as can be determined.
Of these 35 may be counted with orifices varying from one-fourth of
an inch (5 mm.) to one and one-fourth inches (3 cm.) in diameter. The
majority are about one inch (2.5 cm.) in diameter. They penetrate
to various depths the deepest being twoinches (5 cm.). Frequently
the cavity within is larger and of somewhat different shape from the
orifice. Asa rule, though, it has an approximately cylindrical shape
and is about the size of the orifice. Other shapes noted for the orifices

172. Fretp Museum or Natura History — Geovuoey, Vor. ITI.

besides circular are oval, semicircular, kidney-shape and pear-shape.
The direction of the cavity tends to be at right angles to the surface,
but this varies also. Holes similar to these occur in many large iron
meteorites, such as Chupaderos and Charcas, and are usually ascribed
to a boring action of the air, or to the fusing out of troilite nodules.
Their occurrence in the Quinn Canyon meteorite does not seem to
throw any additional light on their origin. Their existence must be
more or less responsible for the noise which accompanies the fall of —
a meteorite, for when a current of compressed air is directed against
one of them a sharp, ear-piercing sound is produced. What the noise
must be from this cause when the whole mass, highly heated, is ad-
vancing at an enormous velocity, is almost beyond comprehension.

Aside from these coarse features of relief of the surface, there are
others of amore minute character. These may be designated as struc-
ture markings and lines of flow. The structure markings show the inti-
mate crystal structure of the iron and are most abundant on the walls
and at the bottom of cavities near the apex of the meteorite. They
consist of groups of parallel ridges about 1.5 mm. apart, cross-hatched
by shorter ridges at right angles. Small square pits about 1 mm. ona
side are formed asaresult. The long ridges are probably formed by
tenite ribbons. Those at right angles are at irregular intervals, and
probably mark the crossing of other bands. Asa rule the groups of
long ridges run in three directions at angles of 60° and often intersect
to form triangles. The lines of flow as a rule cap the ridges of the
meteorite and for the most part follow the crests but also at times
cross them in a series of sinuous, more or less parallel lines. The
metal is brighter along the lines of flow and in broad patches adjacent
tothem. They have the appearance therefore of a thin skin of metal
which has fused and started to flow at various points. The thickness
of this skin can hardly be more than 0.1 mm. The direction of flow
is always away from the center of the meteorite, or in other words
from the apex toward the base of the meteorite.

The pittings on the rear side may be divided into two classes as
regards size and shape though all are probably similar in origin. The
pittings of one class are large and circular or oval in outline. One
of the circular pits is 4 inches (10 cm.) in diameter, and the largest
oval pit has dimensions of 8 x 8 inches (20 x 13 cm.). Others of the
large pittings have less regular shapes but all have sharp edges and
do not merge into one another. The pittings of the other class are
smaller, dot the surface pretty uniformly and average about one inch
(2.5 cm.) in diameter. They show all variations of shape between

JUNE, 1910. Meteorite Stupies II] — FarRINGTON. 173

cavities of circular form and angular depressions between angular
elevations. These angular elevations doubtless represent the octa-
hedral structure of the meteorite. The fact that the octahedral
structure is thus brought into relief indicates that this pitting is due
to a slow process of weathering and solution which the meteorite has
undergone since its arrival on the earth. The larger pits are all
doubtless produced by a process of weathering and solution, but the
cause of their size and shape is not clear to the writer. Pits of the
same general nature though much larger and deeper characterize the
Willamette meteorite and were referred by Ward,* to a weathering
process without any theory as to details. The rear side of the
Quinn Canyon meteorite was, as has been stated, immersed in the
soil and this gave, probably, moisture which aided solution of the iron.
Carbonate of lime in the form of a whitish, closely adhering deposit
covered, when the meteorite arrived at the Museum, the portion
which had been imbedded, about the sides but not to any extent on
the bottom, that is, the flat surface. The larger pits contained a
considerable deposit of hydrous iron oxide in the form of scales which
could easily be pried off. The side of the meteorite which had not
been imbedded showed no weathering.

In connection with his account of the finding of the meteorite, Mr.
Jenney described the passage of a large meteor over the region Feb-
ruary 1, 1894. This account he repeats and elaborates in a later
article} and considers it highly probable that the Quinn Canyon
meteorite fell at this time. While there seems nothing impossible
in the view, it is also true that there seems no way of positively con-
necting the two occurrences. The decomposition seen on the im-
bedded portion of the meteorite might seem to have required a longer
time than fourteen years for its production, but no definite means
of measuring this is known. The slight depth to which the meteorite
was imbedded in the soil shows that it must have reached the earth
with a very low velocity, in fact, so low that it is difficult to conceive
how so large a mass could have alighted so gently. The assumption
of a path nearly tangential to the earth’s surface and a direction of
motion similar to that of the earth seems the only way of explaining
so slight a vertical penetration.

In order to determine the character of the etching figures of the
meteorite two small fragments, weighing 9 and 15 grams respectively,
have been cut from it since its arrival at the Museum. The surface

*Proc. Rochester Acad. Sci., 1904, 4, 141-146.
fAm. Jour. Sci., 1909, 4, 28, 431-434.

174 Fietp Museum or Natura. History — Geoxoey, VoL. III.

of the iron was quite resistant and hence the cutting was performed
with some difficulty. Beneath the surface the iron is relatively soft.
The depth to which the hardening extends is small and unmarked by
any change of structure that can be observed either on etched or

Fig 1. Etching figures of Quinn Canyon meteorite. X2.

unetched sections. Mr. Jenney describes the meteorite as covered
with a ‘‘thin, smooth skin of magnetic oxide’’ which he considered
to have protected the mass from corrosion. It is true that the color
of the surface of the meteorite is brownish-black as compared with
the nickel-white color of the interior, and this surface color probably
indicates superficial oxidation. The coating of oxide is, however,
exceedingly thin. The interior of the iron is of nickel-white color

.—

JuNE, 1910. Mereorite Stupies II] — FarrincTon. 175

and polishes well. Etching is easily performed with dilute nitric
acid, the figures coming out very quickly. In fact, they are dimly
outlined on surfaces which have been simply polished. The figures
seen on etching the fragments are shown enlargedin Fig.1. They are
octahedral in character with long, straight, swollen, and little grouped
bands. The fields are few in number and subordinate. They vary
in size and have the forms of triangles, rhombs, and parallelograms. .
They are filled with dark-gray plessite, much darker in color than the
kamacite. This plessite may be quite uninterrupted or it may con-
tain networks of tenite, seen over the whole field or only in portions
of it. The kamacite of one of the fragments etched shows well-
marked hatching, the lines running in three directions, two at right
angles and one diagonally. The directions of these lines are as a rule
different for the different bands, each band having its own system
but in one group of bands 8 mm. wide but subdivided by little tongues
of tznite into smaller bands about 1 mm. in width, the orientation
of the hatching lines is the same throughout.

- While one of the fragments exhibits hatched kamacite the other
exhibits only spotted kamacite. The spots of the latter are about
I mm. in diameter, and of uniform size. It is possible that the por-
tion of the meteorite showing spotted kamacite was more highly heated
and the hatched kamacite thus metamorphosed to spotted kamacite.

Analysis of the meteorite was made by H. W. Nichols from ma-
terial obtained by boring with a #;-inch drill to a depth of 214 inches.
About 20 grams of material were thus obtained, varying in structure
from continuous shavings an inch or more in length to fine metallic
powder. The color of the material was iron-gray. The portions
used for analysis were carefully sampled from the whole lot of borings.
The analysis gave:

BBR Hae bal y Oe ad ke Ve ER EE ei ed 91.63
DUN Sy sleek ioc a gave ns owl Hew bE Ss 7.33
RAS 6 cg es hk © eh MS eee ee gig BE TAS EN WS evi hare tea va ds 0. 73
OR oe seed RR rise pre ae Daya ahs IGA e opened eeeg tr
wg GI a PRS Cord 8 BR Seen oe ee ac ert rere NS POR a at 0.00
Be Soa ay ig MED ieugtea M ta tee Met Os gba gta ERE wigs a Aiea EP ata 0.20
RS URE Rah ae Gat RST RAN Goda SUGANO Dae lar erg ae MR ben 0.02
99-91

The composition of the meteorite thus corresponds to that usual
to the medium octahedrites. In addition to the components shown
above careful search was also made for gold, platinum, or other rare
metals. These were looked for in the following manner: A portion

176 Fretp Museum or Natura. History — Geotoey, Vot. III.

of the carefully sampled borings weighing 514 grams was dissolved
in nitric acid. Although no residue was obtained, the solution was
evaporated to dryness, ignited so as to convert the iron to sesquioxide,
and an assay made by the crucible method. The charge used con-
_sisted of 50 grams litharge, 25 grams soda, 25 grams borax glass, 5
grams scouring sand, and 4% grams argols. Thelead button obtained
weighed 22 grams. On cupelling this no residue was obtained.

A partial analysis was made of the crust of magnetic oxide de-
scribed on page 171. Fragments of this were broken off by careful
chiselling, and in this way .3396 grams were obtained. The material
was evidently somewhat hydrous and more or less coated with carbon-
ate of lime. It was dissolved by hydrochloric acid although acted on
very slowly by that solvent. Determinations of ferrous and ferric iron

in the solution gave:
Cale. to Theory for

100 Magnetite
ish 2 Ren emer ie Peery Ua rara 20.84 27.62 31
Hes 40 $2, ado 3 saa eel oheatigoerentas 54.60 72.38 69
75-44 100 100

The remainder which was not determined quantitatively, was chiefly
water, lime, CO,, and silica. The proportions of ferrous and ferric
oxide shown by the analysis leave little doubt that the mineral is
magnetite and show that the oxidation which the surface of an iron
meteorite undergoes in its passage through the air may produce this
mineral.

COMPOSITION OF TAINITE.

The composition of tznite, as is well known, varies between rather
wide limits. As these limits do not seem as yet to have been deter-
mined by comparison of analyses, the writer has endeavored to collect
all existing reliable analyses in order that such determination may be
made. The compilation of analyses together with a calculation of the
ratio of iron to nickel-cobalt-copper will be found below:

Fe: Ni+Co
Fe Ni Co Cu Cc Total +Cu
Telcom ehee es 86.44 13.02 OsRA nest) Gigaset OO .00 O39 23
Dee rE eed: 85.00 14 00 weak tr eee Capen titan 99.00 O42
Bra etethen Deter sehs 85.00 15.00 GS luli Lah ate qa LOOSOO 6074-5
—— -y ee |

PAL eA on cs% 83028) tea 6POnOea ess OCO4 GNis 7 OOKOO ee oe
Rav evewdaataiteens BOBO ohare. 19.60 wie tered ale tank 99-90 Aol s-8
OR ere dnjetkoy shes UE teal Rotana YEE Oi 33 eas 1 OFFOr - 5.99593 cer ieee
Y econ eran cate Oe 72. TOs 2308 S580") so.3. Ieye “LOO, 00 BOK 5 vid

~ 0 i ai a ilig

JuNE, 1910. METEORITE StuprEs il] — FARRINGTON. 177

Io.

Ir.

12.

Fe: Ni+Co
Fe Ni Co Cu C Total +Cu
siti Iqbal oe 73.0 > 27700 PeMce Mee eal dy ote pend LOO LOO 2.5. te
miviitegee ea. s!< 7 Wee Veale 3 Say 6202) tend | Ost 2-100 00 ee rare |
Spe ae ee 70320-. 20..92 1.68 ©.30 100.00 ZB Oite
Skis es ere 70.14 29.74 Stig ere et er hone 99.88 re Oey
Sapte gets: 39 69.30" 26.473 °.60 0.37 100.00 OR Aa
Ss aap she: wiles. 68.13 30.85 C200 ©7635. ..5 5 bOO AO TAY tery §
Sn aR rE 65) 5 $32 cr 1.59 100.00 2207%'%
Sees ics 8 65.39 33-20 1.4! 100.00 7 eS Ee
Sears tisk 65.26 34.34 ONFO% eS a iretee ge 2200500 REOv
Baar eis guitars 63 55 50.134.65 1.0L 70:30), (0.49.-100;00 ceo a
BR ea er 63.04 :35..53 1.43 tr. 100.00 Tis’ eek
elec ain Sf 61.89 36.95 0.36 0.80 100.00 Tek
, ~-—- mee!
SI ORE tii, NE CIS 7 i 5 BO ES ai tr. Mien fh ELOOsOO sR TA
Sate tye snk + 57-18 34.00 ee ee ers Wee eee VOL s Liege. S
ecto. tates: s 50.73 47.80 0263. 20397 O55 7 ' TO0100 1 ae
REFERENCES.

Cosby Creek, Reichenbach, Jr.: Pogg. Ann., 1861, xciv, 258. Plates
8 cm. long and 2% cm. broad, mechanically isolated by Reichenbach,
Sr. Mean of three analyses.

Charcas. Meunier: Ann. Chim. et Phys., 1869 (4), xvii, 31. Particles
mechanically isolated by their color.

Caille. Meunier: Ann. Chim. et Phys., 1869 (4), xvii, 32. Net-like web,
isolated by means of dilute nitric acid. . ,

Casas Grandes. Tassin: Proc. U. S. Nat. Mus., 1902, xxv, 73.

Kenton Co. Nichols: Pub. Field Col. Mus., 1tg02 Geol. Ser., i, 315.
Thin, tin-white, elastic, magnetic plates, 4 mm. square, with finely ribbed
surface.

Welland. Davison: Am. Jour. Sci., 1891 (3), xlii, 66. Mechanically
isolated plates ;4—3;4 mm. thick, silver-white to bronze-yellow. flexible
and elastic.

Staunton. Cohen and Weinschenk: Ann. Wien Naturhist Mus., 1891,
vi, 146. Gray, relatively thick and brittle plates. Isolated by dilute
HCl. Calculated to roo after deducting schreibersite.

Cosby Creek. Smith: Comptes Rendu, 1881, xcii, 843. Little thin
plates of white metallic color left after dissolving the iron in acid.

Canyon Diablo. Tassin: Smithsonian Misc. Coll., 1907, i, 212. Calcu-
lated to 100 after deducting 0.26% schreibersite.

Magura. Weinschenk: Ann. Wien Naturhist. Mus., 1889, iv, 97. Thin,
tough, silver-white lamelle soluble with difficulty in acids. Isolated
by dilute HCl. Calculated to 100 after deduction of schreibersite.

Cranbourne. Flight: Phil. Trans. London, 1882, No. 171, 888. White,
flexible, magnetic, triangular or rhombic mechanically isolated plates.

Misteca. Cohen: Ann. Wien Naturhist. Mus., 1892, vii, 152. Dull and
brittle plates. Isolated by HCl. Calculated to 100 after deducting
schreibersite.

178 Fretp Museum or Natura History — Geo.toey, Vot. III.

13. Canyon Diablo. Florence: Am. Jour. Sci., 1895 (3), xlix, 105. Thin
tin-white, flexible plates. Calculated to 100 after deduction of 3.60%
schreibersite.

14. Wichita Co. Cohen and Weinschenk: Ann. Wien Naturhist. Mus., 1891,
vi, 155. Isolated by dilute HCl. Calculated to roo after deduction of
schreibersite.

15. Chupaderos. Manteuffel: Ann. Wien Naturhist. Mus., 1892, vii, 150.
Brittle, tin-white plates. Isolated by HCl. Calculated to 100 after
deducting schreibersite.

16. Toluca. Cohen and Weinschenk: Ann. Wien Naturhist. Mus., 1891, vi,
137. Tin-white, flexible plates. Isolated by HCl. Calculated to 100
after deducting schreibersite.

t7. Canyon Diablo. Fahrenhorst: Ann. Wien Naturhist. Mus., 1900, xv,
376. Thin, flexible plates partly appearing made up of many lamelle,
light-yellow or grayish. Schreibersite, 2.34% deducted.

18. Glorieta Mountain. Cohen and Weinschenk: Ann.Wien Naturhist. Mus.,
1891, vi, 137. Tin-white. flexible, grouped plates. Isolated by HCl
Calculated to 100 after deducting schreibersite.

19. Bischtttbe. Cohen: Ann. Wien Naturhist. Mus., 1897, xii, 54. Large,
flexible plates with included schreibersite. Isolated by HCl.

20. Penkarring Rock. Fletcher: Min. Mag., 1899, xii, 174. Thin, flexible
plates. Analysis calculated to 100 after deducting 4.18% schreibersite.

21. Medwedewa. bBerzelius: Pogg. Ann., 1833, xxxiii, 133. Analysis of
skeleton material left behind after dissolving in HCl.

22. Beaconsfield. Sjéstrém: Monatsberichte Berlin Akad., 1897, 1041. Tin
to silver-white, lustrous plates. Iron determined by difference.

The analyses, as will be observed, show variations of composition
from Fe, Ni to Fe Ni. While this variation is a wide one it is evident
that it is between certain limits, and that it would be incorrect to
ascribe too indefinite a composition to tznite.

TIMES OF FALL OF METEORITES.

The following study has already been published in part by the
author.* In the present paper the records are given in full and con-
tributions to the subject by other authors are incorporated.

The times of fall of meteorites may be studied with reference to
the year, month, day,and hour. Theyearly falls should give evidence
as to the frequency of the occurrence and exhibit periods if any occur.
The falls by months should show the relation of meteorites to Wwell-
established star showers and the portion of the earth’s orbit where
meteorites are most frequently encountered. The falls by days should
exhibit periodicity if any exists and variation in the uniformity of
supply. Finally the hours of fall should give the direction of move-

*Am. Jour. Sci., rgro (4), 29, 211-215.

JUNE, 1910. Meteorite Stupies II] — Farrincron. 179

ment of meteorites. Since new falls occur yearly, data for study of
these points are obviously constantly on theincrease. It is desirable,
however, to make comparisons at intervalsin order that any changes
may be discerned. At the present time the admirable catalogues of
Wilfing * and others, afford excellent means for the collection of such
data. From these catalogues, with such additions and corrections
as could be made from other sources, the writer has obtained record
of 350 well authenticated meteorite falls of which the year and month
are known, 327 of which the day is known, and 273 of which the time
of day is known. In this number it has been sought not to include
finds referred by residents of a locality to meteors which they had seen
a year or more before, since the residents.of most localities can, on the
occasion of a meteorite find, recall a large meteor seen in that locality
at some previous time. To connect this, however, without further
reason with the meteorite found seems an unreliable method of pro-
cedure. :

Considering the falls by years it is well known that previous to
the nineteenth century little reliable record of meteorite falls is avail-
able. Single falls are known for the years 1492, 1668, 1715, 1723,
1751, 1766, 1773, 1785, 1787, 1790, 1794, 1795, and 1796, and two
falls each for the years 1753, 1768,and 1798. For the early part of the
nineteenth century the record is not very complete since during the
that period the possibility of meteorite falls was yet much doubted.
However, the record may as well begin with 1800. From that year
to the present 331 falls may be accepted as well authenticated as to
their month and year. During this period eleven years show no falls
whatever. These years are, 1800, 1801, 1809, 1816, 1817, 1832,
1839, 1888, 1906, 1908, and 1909. Of these the years of the present
decade will probably have falls to their credit after a time, since the
record of falls usually lags several years behind their occurrence.
The largest number of falls shown in any year during the period is
Ir in 1868. The years 1865, 1877, and 1886 show 7 each. All the
other years show from 1 to 6 falls each. The full record by years
beginning with 1800 is as follows:

ESO)... 2 ° LOOO Ri ec. I Leleae rs. 4 1818 3
BBOE si e3tin ° O09 suis 2 ESIB Gr he feis 2 1819 2
URL 2 eine none I BOOS ay vo 3 shah ear ee 2 ES20% 340; cen I
ty eae 3 FHGQ CS, ° PETS votre a 2 1821

02 eA 2 FSEIOi 2 ESTO a Sine ° 1822 5
OUR lore ss 2 1811 2 2.2 tere ° 1823 2

*Die Meteoriten in Sammlungen, Tibingen, 1897.

180 Fre_tp Museum or NaTuRAL History — GEo.oey, Vot. III.

POSH. Fae 3 1846 4 1868 II TOQO oi <i> sae 6
TS2S eo ses 2 LDAP os tials 2 S095 234s 6 TSO a santas 2
TOPO aoe. 2 MEA On lsat 3 1870 3 ESQ2 i vee cs 3
DOB er. 3 TSAO Go I 1871 3 LSQOSs fects 4
ES IB%s cress I TORO i) sik: 2 AA aren ctitets 4 POO A Rtas 3
OPO Aes 3 1 RL G es Ei anGer 2 1873 3 POOS ir act: 3
1830 2 ok ieee sich ie 4 POT Ais s0shs 5 1896 4
TOST Ans keer 2 FOG 2 saint 3 ky A a 5 TOQ9 bis 6
baie Yee roar ° DO SAS at scg: I LO RO). 30-0515 5 TS9S)0 oo: 5 3
POQGy2 css Felc. I POSS escciis. Ae POUT os vukets 7 T8607 os 5
1834 a TOO 253 3 TS 9Oicos: set: 5 EQOOS 255) 21.5 S
1835 3 1857 OSfSES 7G sek sas 6 TOOK si a st 2 3
BOS Oil heres 3 LOSS ss Ys pe Gote lee Ee 3 1902 5
1837 I PS Omsk 5 cate Gaba aaa 2 L903) ee 3
1 heik to) ae Ro 5 1860 5 DOOR nieve 4 TQOAs: ais chen I
1839 ° VBGOR cree is 3 PEO2 es as 3 QOS so, sts bs
1840 3 DOOR 20 ets 2 1884 3 EQOOM 2. 530s °
1841 3 TSO3 i. eae 6 TSS Siete 4 EQO Frc acts I
TOAA RG nuikins 3 VSOR ween 3 1886 7 1908 °
Tease ene, 5 1865. 7 1 Hees ARS eR 6 TQOO. ts. °
TOA es ey eS ESOGs oo. 6 TOSS cre ° —
SAR crates 3 T8697 See TOSOn chests 5 350

This*record on the whole seems to indicate a comparatively uni-
form supply of meteorites, which is the more remarkable when one
considers the various chances affecting the observation of their fall.
The record seems to afford no evidence of cycles or periodicity which
can be traced with certainty. Still the record of years is perhaps not
as satisfactory for establishing conclusions in this regard as is that
of other periods. As the writer has shown elsewhere* at least goo
meteorites probably reach the earth yearly. Of these only an |
average number of three is recorded, so that it is evident that a large
allowance must be made for unrecorded ones. Yet it is fair to pre-
sume that those recorded are typical of the whole, because while
opportunities for observation of meteorite falls have probably con-
tinually increased in number since 1800, the record by decades shows
that the decade from 1860 to 1870 considerably exceeded in number
of falls either of the two succeeding ones.

Passing from the falls by years, the falls by months may be ex-
amined. Such an examination should have an especial significance
in showing the relations which meteorites may have to well-known
star showers. Two of the best known of these showers occur in
August and November. If meteorites are related to these, these
months should show a larger fall than others. If meteorites are not
related to these, no special increase for these months should be shown.

* Pop. Sci. Mon., 1904, pp. 351-354.

JUNE, 1910. Meteorite Stupies II] — Farrincron. 181

On compiling the results it is found that the months of May and
June exhibit the greatest number of falls. The number for Novem-
ber falls below the average and that for August rises only slightly
above. The evidence from this record is therefore that meteorites
are not related to the best known star showers. It is fair to presume
that the record by months will be somewhat influenced by the times
that observers are most abroad. Most of the observations of me-
teorite falls are made in the northern hemisphere and in this hem-
isphere observers are more likely to be out of doors and hence more
likely to observe the fall of meteorites in the summer than in the
winter months. The record shows that as a whole the number of falls
recorded is less for the winter than the summer months, yet the
number of falls cannot be influenced by that alone since the high
record for May and June drops to nearly half that number ‘in July.
Further the months of August, September and October are equally
favorable as regards weather for observations of meteorite falls with
those of April, May and June, yet the latter period much excels the
former in number of falls. The excess of fallsin May and June must,
therefore, be due to other causes than favorable conditions of ob-
servation and seems to indicate that in the portion of the earth’s orbit
passed through in these months there is an unusual number of me-
teorites. The full table for the different months is as follows:

Jan. Feb. Mar. April May June July Aug. Sept. Oct. Nov. Dec.
25 24 22 32 44 45 23 36 30 24 24.5. (23=250
This record is shown graphically in the accompanying diagram, Fig. 2.

SS

] 1 I
z a « c = > > G y °
< ua = a < 5 2 S S 3 3 )
= ire < = 4 Pt < rT) 8 z a

Fig. 2. Curve of meteorite falls by months.

182 Fretp Museum or NaTurRAL History — Geovoey, Vot. III.

Comparison of the falls of meteorites by months as here given with
those of falling stars and fireballs as given by W. H. Pickering * shows
a marked difference of distribution. According to Pickering’s list
the falling stars and fireballs are much more uniformly distributed
through the year than are meteorites and the periods of greatest
number of meteoric falls are from July to November. In May and
June their number is at its minimum. Hence the record seems to
show a difference in character between meteors and meteorites and
furnishes per se a ground for questioning the gradation that has been
supposed to exist between meteors and meteorites.

Tabulation of the falls by days of the year seems to show little
of significance. The largest number of falls for any one day is 5
on October 13, and this is a month when the total number of falls is
not large. Four days show 4 falls each and 158, or nearly half the
total number, no falls at all. The days without falls seem to be scat-
tered indiscriminately through the year, without marked grouping
or arrangement. The days showing falls aside from those mentioned,
have from one to three falls each without any marked grouping that
is apparent. Such a record seems also to indicate that to refer a
meteorite falling on the day of a star shower to such showers is unsafe
practice especially if the observations are not sufficient to assign the
two to the same radiant. The meteorite falls are so uniformly dis-
tributed throughout the year that the two occurrences might easily
be coincident without being otherwise related. The full record of the
falls by days is as follows:

Jan. Feb. Mar. Apr.MayJuneJulyAug.Sept.Oct.Nov.Dec.

De Gosden se 2 I My aaa I Si cee Yale Bee I
BSE Seasons i Spee I 2 sf j ate 2
BE Sarai Sb aes ess 2 2 I oe hety I 2 a
Brod istece te atave, Sears I I ie 52 I Te Gt Ny as I
Boe racsent'e sedate I Ad oie Ane dee e I I
Dire oes acie RR es 2 2 2 he I I I
Bah cis te GRE see ok aes: 2 2 2 I I
Sa itene cc teers I As 3 I Tee. I
Oni seston 2 2 7 ere ame eo 2 at I

POM Eerste hes theron ts 3 3 1 ie I 2 I I I

4 AIR rar kite os I 2 I I 2 I I

£22 Rak. [ aes I Ei 4 I Eee 2

Lgissia et eeeewtaoecestes 2 Bae a a, Tie es 5

DA rictsrctcrsmarnarsteats 5 Ry Name Ve I Ty oe I

Tip sre ogame ate I 2 I 2 I 2 Tn feet I 2

DOs eterece ets I 3 I 2 2 I i

* Popular Astronomy, 1909, 17, 277.

JUNE, 1910. METEORITE STUDIES ITI — FarRINGTON. 183

Jan.Feb.Mar. Apr.MayJuneJulyAug.Sept.Oct.Nov.Dec.

Ea ea gis Soe 2 I aol Siti Sed: SS carpe Wee tore I
IY sta rte scariest 3 CIEE. 2 I , rE se

a CRE Oe ANCE 2 I 2 BS I I 2 I
eS eed cats I sea eer I < I

Rr Rse sores 20s I Faber seat I 2

BAe tesais eter nsione I x re I Bale eee 2
| a aE 3 1 I I I
Dee ote A Fay ore I pape 2 I I

Np Er retiree 2 A Se I I I Et ay I I
BOG che sew bene 3 2 ses I I Et ays
Bea cies satan pee I I PS ees I I i
Mees ligt 6 Bite, 8 I I 2 I 3 ra 1 Oe ee SR

2 Uae ete I I I I 3 I

RON pn cla a cco I I I I : 4

ang aes a Shas a 2 I I I

eae eee

23° 99° 32" 90 4k. . 2a 8... 98- 08, 24-03; 40.324
Of all times of fall of meteorites the most satisfactory for study
are probably the hours of fall, since the ratio of number of falls to
number of hours is larger than to days, months, or years. As is well
known, the hours of fall show the direction of movement of meteor-
ites, since (with a few minor possible obvious exceptions) meteorites
falling from noon to midnight, or afternoon falls, as they may be
called, must be moving in the same direction as the earth; while those
falling between midnight and noon, or forenoon falls, are moving in
a direction opposite to that of the earth or else at a speed so slow that
they are overtaken by it. While the hour of fall is not known of as
many meteorites as is the year and month, yet of 273 sufficiently sat-
isfactory records are available. Of these 273 falls 184 occurred in the
time from noon to midnight, and 89 from midnight to noon. The
record in full is as follows, the total number being less by seven than
that recorded for forenoon and afternoon, since of these seven the
hour is not known:

BOUTS, oo 80 3% F2 De R a e ea BO a ey ~ Total
foe | a ae eas I Bi Se Os a 9 ESE IO Gas kge swe OO
1” SOP airs 4 ES ROE Ft SEER EE a BOS Oe a gene eat LG

As in the case of the months and the years, it is quite likely that
here also considerable allowance should be made for conditions of
observation. It is reasonable to expect that the number of falls
recorded in the early morning hours would be less than that for other
times, since mankind is generally asleep then. That some such allow-
ance must be made is indicated by the records, for the number of falls
from midnight to 6 A. M. is only 21, while from 6 A. M. to noon it is 68;

184 Fretp Museum or Natura. History — GEotoey, Vor. III.

from noon to 6 P: M. 124, and from 6 P. M. to midnight 60. Hence it
seems probable that some of the diminution in the number of falls
is due to lack of observers, although Newton* seemed to conclude
from studies of the orbits of the morning falls that lack of observ-
ers had little to do with their scarcity. Lack of meteorites during
morning hours may also be due in part, as Newton suggested, to the
fact that such as have retrograde motion are more likely to be burned
up by the greater velocity with which they strike the earth’s atmos-
phere. This increase in velocity is not so great as might be supposed
since Lowell has shown f that it cannot exceed 2.66 miles per second.
Yet Pickering t thinks it is sufficient to destroy all that have retro-
grade motion, or that the velocity of such as have retrograde motion
would be higher than any that has yet been recognized. It is not
clear how such an increase would be very apparent if this increase at
most is only 2.66 miles per second. On account of the above proba-
bilities Pickering is of the opinion that most if not all of the meteorites
which fall in the morning hours are moving at so slow a speed that
they are overtaken by the earth. Schiaparelli, who gave the matter
much study and to whom we are indebted for extensive researches
in the relations between comets and meteors, concluded that many
meteorites had hyperbolic velocities and hence must come from the
world of fixed stars rather than from comets or the solar system. ||
Newton assigned to the stone of Stannern a velocity of 45 miles per
second, and concluded that most meteorites are allied to short period
comets in their velocities.§ Pickering {| regards it doubtful whether
any stony meteorites move fast enough to be accredited with cometary
velocities.

The hourly falls of the writer’s table are shown plotted in Plate LIX.
It will be observed that the peak of the falls occurs at 3 P.M. Picker-
ing has shown ** that other things being equal the greatest number of
meteorites would be expected when the Earth’s quit is highest above
the horizon and that this occurs. for the northern hemisphere, longi-
tude go°, at 3 Pp. M., May 6. This high point agrees with.that of the
greatest number of meteorites, for they are most numerous in May

* Am. Jour. Sci., 1888, 3, 36, 10.

T Science, N. S., 1909, 30, 339-

t Popular Astronomy, 1910, 18, 264.

|| Entwurf einer Astronomischen Theorie der Sternschnuppen. Boguslaw-
ski’s translation, 1871, p. 228.

§ Am. Jour. Sci., 1888, 3, 36, 11, and 13.

{ Popular Astronomy, 1910, 18, 276.

¥* Od. cit., p. 272.

0 haa

JuNE, 1910. MeErTeEorRITE Stupies III — FarrRincrTon. 185

and at3p.M. Itmay also be remarked that the writer has shown that
meteorites are most numerous in mountain regions,* so that the high
points seem in every respect to be the most successful in acquiring
meteorites.

It would be possible from the writer’s data to compare falls at
different intervals and for different periods in order to determine
whether various periods agree in times of fall. Such examination of
the records as the writer has made shows that the distribution of the
falls is about the same in all the periods. In order to secure inde-
pendent testimony on this point the writer’s results may be compared
with those of Haidinger, whoin 1867 f gave the hours of 178 meteorite
falls. His table was as follows:

12 BOS ao a eB a aes. cee We FOR TE

area oer I 3 2 2 4 5 4-13 5 7 ee 5 ae ey 2
Be eos Ss cies ein st Simp STS: Vanes eee ea «ao <n ~ D0. s* -m 104

. On examination of these falls by name, however, it appears that
some are assigned times of fall which later investigation has shown
to be unreliable, as is true of the meteorite of Mincy for example and
others listed are not now recognized as meteoritic. For these reasons
about 40 falls must be eliminated from Haidinger’s list. Omitting
these the result is as follows:

$92 eee ee 6 Or Rs ® S tO: BE

yp | © hae ON SSS aelEiods Eye kt ee ay SBR EOL OR Re eR TE Yat
Se Sakis ces J PaCS! TSO Ae ek Seg aN eet, (oR Taba «Ds Bee Te

An excess of afternoon over forenoon falls is seen here as in the
writer’s list, although the proportion is less, it being nearly 2:1 in
the writer’s list and 1.4:1 in Haidinger’s list. More significant
perhaps is the fact that both lists show an excess of falls at 7 A. M.,
II A. M., and 3 P. M.

On the whole the study of the times of fall of meteorites in the
manner here adopted seems to show (1) that they differ considerably
from meteors in times of fall, (2) that they are not noticeably related
to any of the well known star showers and (3) that the rate of their
supply to the earth is remarkably uniform.

57
81

LIST OF METEORITES OF THE UNITED STATES OF
AMERICA BY STATES.

The following list comprises the meteorites of the United States as
at present known, grouped by States. Great care has been taken in

* Pop. Sci. Mon., 1904, p. 352.
{ Sitzb. Kais. Akad. der Wiss. Wien. Bd. 55.

‘

186 FreLtp Museum or NaTuRAL History — Geo oey, Vot. III.

the preparation of this list to include only meteorites which may
properly be regarded as separate falls, and on the other hand to
include all that should be so regarded. It is thought that such a list
will be useful for reference and tend toward uniformity of nomencla-
ture. The classification of each meteorite according to Brezina’s
system, so far as known, is shown by abbreviations, the full forms of
which are as follows:

Cc. Stone, Spherulitic chondrite.

Cea. Stone, Veined spherulitic chondrite.
Ceb. Stone. Breccia-like spherulitic chondrite.
Ceo, Stone, Ornans spherulitic chondrite.
Cck. Stone, Crystalline spherulitic chondrite.
Cg. Stone, Gray chondrite.

Cga. Stone, Veined gray chondrite.
Cgb. Stone, Breccia-like gray chondrite.
Chla. Stone, Veined chladnite.

Cho. Stone, Howarditic chondrite.

Ci: Stone, Intermediate chondrite.

Cia, Stone, Veined intermediate chondrite.
Cib. Stone, Breccia-like intermediate chondrite.
Ck: Stone, Crystalline condrite.

Cka. Stone, Veined crystalline chondrite.
Ckb. Stone, Breccia-like crystalline chondrite.
Ca; Stone, Black chondrite.

Csa: Stone, Veined black chondrite.

Csb. Stone, Breccia-like black chondrite.

Cw. Stone, White chondrite.

Cwa. Stone, Veined white chondrite.

Cwb. Stone, Breccia-like white chondrite.

1: Iron, Ataxite.

Db. Iron, Babb’s Mill ataxite.

De. Iron, Cape ataxite.

D1. Iron, Linville ataxite.

Dn. Iron, Nedagolla ataxite.

Dr. Iron, Rafruti ataxite.

Ds. Iron, Siratik ataxite.

Dsh. Iron, Shingle Springs ataxite.

Diz Iron, Tucson ataxite.

ipl Iron, Hexahedrite.

Ha: Iron, Granular hexahedrite.

Hb. Iron, Breccia-like hexahedrite.

Ho. Stone, Howardite.

Ke. Stone, Carbonaceous, spherulitic chondrite.
M. Iron-stone, Mesosiderite.

Mg. Iron-stone, Grahamite.

O. Iron, Octahedrite.

Of: Iron, Fine octahedrite.

June, r910. Meteorite Stupies lI] — FarrincTon. 187

Off. Iron, Finest octahedrite.

Offbp. Iron, Breccia-like finest octahedrite.
Og. lron, Coarse octahedrite.

Ogg, Iron, Coarsest octahedrite.

Oh. Iron, Hammond octahedrite.

Om. Iron, Medium octahedrite.

¥; Iron-stone, Pallasite.

Pi. Iron-stone, Imilac pallasite.

Pk. Iron-stone, Krasnojarsk pallasite.
Pr. Iron-stone, Rokicky pallasite.

LIST OF METEORITES BY STATES

ALABAMA.
Auburn, Lee Co., H. 32° 37’ N. 85° 32’ W., found 1867.
Chulafinnee, Cleburne Co., Om. 33° 35’ N. 85° 42’ W.. found 1873.
Danville, Morgan Co., Cga. 34° 24’ N. 87° 5’ W., fell Nov. 27, 1868.
Desotoville, Choctaw Co., H. 32° 13’ N. 88° 10’ W., found 1859.
Felix, Perry Co., Kc. 32° 33’ N. 87° 12’ W., fell May 15, 1900.
Frankfort, Franklin Co., Ho. 34° 30’ N. 87° 52’ W., fell Dec. 5, 1868.
Leighton, Colbert Co., Cgb. 34° 40’ N. 87° 35’ W., fell Jan. 12, 1907.
Limestone Creek, Monroe Co., Dc. 31° 34’ N. 87° 30’ W., found 1834.
Selma, Dallas Co., Cc. 32° 25’ N. 87° W., found 1906.
Summit, Blount Co., Ha. 34° 13’ N. 86° 30’ W., found 1890.
Walker County, H. 33° 50’ N. 87° 15’ W., found 1832.
Stones, 5; irons 6; total, rr. Observed falls, 4.

ARKANSAS.

Joe Wright Mountain, Independence Co., Om. 35° 43’ N. 91° 27’ W., found
1884.

Cabin Creek, Johnson Co., Om., 35° 24’ N. 93° 17’ W., fell March 27, 1886.

Stones, 0; irons 2; total, 2. Observed falls, 1.

ARIZONA.

Canyon Diablo, Coconino Co., Og. 35° 10’ N. 111° 7’ W., found 1891.
Coon Butte, Coconino Co., Cib. 35° ro’ N. 111° 7’ W., found 1906.
Tucson, Pima Co., Dt. 32° 12’ N. 110° 35’ W., found 1851.

Weaver, Maricopa Co., Dt. 33° 58’ N 112° 35’ W., found 1898.
Stones, 1; irons 3; total 4. Observed falls. o.

CALIFORNIA.
Canyon City, Trinity Co., Og. 40° 35’ N. 123° 5’ W., found 1875.
Ivanpah, San Bernardino Co.. Om. 35° 30’ N. 115° 28’ W., found 1880.
Oroville, Butte Co., Om. 39° 18’ N. 122° 38’ W., found 1893.
San Emigdio Ranye, San Bernardino Co., Cc., found 1887.
Shingle Springs, El Dorado Co., Dsh. 38° 43’ N. 120° 53’ W., found 1869.
Surprise Springs, San Bernardino Co., Om. 34° 12’ N. 115° 54’ W.. found,
_ 1899. .
Stones, 1; irons, 5; total, 6. Observed falls, o.

188 Fre_tp Museum or NaTurRAL History — Geovoey, Vot. III.

COLORADO.

Bear Creek, Jefferson Co., Of. 39° 38’ N. 105° 16’ W., found 1866.
Franceville, El Paso Co., Om. 38° 48’ N. 104° 35’ W., found 1890.
Guffey, Park Co., Dr 38° 45’ N. 105° 30’ W., found 1907.

Russel Gulch, Gilpin Co., Of. 39° 47’ N. 105° 31’. W., found 1863.
Ute Pass, Summit Co., Ogg. 39° 48’ N. 106° 10’ W., found 1894.
Stones, 0; irons, 5; total, 5. Observed falls, o.

CONNECTICUT.

Weston, Fairfield Co., Ccb. 41° 13’ N. 73° 27’ W., fell Dec. 14, 1807.
Stones. 1; Irons, 0; total. 1. Observed falls, 1.

GEORGIA

Canton, Cherokee Co., Ogg. 34° 12’ N. 84° 30’ W., found 1894.

Dalton, Whitfield Co., Om. 34° 59’ N. 84° 54’ W., found 1877.
Forsyth, Monroe Co., Cwa. 33° 3’ N. 83° 56’ W., fell May 8, 1829.
Hollands Store, Chattooga Co., Ha. 34° 22’ N. 85° 26’ W., found 1887.
Locust Grove, Henry Co., Ds. 33° 20’ N. 84° 8’ W., found 1857.
Losttown Creek, Cherokee Co., Om. 34° 10’ N. 84° 32’ W., found 1868.
Lumpkin, Stewart Co., Cck. 31° 54’ N. 84° 57’ W., fell Oct. 6, 1869.
Pickens County, Cck. 34° 30’ N. 84° 28’ W., found 1908.

Putnam County, Of. 33° 16’ N. 83° 25’ W., found 1839.

Thomson, McDuffie Co., Cga. 33° 23’ N. 82° 30’ W., fell Oct. 15. 1888.
Union County, Ogg. 34° 56’ N. 83° 58’ W., found 1853.

Stones, 4; irons, 7; total, 11. Observed falls, 3.

IDAHO.

Hayden Creek, Lemhi Co., Om. 45° 0’ N. 113° 45’ W., found 1895.
Stones, 0; irons, 1; total, 1. Observed falls, o.

INDIANA.

Harrison County, Cho. 38° 12’ N. 86° 8’ W.., fell March 28, 1859.
Kokomo, Howard Co., De. 40° 34’ N. 86° 2’ W., found 1862.
Plymouth, Marshall Co., Om. 41° 20’ N. 86° 18’ W., found 1893.
Rochester, Fulton Co., Cc. 41° 5’ N. 86° 13’ W.., fell Dec. 21, 1876.
Rushville, Rush Co., Cg. 39° 22’ N. 85° 3’ W., found 1860.

South Bend, St. Joseph Co., Pi. 41° 40’ N. 86° 15’ W., found 1893.
Stones, 3; iron-stones, 1; irons, 2; total, 6. Observed falls, 2.

IOWA.

Estherville, Emmet Co., M. 43° 24’ N. 94° 50’ W., fell May 10, 1879.
Forest City, Winnebago Co., Ccb. 43° 17’ N. 93° 38’ W., fell May 2, 1890.
Homestead, Iowa Co., Cgb. 41° 39’ N.‘91° 32’ W., fell Feb. 12, 1875.
Marion, Linn Co., Cwa.-41° 57’ N. 91° 34’ W., fell Feb. 25, 1847.

Stones, 3; iron-stones, 1; irons,o; total,4. Observed falls, 4.

KANSAS.
Admire, Lyon Co., Pr. 33° 0’ N. 96° 5’ W., found 1891.
Brenham, Kiowa Co., Pk. 37° 38’ N. 99° 13’ W., found 1885.
Elm Creek, Lyon Co., Cco. 38° 40’ N. 96° 5’ W., found 1906.

apn aly

JUNE, 1910. Meteorite Stupies [il — FaRRINGTON.

189

Farmington, Washington Co., Csa. 39°48’ N. 97° 5’ W., fell June 25, 1890.

Jerome, Gove Co., Cck. 38° 47’ N. 100° 14’ W., fell Apr. 10, 1894.
Long Island, Phillips Co., Ck. 39° 56’ N. 99° 34’ W., found 1891.
Modoc, Scott Co., Cga. 38° 30’ N. 100° 55’ W., fell Sept 2, 1905.
Ness County, Cib. 38° 30’ N. 99° 37’ W., found 1897.

Oakley, Logan Co., Ck. 38° 55’ N. 101° o’ W., found 1895.
Ottawa, Franklin Co., Cho. 38° 37’ N. 95° 18’ W., fell Apr. 9, 1896.

Prairie Dog Creek, Decatur Co., Cck. 39° sof N. 100° 24’ W., found 1893.

Saline, Sheridan Co., Cck. 39° 22’ N. 100° 27’ W., fell Nov. 15, 1898.
Scott, Scott Co., 38° 30’ N. 100° 55’ W., found 1905.

Tonganoxie, Leavenworth Co., Om. 39° 8’ N. 95° 7’ W., found 1886.
Waconda, Mitchell Co., Ccb. 39° 20’ N. 98° 10’ W., found 1873.
Stones, 12; iron-stones, 2; irons, 1; total 15. Observed falls, 5.

KENTUCKY.

Bath Furnace, Bath Co., Cia. 38° 2’ N. 83° 37’ W., fell Nov. 15, rgo2.
Casey County, Og. 37° 20’ N. 84° 55’ W., found 1877.

Cynthiana, Harrison Co., Cg. 38° 24’ N. 84° 16’ W., fell Jan. 23, 1877.
Eagle Station, Carroll Co., Pr. 38° 37’ N. 85° o’ W., found 1880.
Frankfort, Franklin Co., Om. 38° 7’ N. 84° 57’ W., found 1866.
Kenton County, Om. 38° 40’ N. 84° 29’ W., found 1889.

La Grange, Oldham Co., Of. 38° 37’ N. 85° 25’ W., found 1860.
Marshall County, Om. 36° 50’ N. 88° 17’ W., found 1860.

Mount Vernon, Christian Co., Pk. 36° 50’ N. 87° 28’ W., found 1868.
Nelson County, Ogg. 37° 48’ N. 85° 27’ W., found 1860.

Salt River, Bullitt Co., Off. 37° 56’ N. 85° 54’ W., found 1850.
Scottsville, Allen Co., H. 36° 45’ N. 86° 10’ W., found 1867.
Smithland, Livingston Co., Db. 37° 18’ N. 88° 17’ W., found 1839.
Williamstown, Grant Co., Om. 38° 35’ N. 84° 30’ W., found 1892.
Stones, 2; iron-stones, 2; irons, 10; total, 14. Observed falls, 2.

MAINE.
Andover, Oxford Co., Cc. 44° 36’ N. 70° 47’ W.., fell Aug. 5, 1898.
Castine, Hancock Co., Cwa. 44° 24’ N. 68° 48’ W., fell May 20, 1848.
Nobleborough, Lincoln Co., Ho. 44° 4’ N. 69° 28’ W.., fell Aug. 7, 1823.
Searsmont, Waldo Co., Cc. 44° 22’ N. 69° 12’ W.., fell May 21, 1871.
Stones, 4; irons, 0; total, 4. Observed falls, 4

MARYLAND.
Emmitsburg, Frederick Co., Om. 39° 43’ N. 77° 20’ W., found 1854.
Lonaconing, Allegheny Co., Og. 39° 28’ N. 79° 2’ W., found 1888.
Nanjemoy, Charles Co., Cc. 38° 25’ N. 77° 12’ W., fell Feb. 10, 1825.
Stones, 1; irons, 2; total, 3. Observed falls, 1

: MICHIGAN.
Allegan, Allegan Co., Cco. 42° 34’ N. 85° 52’ W.., fell July ro, 1899.
Grand Rapids, Kent Co., Of. 42: 59’ N. 85° - W., found 1883.
Reed City, Osceola Co., Oh. 43° 53’ N. 85° 32’ W.., found 1895.
Stones, 1; irons, 2; total, 3. Observed falls. 1.

190 Fretp Museum or Natura History — Geovoey, Vot. III.

MINNESOTA
Arlington, Sibley Co., Om. 44° 30’ N. 93° 56’ W., found 1894.
Fisher, Polk Co., Cia. 47° 48’ N. 96° 49’ W., fell April 9, 1894.
Stones.1; irons,1; total,2. Observed falls, 1.

MISSOURI.
Billings, Christian Co., Om. 37° 5’ N. 93° 28’ W., found 1903.
Butler, Bates Co., Off. 38° 18’ N. 94° 25’ W., found 1874.
Cape Girardeau, Cape Girardeau Co., Cc. 37°13’ N. 89° 32’ W., fell Aug. 14,
1846.
Central Missouri, Ogg. Central portion of state, found 1855.
Little Piney, Pulaski Co., Cc. 37° 55’ N. 92° 5’ W., fell Feb. 13, 1839.
Mincy, Taney Co., M. 36° 35’ N. 93° 7’ W., found 1856.
Saint Francois County, Og. 37° 55’ N. go° 36’ W., found 1863.
Saint Genevieve County, Of. 37° 47’ N. 90° 22’ W., found 1888.
Warrenton, Warren Co., Cco. 38° 44’ N. 91° 12’ W., fell Jan. 3, 1877.
Stones, 3; iron-stones, 1; irons, 5; total, 9. Observed falls, 3.

MONTANA.

Illlinois Gulch, Deer Lodge Co., Dn. 46° 39’ N. 112° 32’ W., fell 1897.
Stones, 0; irons, 1; total, 1. Observed falls, o.

NEBRASKA.
Ainsworth, Brown Co., Om. 42° 30’ N. 99° 50’ W., found 1907.
Mariaville, Rock Co., Iron, 42° 45’ N. 99° 25’ W., desc. 1897.
Ponca Creek, Boyd Co., Ogg., desc. 1863.
Redwillow County, Iron, desc., 1897.
York, York Co., Iron, 40° 52’ N. 97° 33’ W., found 1878.
Stones, 0; irons, 5; total, 5. Observed falls, o.

NEVADA.

Quinn Canyon, Nye Co., Om. 38° 30’ N. 115° 20’ W., found 1908.
Stones, 0; irons, 1; total, 1. Observed falls, o.

NEW JERSEY.

Deal, Monmouth Co., Ci. 40° 14’ N. 74° 1’ W., fell Aug. 14, 1829.
Stones, 1; irons, 0; total, 1. Observed falls, 1.

NEW MEXICO.

Costilla, Taos Co., Om. 36° 50’ N. 105° 13’ W., found 1881.

El Capitan, Lincoln Co., Om. 33° 30’ N. 105° 30’ W., found 1893.

Glorieta Mountain, Santa Fe Co., Om. 35° 22’ N. 105° 50’ W., found 1884.
Luis Lopez, Socorro Co., Om. 34° 0’ N. 107° o’ W., found 1896.

Oscuro Mountains, Socorro Co., Og. 33° 45’ N. 107° 20’ W., found 1895.
Sacramento Mountains, Otero Co., Om. 32° 32’ N. 105° 20’ W., found 1896.
Stones, 0; irons, 6; total6. Observed falls, o.

NEW YORK.

Bethlehem, Albany Co., Cck. 42° 6’ N. 73° 47’ W., fell Aug. 11, 1859.
Burlington, Otsego Co., Om. 42° 40’ N. 75° 8’ W., found 1819.

June, 1910. Mereorite Stupres lil — FarrInGTOoN. IgI

Cambria, Niagara Co,. Of. 43° 13’ N. 78° 45’ W., found 1818.

Seneca Falls, Seneca Co., Om. 42° 57’ N. 76° 58’ W., found 1850.
Tomhannock Creek, Rensselaer Co., Cgb. 42° 52’ N. 73° 36’ W., found 1863.
Stones, 2; irons, 3; total, 5. Observed falls, r.

NORTH CAROLINA.

Asheville, Buncombe Co., Om. 35° 36’ N. 82° 31’ W., desc. 1839.

Black Mountain, Buncombe Co., Og. 35° 53’ N. 80° 3’ W., found 1839.
Bridgewater, Burke Co., Of. 35° 45’ N. 81° 53’ W., found 1890.

Castalia, Nash Co., Cgb. 36° 4’ N. 78° 4’ W.., fell May 14, 1874.

Colfax, Rutherford Co., Om. 35° 18’ N. 81° 45’ W., found 1880.

Cross Roads, Wilson Co., Cg. 35° 38’ N. 78° 7’ W., fell May 24, 1892.
Deep Springs, Rockingham Co., Db. 36° 20’ N. 79° 35’ W., found 1846.
Duel Hill, Madison Co., Og. 35° 51’ N. 82° 44’ W., found 1873.

Ferguson, Haywood Co., Stone, 35° 36’ N. 83° 0’ W., fell July 18, 1889.
Flows, Cabarrus Co., Cga. 35° 18’ N. 89° 33’ W., fell Oct. 31, 1849.
Forsyth County, Dn. 36° 8’ N. 80° 20’ W., found 1895.

Guilford County, Om. 36° 4’ N. 79° 48’ W., desc. 1822.

Hendersonville, Henderson Co., Cc. 35° 19’ N. 82° 28’ W., found rgotr.
Jewel Hill, Madison Co., Of. 35° 49’ N. 82° 45’ W., found 1854.

Lick Creek, Davidson Co., H. 35° 40’ N. 80° 12’ W., found 1879.

Linville, Burke Co., Dl. 35° 48’ N. 81° 55’ W., found 1882.

Murphy, Cherokee Co., H. 35° 6’ N. 84° 2’ W., found 1899.

Persimmon Creek, Cherokee Co., Offbp. 35° 3’ N. 84° 4’ W., found 1893.
Smith’s Mountain, Rockingham Co., Of. 36° 32’ N. 79° 58’ W., found 1863.
Stones, 5; irons, 14; total, 19. Observed falls, 4.

NORTH DAKOTA.
Jamestown, Stutsman Co., Of 46° 42’ N. 98° 34’ W., found 1885.
Niagara, Grand Forks Co., Og. 47° 58’ N. 97° 52’ W., found 1879.
Stones, 0; irons, 2; total, 2. Observed falls, o.

OHIO.

Anderson Township, Hamilton Co., P. 39° 10’ N. 84° 18’ W., desc. 1884.
Cincinnati, Hamilton Co., Ds. 39° 7’ N. 84° 29’ W., desc 1808.
Hopewell Mounds, Ross Co., Om. 39° 10’ N. 83° 20’ W., desc. 1902.

New Concord, Guernsey Co., Cia. 39° 58’ N. 81° 44’ W., fell May 1, 1860.
Pricetown, Highland Co., Cw. 33° 11’ N. 83° 44’ W., fell Feb. 13, 1893.
Wooster, Wayne Co., Om. 40° 48’ N. 81° 58’ W , found 1858.

Stones, 2; ironstones, 1; irons, 3; total, 6. Observed falls, 2.

OREGON.

Port Orford, Curry Co., P. 42° 46’ N. 124° 28’ W., found 1859.
Willamette, Clackamas Co., Om. 45° 22’ N. 122° 35’ W., found rgoz.
Stones, 0; ironstones, 1; irons, 1; total, 2. Observed falls, o.

PENNSYLVANIA.
Bald Eagle, Lycoming Co., Om. 41° 12’ N. 77° 5’ W., found 1891.
Mount Joy, Adams Co., Ogg. 39° 44’ N. 77° 20’ W., found 1887.

192 Fretp Museum or NaturAL History — Geo.oecy, Vor. III.

Pittsburg, Allegheny Co., Ogg. 40° 27’ N. 79° 57’ W., found 1850.
Shrewsbury, York Co., Om. 39° 45’ N. 76° 35’ W., found 1907.
Stones, 0; irons, 4; total, 4. Observed falls, o.

SOUTH CAROLINA.
Bishopville, Sumter Co., Chla. 34° 12’ N. 80° 18’ W., fell Mar. 25, 1843.
Chesterville, Chester Co., Dn. 34° 42’ N. 81° 15’ W., found 1847.
Laurens County, Off. 34° 30’ N. 82° 14’ W., found 1857.
Lexington County, Og. 33° 57’ N. 81° 18’ W., found 1880.
Ruff’s Mountain, Newberry Co., Om. 34° 15’ N. 81° 21’ W., found 1844.
Stones, 1; irons, 4; total, 5. Observed falls, 1.

SOUTH DAKOTA.
Bath, Brown Co., Ccb. 45° 27’ N. 98° 19’ W., fell Aug. 29, 1892.
Fort Pierre, Stanley Co., Om. 44° 23’ N. 100° 46’ W . found 1856.
Stones, 1; irons, 1; total, 2. Observed falls, 1.

TENNESSEE.

Babb’s Mill, Greene Co., Db. 36° 18’ N. 82° 54’ W., found 1842.
Carthage, Smith Co., Om. 36° 20’ N. 85° 56’ W.. found 1844.
Charlotte, Dickson Co., Of. 36° 13’ N. 87° 20’ W., fell Aug. 1, 1835.
Cleveland, Bradley Co., Om. 35° 8’ N. 84° 53’ W., found 1860.
Coopertown, Robertson Co., Om. 36° 25’ N. 87° o’ W., found 1860.
Cosby Creek, Cocke Co., Og. 35° 48’ N. 83° 15’ W., found 1837.

Crab Orchard, Cumberland Co., Mg. 35° 53’ N. 84° 48’ W., found 1887.
Drake Creek, Sumner Co., Cwa. 36° 18’ N. 86° 34’ W., fell May 9. 1827.
Jackson County, Om. 36° 25’ N. 85° 37’ W., found 1846.

Jonesboro, Washington Co., Of. 36° 16’ N. 82° 30’ W., found 1891.

. Morristown, Hamblen Co., Mg. 36° 9’ N. 83° 24’ W., found 1887.
Murfreesboro, Rutherford Co., Om. 35° 50’ N. 86° 20’ W., found 1847.
Petersburg, Lincoln Co., Ho. 35° 20’ N. 86° 38’ W.., fell Aug. 5, 1855.
Smithville, Dekalb Co., Og. 35° 55’ N. 85° 46’ W., found 1840.
Tazewell, Claiborne Co., Off. 36° 27’ N. 83° 48’ W., found 1853.
Wallens Ridge, Claiborne Co., Og. 36° 30’ N. 83° 30’ W., found 1887.
Stones, 2; ironstones, 2; irons, 12; total, 16. Observed falls, 3.

TEXAS.

Bluff, Fayette Co.. Ckb. 29° 52’ N. 96° 48’ W., found 1878.
Carlton, Hamilton Co., Off. 31° 50’ N. 98° 10’ W., found 1887.
Denton County, Om. 33° 14’ N. 97° 8’ W. found 1856.

Estacado, Crosby Co., Cka. 33° 35’ N. 101° 30’ W., found 1906.
Fort Duncan, Maverick Co., H. 28° 35’ N. 100° 24’ W., found 1852.
Iredell, Bosque Co., H. 31° 53’ N. 97° 52’ W., found 1898.

Kendall County, Hb. 29° 24’ N. 98° 30’ W., found 1887.
MacKinney, Collin Co., Cs. 33° 9’ N. 96° 45’ W., found 1870.

Mart, McLennan Co., Off. 31° 10’ N. 96° 45’ W., found 1898.

Pipe Creek, Bandera Co., Cka. 29° 43’ N. 98° 56’ W., found 1887.
Red River, Om. 32° 7’ N. 95° 10’ W., found 1808.

San Angelo, Tom Green Co., Om. 31° 20’ N. 100° 20’ W., found 1897.

td
MereoritTe Stupies Il] — FarRINGTON. 193

San Pedro Springs, Bexar Co., Cw. 29° 27’ N. 98° 27’ W., found 1887.
Travis County, Cs. 30° 20’ N. 97° 29’ W., found 1890.

Wichita County, Og. 34° 0’ N. 98° 40’ W., found 1836.

Stones, 6; irons, 9; total, 15. Observed falls, o.

UTAH.

Salt Lake City, Salt Lake Co., Cgb. 40° 58’ N. 111° 25’ W., found 186y.
Stones 1; irons, 0; total, 1. Observed falls, o.

VIRGINIA.

Botetourt County, D. 37° 30’ N. 79° 50’ W., found 1850.

Cranberry Plains, Giles Co., O. 37° 13’ N. 80° 47’ W., found 1852.
Hopper, Henry Co., Om. 36° 35’ N. 79° 45’ W., found 1889.

Indian Valley, Floyd Co., Ha. 36° 58’ N. 80° 39’ W., found 1887.
Richmond, Henrico Co., Cck. 37° 29’ N. 77° 28’ W., fell June 4, 1828.
Staunton, Augusta Co., Om. 38° 14’ N. 79° 1’ W., found 1858.
Stones, 1; irons, 5; total.6 Observed falls, r.

WEST VIRGINIA.

Greenbrier County, Og. 37° 32’ N. 80° 18’ W., found 1880.
Jennie’s Creek, Wayne Co., Og. 37° 53’ N. 82° 22’ W., found 1883.
Stones, 0; irons, 2; total, 2. Observed falls, o.

WISCONSIN.

Algoma, Kewaunee Co., Om. 44° 30’ N. 87° 30’ W., found 1887.
Hammond, St. Croix Co., Oh. 44° 55’ N. 92° 22’ W., found 1884.
Trenton, Washington Co., Om. 43° 20’ N. 88° 12’ W., found 1858.
Vernon County, Cka., 43° 30’ N. 91° 10’ W., fell Mar. 26, 1865.
Stones, 1; irons, 3; total, 4. Observed falls, r.

-

WYOMING.

Silver Crown, Laramie Co., Og. 41° 10’ N. 105° 20’ W., found 1887.
Stones, 0; irons, 1; total, 1. Observed falls, o.

‘LX ‘BSLINVOSLSW NOLHDIS7 JO NOILOSS ‘Z ‘DIY '’6X ‘“ZLINOSLAW NOLHDIS “| Oly

‘Al 3LV1d ‘Il *IOA ‘AD07103D “AMYOLSIH IWHNLYN JO WN3SSNW Q13i4

LIBRARY
UNIVERSITY OF ILLINGIS
URBANA

‘lly X "ALIYOSLAIW NOANVO NNIN® 4O 3GIG LNOYS

‘IAT ALWid ‘Ill “TOA £AD01039 ‘AY LSIH WHNLVYN JO WN3SSNW O13!I4

LIBRARY
UNIVERSITY OF ILLINUIS
URBANA

FIELD MUSEUM OF NATURAL HISTORY. GEOLOGY, VOL. Ill, PLATE LVII.

SIDE VIEW OF QUINN CANYON METEORITE. xX 14.

LIBRARY
UNIVERSITY OF ILLiNUIS
URBANA

"114 X “BLINOSL3EW NOANVYD NNIN® 4O 3aig YyvaYy

“IAT 3Lvid ‘Hl “TOA ‘AD071039 “AMYOLSIH IVWYNLYN JO WN3SNW O13I3

LIBRARY
UNIVERSITY OF iLLINGIS
IRBANA

FIELD MUSEUM OF NATURAL HISTORY. GEOLOGY, VOL. Ill, PLATE LIX.

35
34
33
32
31
30
29
28
27
26
25
24
23
22
21

tt
i]

—_—
ao N @ 6

-_—_— =|-_ —_
Nw » w

-
=~ nw waraunan eso o

Bee eS eS Ord SO NO. ANAS. B23 4S OF 38. O18 TE 82

A. M. P. M.

Curve OF METEORITE FALLS BY Hours.

<3

AMOERT

NOt > le a . ;

< at : be Newent <4 BS raun® = van,
oe : ae : — Se. . 3 : 23
Y ave EAP SOF Fanner (Gee ge Feneey

Y.

a 3

<
a

DES ouNe,

g Ag f Q

ty oon

ee 5 ae . Se ae. a} , - et <P, :
ys — AQER ya! E32 (Fh > “24 rt . : 7 a4 ; t— ~s
Ry SON FRY SOAR RY NERY YF ORY SUA DENY SONA MMOERY Peaneny ey Uwe ny ;

yi
°
Oo

xe.

c

LIAN EMO Way 4 “ aunt 9
*

Shi.

Aeac®
case
8 8004

a Oy
~
S

:

kip

So FERES
Be

Ds.

Mi,

Oy

AMOER

«

hr
cS
x/

at
%,

a) cace

A
~
3

y
=
=
K

a)
>
aI :
“ds

TT oe
e 800,

aS
Oe
x

3h 8 —— t * ae . Sh . fi : -

> = “= FSO ERO ERD 0 ERAS Y, = 26 :

+ OA WDER, Me WOERY SG NROERY SG \ROERY NS . mDeRE
2 ne AKO MY, Maw SN . v P < 2 La pp

VEN Nee
: Nos waant

OD,

<=
Ls]

ES, 4 ay : ese ees

yas

acd

eBay
., nore

wt

ae

\
aoe nen. Waasan
eave sore Pee
opr ig

“ ; St
Met Gee Ry Be
; 4 (on le

2 ‘

=

OA it a
Seton tes) Shiau

sige cori

oy
rd ¥e
fe a

UNIVERSITY OF ILLINOIS-URBANA

INIA

3 0112 084203220