350 
 
 >*• *' 
 
 t 
 
 ILLINOIS STATE 
 
 LABORATORY 
 OF NATURAL HISTORY 
 
 LIBRARY 
 
 <+t+444*4*4+4+t+4444^+ 
 
 L I G> RARY 
 
 OF THL 
 
 U N I VER.SITY 
 
 OF ILLINOIS 
 
 'URAL HISTORY SURVI 
 
 550.5 
 
 FI 
 v.3, cop.Q. 
 
 REMOTE gf QRAGi 
 
 R 
 
4 
 
LIBRARY 
 
 UNIVERSITY OF ILLINOIS 
 
 URBANA 
 
Field Museum of Natural History. 
 Publication 145. 
 Geological Series. Vol. Ill, No. 
 
 METEORITE STUDIES III 
 
 BY 
 
 Oliver Cummings Farrington. 
 
 Curator, Department of Geology. 
 
 Chicago, U. S. A. 
 
 June 1, 1910. 
 
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]/ 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 stone in the air. The large fractured 
 surface is roughly triangular in shape with sides about 3 inches (7.5 
 cm.) in length. The encrusted surfaces of the stone are all smoothed 
 
 165 
 
166 Field Museum of Natural History — Geology, 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 Studies III — Farrington. 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 4 mm. 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 
 1 1 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 much 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. f 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. 
 t Meteoritenkunde, Heft II. p. 63. 
 
168 Field Museum of Natural History — Geology, 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 .06 mm. in diameter. A series of 
 parallel alternate rods of chrysolite and glass averaging .03 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 are as 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 is made 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 Studies III — Farrixgton. 169 
 
 A partial analysis of the meteorite was made by Mr. H. W. Nichols 
 with results as follows: 
 
 SiO, 35 69 
 
 Al, Oi 1 .03 
 
 Cr« Oi 0.12 
 
 Ni O 1 . 04 
 
 Co O 0.08 
 
 Ca O 1 93 
 
 Na, O 0.95 
 
 KiO 0.47 
 
 P 0.40 
 
 S 2. 11 
 
 Fe ." 10.48 
 
 Ni 1 59 
 
 Co 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 90 
 miles east from Tonopah, 18 miles north from the Mt. Diablo base 
 line, and 100 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 Field Museum of Natural History — Geology, Vol. 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 12 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 was shipped 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, furro wings, 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 somewhat irregular. 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 20 inches. 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. Meteorite Studies III — Farringtox. 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 (10 cm.) 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 square inch 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 witn 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 two inches (5 cm.). Frequently 
 the cavity within is larger and of somewhat different shape from the 
 orifice. As a rule, though, it has an approximately cylindrical shape 
 and is about the size of the orifice. Other shapes noted for the orifices 
 
172 Field Museum of Natural History — Geology, Vol. III. 
 
 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 a more 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. on a 
 side are formed as a result. The long ridges are probably formed by 
 tasnite ribbons. Those at right angles are at irregular intervals, and 
 probably mark the crossing of other bands. As a rule the groups of 
 long ridges run in three directions at angles of 6o° 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 
 to them. 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 Studies III — 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 
 articlef 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. 
 t Am. Jour. Sci., 1909, 4, 28, 431-434. 
 
174 Field Museum of Natural History — Geology, 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 i . Etching figures of Quinn Canyon meteorite. X 2. 
 
 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 
 
Juxe, 1910. Meteorite Studies III — Farrington. 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 enlarged in 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 taenite, 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 taenite 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 2^ 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: 
 
 Fe 9 1 . 63 
 
 Ni :.... 7-33 
 
 Co o. 73 
 
 Cu tr. 
 
 S o .00 
 
 P o . 20 
 
 Si 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 Field Museum of Natural History — Geology, Vol. III. 
 
 of the carefully sampled borings weighing 53^ 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 4X grams argols. The lead 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: 
 
 Fe O 20.84 
 
 Fe 2 3 54- 60 
 
 75-44 
 
 Calc. to 
 
 100 
 
 Theory for 
 Magnetite 
 
 27 .62 
 
 31 
 
 72-38 
 
 69 
 
 The remainder which was not determined quantitatively, was chiefly 
 water, lime, C0 2 , 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 T^NITE. 
 
 The composition of taenite, 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 
 
 1 86.44 
 
 2 85 .00 
 
 3 85.00 
 
 Ni 
 
 13 .02 
 
 14 00 
 
 15.00 
 
 Co 
 0.54 
 
 83.28 .... 16 68 
 
 80 . 30 19 . 60 
 
 74.78 24.32 
 
 73.10 23.63 
 
 Cu 
 
 04 
 
 
 
 Fe:Ni+Co 
 
 2 
 
 Total 
 
 +Cu 
 
 
 100 .00 
 
 6.9:1 
 
 
 99 .00 
 
 6.4:1 
 
 
 100 .00 
 
 6.0:1 
 
 
 100 .00 
 
 5.2:1 
 
 
 99.90 
 
 4.1 : j 
 
 5° 
 
 99-93 
 
 3.2 : 1 
 
 17 
 
 100.00 
 
 3.0:1 
 
June, 1910. Meteorite Studies III — Farrington. 
 
 177 
 
 Fe 
 
 8 73-o 
 
 9 72 . 12 
 
 10 7i- 2 9 
 
 11 70. 14 
 
 12 69.30 
 
 13 68.13 
 
 14 65.54 
 
 15 ' 65.39 
 
 16 65 . 26 
 
 17 63.55 
 
 18 63.04 
 
 19 61 .89 
 
 20 61 .87 
 
 21 57- lS 
 
 22 50 .73 
 
 Xi 
 27 .00 
 
 27-73 
 26.73 
 29.74 
 
 20-73 
 3085 
 3287 
 33- 20 
 34-34 
 34-65 
 35-53 
 36.95 
 
 34.00 
 47.80 
 
 Co 
 
 0.02 
 1.68 
 
 .60 
 0.69 
 
 i-59 
 
 1 .41 
 0.40 
 1 .01 
 
 1-43 
 
 0.36 
 
 Cu 
 
 33 
 
 0.12 
 0.30 
 
 o-37 
 
 0.49 
 
 tr. 
 
 0.80 
 
 38.13 .... tr 
 
 0.55 
 
 0.63 0.37 0.47 
 
 Total 
 100 .00 
 100.00 
 100.00 
 
 99.88 
 100.00 
 100 .00 
 100 .00 
 100 .00 
 100 .00 
 100.00 
 100 .00 
 100.00 
 
 100.00 
 91-73 
 
 Fe:Ni + Co 
 4-Cu 
 2.8 
 
 2-7 
 
 2.6 
 
 2-5 
 
 2.4 
 
 REFERENCES. 
 
 1. Cosby Creek, Reichenbach, Jr.: Pogg. Ann., 1861, xciv, 258. Plates 
 
 8 cm. long and 2K cm. broad, mechanically isolated by Reichenbach, 
 Sr. Mean of three analyses. 
 
 2. Charcas. Meunier: Ann. Chim. et Phys., 1869 (4), xvii, 31. Particles 
 
 mechanically isolated by their color. 
 
 3. Caille. Meunier: Ann. Chim. et Phys., 1869 (4), xvii, 32. Net-like web, 
 
 isolated by means of dilute nitric acid. 
 
 4. Casas Grandes. Tassin: Proc. U. S. Nat. Mus., 1902, xxv, 73. 
 
 5. Kenton Co. Nichols: Pub. Field Col. Mus., 1902 Geol. Ser., i, 315. 
 
 Thin, tin- white, elastic, magnetic plates, 4 mm. square, with finely ribbed 
 surface. 
 
 6. Welland. Davison: Am. Jour. Sci., 1891 (3), xlii, 66. Mechanically 
 
 isolated plates ^j-jV mm. thick, silver-white to bronze-yellow, flexible 
 and elastic. 
 
 7. Staunton. Cohen and Weinschenk: Ann. Wien Naturhist Mus., 1891, 
 
 vi, 146. Gray, relatively thick and brittle plates. Isolated by dilute 
 HC1. Calculated to 100 after deducting schreibersite. 
 
 8. Cosby Creek. Smith: Comptes Rendu, 1881, xcii, 843. Little thin 
 
 plates of white metallic color left after dissolving the iron in acid. 
 
 9. Canyon Diablo. Tassin: Smithsonian Misc. Coll., 1907, i, 212. Calcu- 
 
 lated to 100 after deducting 0.26% schreibersite. 
 to. Magura. Weinschenk: Ann. Wien Naturhist. Mus., 1889, iv, 97. Thin, 
 
 tough, silver-white lamellae soluble with difficulty in acids. Isolated 
 
 by dilute HC1. Calculated to 100 after deduction of schreibersite. 
 [i. Cranbourne. Flight: Phil. Trans. London, 1882, No. 171, 888. White, 
 
 flexible, magnetic, triangular or rhombic mechanically isolated plates. 
 [2. Misteca. Cohen: Ann. Wien Naturhist. Mus., 1892, vii, 152. Dull and 
 
 brittle plates. Isolated by HC1. Calculated to 100 after deducting 
 
 schreibersite. 
 
178 Field Museum of Natural History — Geology, Vol. 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 HC1. Calculated to 100 after deduction of 
 schreibersite. 
 
 15. Chupaderos. Manteuff el : Ann. Wien Naturhist. Mus., 1892, vii, 150. 
 
 Brittle, tin-white plates. Isolated by HC1. Calculated to 100 after 
 deducting schreibersite. 
 
 16. Toluca. Cohen and Weinschenk: Ann. Wien Naturhist. Mus., 1891, vi, 
 
 137. Tin-white, flexible plates. Isolated by HC1. Calculated to 100 
 after deducting schreibersite. 
 
 17. Canyon Diablo. Fahrenhorst: Ann. Wien Naturhist. Mus., 1900, xv, 
 
 376. Thin, flexible plates partly appearing made up of many lamellae, 
 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 HC1 
 Calculated to 100 after deducting schreibersite. 
 
 19. Bischtube. Cohen: Ann. Wien Naturhist. Mus., 1897, x "> 54- Large, 
 
 flexible plates with included schreibersite. Isolated by HC1. 
 
 20. Penkarring Rock. Fletcher: Min. Mag., 1899, xii, 174. Thin, flexible 
 
 plates. Analysis calculated to 100 after deducting 4.18% schreibersite. 
 
 21. Medwedewa. Berzelius: Pogg. Ann., 1833, xxxiii, 133. Analysis of 
 
 skeleton material left behind after dissolving in HC1. 
 
 22. Beaconsfield. Sjostrdm: 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 7 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 tasnite. 
 
 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. The yearly 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 well- 
 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., 1910 (4), 29, 211— 215. 
 
June, 1910. Meteorite Studies III — Farrington. 179 
 
 ment of meteorites. Since new falls occur yearly, data for study of 
 these points are obviously constantly on the increase. It is desirable, 
 however, to make comparisons at intervals in order that any changes 
 may be discerned. At the present time the admirable catalogues of 
 Wiilfing * 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, 18 16, 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 
 11 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: 
 
 1 800 o 1 806 1 1812 4 1818 3 
 
 1 80 1 o 1807 2 1813 2 18 19 2 
 
 1802 1 1808 3 1814 2 1820 1 
 
 1803 3 1809 o 1815 2 1821 1 
 
 1804 2 1810 2 1816 o 1822.. .. 5 
 
 1805 2 1811 2 1817 o 1823 2 
 
 * Die Meteoriten in Sammlungen, Tubingen, 1897. 
 
180 Field Museum of Natural History — Geology, Vol. III. 
 
 1824 .... . 3 1846 4 1868 11 1890 6 
 
 1825 2 1847 2 1869 6 1891 2 
 
 1826 2 1848 3 1870 3 1892 3 
 
 1827 3 1849 1 1871 3 1893 4 
 
 1828 1 1850 2 1872 4 1894 3 
 
 1829 3 1851 2 1873 3 1895 3 
 
 1830 2 1852 4 1874 5 1896 4 
 
 1831 2 1853 3 1875 5 1897 6 
 
 1832 o 1854 1 1876 5 1898 3 
 
 1833 1 1855 4 1877 7 1899 5 
 
 1834 2 1856 3 1878 5 1900 3 
 
 1835 3 1857 6 1879 6 1901 3 
 
 1836 3 1858 4 1880 3 1902 5 
 
 1837 1 1859...... 5 1881 2 1903 3 
 
 1838 5 i860 5 1882 4 1904 1 
 
 1839 1861 3 1883 3 1905 3 
 
 1840 3 1862 2 1884 3 1906 o 
 
 1841 3 1863 6 1885 4 1907 1 
 
 1842 3 1864 3 1886 7 1908 o 
 
 1843 5 1865 7 1887 6 1909 o 
 
 1844 3 1866 6 1888 o 
 
 1845 3 1867 2 1889 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 900 
 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 i860 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 Studies III — Farrington. 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 falls in 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 21=350 
 
 This record is shown graphically in the accompanying diagram, Fig. 2. 
 
 Curve of meteorite falls by months. 
 
182 Field Museum of Natural History — Geology, Vol. 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. 
 1 1 . . 1 3 • • 2 
 
 Popular Astronomy, 1909, 17, 277. 
 
June, 1910. Meteorite Studies III — Farrington. 183 
 
 Jan. Feb. Mar. Apr. Mayjunejuly Aug. Sept. Oct. Nov. Dec. 
 
 17 1 1 3 1 2 1 
 
 18 3 1 .. 2 1 1 .. 1 
 
 19 2 1 2 1 3 1 1 2 1 
 
 20 1 1 1 3 2 1 i 
 
 21 1 1 2 .. .. 1 2 .. 1 
 
 22 1 . . 3 1 1 1 3 1 . . 
 
 23 3 l ■ • x • • 1 ■ • l 
 
 24 1 1 2 2 .. .. 1 1 
 
 25 2 1 3 1 1 1 2 .. .. 1 
 
 26 3 2 1 .. .. 1 1 1 
 
 27 1 1 1 2 1 .. 1 .. 3 
 
 28 1 1 2 .. 1 3 .. .. 1 
 
 29 1 1 .. 1 1 .. 3 1 
 
 3° 1 1 » • • I ■ • 4 
 
 31 2 . . 1 1 . . 1 
 
 23 23 21 29 41 42 21 32 28 24 23 20=327 
 
 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 : 
 
 Hours 12 1 2 3 4 5 6 7 8 91011 Total 
 
 a. m 1 2 3 2 6 7 7 18 12 10 9 12 = 89 
 
 P- m 24 13 19 33 21 15 11 8 16 7 9 3 = 176 
 
 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 2 1 , while from 6 a. m. to noon it is 68 ; 
 
184 Field Museum of Natural History — Geology, Vol. 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 J 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 90 , at 3 p. 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. 
 % 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. 
 IT Popular Astronomy, 1910, 18, 276. 
 ** Op. cit., p. 272. 
 
June, 1910. Meteorite Studies III — Farrington. 185 
 
 and at 3 p. m. It may 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, who in 1867 f gave the hours of 178 meteorite 
 falls. His table was as follows: 
 
 12 1 2 3 4 5 6 7 8 9 10 11 
 
 am 1 3 2 2 4 5 4 13 5 7 5 2 3 = 74 
 
 P. M 9 11 11 19 18 9 6 10 5 1 o 5 = 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: 
 
 12 1 23456789 10 11 
 
 am 1 1 1 2 3 3 4 10 5 5 5 17 = 57 
 
 p m 7 9 9 16 15 7 5 7 3 o o 3 = 81 
 
 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., 
 11 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. 
 
 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. 
 tSitzb. Kais. Akad. der Wiss. Wien. Bd. 55. 
 
186 Field Museum of Natural History — Geology, Vol. 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. 
 
 Cca. Stone, Veined spherulitic chondrite. 
 
 Ccb. 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. 
 
 Cs. 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 
 
 D. Iron, Ataxite. 
 
 Db. Iron, Babb's Mill ataxite. 
 
 Dc. Iron, Cape ataxite. 
 
 Dl. Iron, Linville ataxite. 
 
 Dn. Iron, Nedagolla ataxite. 
 
 Dr. Iron, Rafruti ataxite. 
 
 Ds. Iron, Siratik ataxite. 
 
 Dsh. Iron, Shingle Springs ataxite. 
 
 Dt. Iron, Tucson ataxite. 
 
 H. Iron, Hexahedrite. 
 
 Ha. Iron, Granular hexahedrite. 
 
 Hb. Iron, Breccia-like hexahedrite. 
 
 Ho. Stone, Howardite. 
 
 Kc. Stone, Carbonaceous, spherulitic chondrite. 
 
 M. Iron-stone, Mesosiderite. 
 
 Mg. Iron-stone, Grahamite. 
 
 O. Iron, Octahedrite. 
 
 Of. Iron, Fine octahedrite. 
 
June, 1910. Meteorite Studies III — Farrington. 187 
 
 Off. Iron, Finest octahedrite . 
 
 Offbp. Iron, Breccia-like finest octahedrite. 
 
 Og. Iron, Coarse octahedrite. 
 
 Ogg. Iron, Coarsest octahedrite. 
 
 Oh. Iron, Hammond octahedrite. 
 
 Om. Iron, Medium octahedrite. 
 
 P. Iron-stone, Pallasite. 
 
 Pi. Iron-stone, Imilac pallasite. 
 
 Pk. Iron-stone, Krasnoyarsk pallasite. 
 
 Pr. Iron-stone, Rokicky pallasite. 
 
 LIST OP 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° jo' 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, 11. 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, o; irons 2; total, 2. Observed falls, 1. 
 
 ARIZONA. 
 
 Canyon Diablo, Coconino Co., Og. 35° 10' N. iii° 7' W., found 1891. 
 Coon Butte, Coconino Co., Cib. 35° 10' N. 111° 7' W., found 1906. 
 Tucson, Pima Co., Dt. 32° 12' N. no 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 Range, 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 Field Museum of Natural History — Geology, Vol. 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, o; 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, o; total. 1. Observed falls, 1. 
 
 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 o' N. 113 45' W., found 1895. 
 Stones, o; irons, 1; total, 1. Observed falls, o. 
 
 INDIANA. 
 
 Harrison County, Cho. 38 12' N. 86° 8' W., fell March 28, 1859. 
 Kokomo, Howard Co., Dc. 4 o° 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 i860. 
 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.yi° 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. 
 
 Admire, Lyon Co., Pr. 33 o' N. 96 5' W., found 1891. 
 Brenham, Kiowa Co., Pk. 37 38' N. 99 13' W., found 1885. 
 Elm Creek, Lyon Co., Ceo. 38 40' N. 96 5' W., found 1906. 
 
June, 1910. Meteorite Studies III — Farrington. 189 
 
 Farmington, Washington Co., Csa. 39°48' N. 97 5' W., fell June 25, 1890. 
 Jerome, Gove Co., Cck. 38 47' N. ioo° 14' W., fell Apr. 10, 1894. 
 Long Island, Phillips Co., Ck. 39 56' X. 99 34' W., found 1891. 
 Modoc, Scott Co., Cga. 38 30' N. ioo° 55' W., fell Sept 2, 1905. 
 Xess 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' X. 95 18' W., fell Apr. 9, 1896. 
 Prairie Dog Creek, Decatur Co., Cck. 39 42' N. ioo° 24' W., found 1893. 
 Saline, Sheridan Co., Cck. 39 22' N. ioo° 27' W., fell Nov. 15, 1898. 
 Scott, Scott Co., 38 30' X. ioo° 55' W., found 1905. 
 Tonganoxie, Leavenworth Co., Om. 39 8' X. 95 7' W., found 1886. 
 Waconda, Mitchell Co., Ccb. 39 20' X. 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' X. 83 37' W., fell Xov. 15, 1902. 
 
 Casey County, Og. 37 20' X. 84 55' W., found 1877. 
 
 Cynthiana, Harrison Co., Cg. 38 24' X. 84 16' W., fell Jan. 23, 1877. 
 
 Eagle Station, Carroll Co., Pr. 38 37' X. 85 o' W., found 1880. 
 
 Frankfort, Franklin Co., Om. 38 7' X. 84 57' W., found 1866. 
 
 Kenton County, Om. 38 40' X. 84 29' W., found 1889. 
 
 La Grange, Oldham Co., Of. 38 37' X. 85° 25' W., found i860. 
 
 Marshall County, Om. 36 50' X. 88° 17' W., found i860. 
 
 Mount Vernon, Christian Co., Pk. 36 50' X. 87 28' W., found 1868. 
 
 Xelson County, Ogg. 37 48' X. 85 27' W., found i860. 
 
 Salt River, Bullitt Co., Off. 37 56' X. 85 54' W., found 1850. 
 
 Scottsville, Allen Co., H. 36 45' X. 86° 10' W., found 1867. 
 
 Smithland, Livingston Co., Db. 37 18' X. 88° 17' W., found 1839. 
 
 Williamstown, Grant Co., Om. 38 35' X. 84 30' W., found 1892. 
 
 Stones, 2; iron-stones, 2; irons, 10; total, 14. Observed falls, 2. 
 
 MAINE. 
 
 Andover, Oxford Co., Cc. 44 36' X. 70 47' W., fell Aug. 5, 1898. 
 Castine, Hancock Co., Cwa. 44 24' N. 68° 48' W., fell May 20, 1848. 
 Xobleborough, Lincoln Co., Ho. 44 4' X. 69 28' W., fell Aug. 7, 1823. 
 Searsmont, Waldo Co., Cc. 44 22' X. 69 12' W.. fell May 21, 1871. 
 Stones, 4; irons, o; total, 4. Observed falls, 4. 
 
 MARYLAND. 
 
 Emmitsburg, Frederick Co., Om. 39° 43' X. 77 20' \V"., found 1854. 
 Lonaconing, Allegheny Co., Og. 39 28' X. 79 2' W., found 1888. 
 Nanjemoy, Charles Co., Cc. 38 25' X. 77 12' W., fell Feb. 10, 1825. 
 Stones, 1; irons, 2; total, 3. Observed falls, 1. 
 
 MICHIGAN. 
 
 Allegan, Allegan Co., Ceo. 42 34' X. 85 52' W., fell July 10, 1899. 
 Grand Rapids, Kent Co., Of. 42 59' X. 85 42' W., found 1883. 
 Reed City, Osceola Co., Oh. 43 53' X. 85 32' W., found 1895. 
 Stones, 1; irons, 2; total, 3. Observed falls. 1. 
 
190 Field Museum of Natural History — Geology, Vol. 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°i3'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. 90 36' W., found 1863. 
 Saint Genevieve County, Of. 37 47' N. 90 22' W., found 1888. 
 Warrenton, Warren Co., Ceo. 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, o; 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, o; irons, 5; total, 5. Observed falls, o. 
 
 NEVADA. 
 
 Quinn Canyon, Nye Co., Om. 38 30' N. 115 20' W., found 1908. 
 Stones, o; 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, o; 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 o' -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, o; irons, 6; total 6. 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. Meteorite Studies III — Farrington. 191 
 
 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, 1. 
 
 NORTH CAROLINA. 
 
 Asheville, Buncombe Co., Om. 35 36' N. 82 31' W., desc. 1839. 
 
 Black Mountain, Buncombe Co., Og. 35 53' N. 8o° 3' W., found 1839. 
 
 Bridgewater, Burke Co., Of. 35 45' N- 8i° 53' W., found 1890. 
 
 Castalia, Nash Co., Cgb. 36 4' X. 78 4' W., fell May 14, 1874. 
 
 Colfax, Rutherford Co., Om. 35 18' N. 8i° 45' W., found 1880. 
 
 Cross Roads, Wilson Co., Cg. 35 38' X. 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' X. 82 44' W., found 1873. 
 
 Ferguson, Haywood Co., Stone, 35 36' X. 83 o' W., fell July 18, 1889. 
 
 Flows, Cabarrus Co., Cga. 35 18' N. 8o° 33' W., fell Oct. 31, 1849. 
 
 Forsyth County, Dn. 36 8' X. 8o° 20' W., found 1895. 
 
 Guilford County, Om. 36 4' N. 79 48' W., desc. 1822. 
 
 Hendersonville, Henderson Co., Cc. 35 19' X. 82 28' W., found 1901. 
 
 Jewel Hill, Madison Co., Of. 35 49' N, 82 45' W., found 1854. 
 
 Lick Creek, Davidson Co., H. 35 40' N. 8o° 12' W., found 1879. 
 
 Linville, Burke Co., Dl. 35 48' N. 8i° 55' W., found 1882. 
 
 Murphy, Cherokee Co., H. 35 6' N. 84 2' W., found 1899. 
 
 Persimmon Creek, Cherokee Co., Offbp. 35° 3' X. 84 4' W., found 1893. 
 
 Smith's Mountain, Rockingham Cd., Of. 36° 32' X. 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. 
 Xiagara, Grand Forks Co., Og. 47 58' X. 97 52' W., found 1879. 
 Stones, o; irons, 2; total, 2. Observed falls, o. 
 
 OHIO. 
 
 Anderson Township, Hamilton Co., P. 39 10' X. 84 18' W., desc. 1884. 
 Cincinnati, Hamilton Co., Ds. 39 7' X. 84 29' W., desc 1898. 
 Hopewell Mounds, Ross Co., Om. 39 10' X. 83 20' W., desc. 1902. 
 New Concord, Guernsey Co., Cia. 39 58' X. 8i° 44' W., fell May 1, i860. 
 Pricetown, Highland Co., Cw. 33° 11' N. 83 44' W., fell Feb. 13, 1893. 
 Wooster, Wayne Co.. Om. 40 48' N. 8i° 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' X. 122 35' W., found 1902. 
 Stones, o; 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 Field Museum of Natural History — Geology, Vol. 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, o; irons, 4; total, 4. Observed falls, o. 
 
 SOUTH CAROLINA. 
 
 Bishopville, Sumter Co., Chla. 34 12' N. 8o° 18' W., fell Mar. 25, 1843. 
 
 Chesterville, Chester Co., Dn. 34 42' N. 8i° 15' W., found 1847. 
 
 Laurens County, Off. 34 30' N. 82 14' W., found 1857. 
 
 Lexington County, Og. 33 57' N. 8i° 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. ioo° 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 i860. 
 Coopertown, Robertson Co., Om. 36 25' N. 87 o' W., found i860. 
 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. 
 Smith ville, 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. 
 
 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. S3° 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. ioo° 20' W., found 1897. 
 
Meteorite Studies III — 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 o' N. 98 40' W., found 1836. 
 Stones, 6; irons, 9; total, 15. Observed falls, o. 
 
 Salt Lake City, Salt Lake Co., Cgb. 40 58' N. m° 25' W., found 1869. 
 Stones 1; irons, o; 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. 8o° 47' W., found 1852. 
 Hopper, Henry Co., Om. 36 35' N. 79 45' W., found 1889. 
 Indian Valley, Floyd Co., Ha. 36 58' N. 8o° 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, 1. 
 
 WEST VIRGINIA. 
 
 Greenbrier County, Og. 37 32' N. 8o° 18' W., found 1880. 
 Jennie's Creek, Wayne Co., Og. 37 53' N. 82 22' W., found 1883. 
 Stones, o; 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, 1. 
 
 WYOMING. 
 
 Silver Crown, Laramie Co., Og. 41 10' N. 105 20' W., found 1887. 
 Stones, o; irons, 1; total, 1. Observed falls, o. 
 
LIBRARY 
 UNIVERSITY Of ILLINOIS 
 
 URBANA 
 
LIBRARY 
 
 UNIVERSITY OF ILLINUIS 
 
 URBANA 
 
FIELD MUSEUM OF NATURAL HISTORY. 
 
 GEOLOGY, VOL. Ill, PLATE LVII. 
 
 Side View of Quinn Canyon Meteorite, x \ c .. 
 
LIBRARY 
 
 UNIVERSITY OF ILLINOIS 
 
 URBANA 
 
LIBRARY 
 
 UNIVERSIIY Oh ILLINUIS 
 
 URBAWA 
 
MUSEUM OF NATURAL HISTORY 
 
 GEOLOGY, VOL. Ill, PLATE UX. 
 
 12 I 2 3 4- 5 6 7 8 9 10 11 12 1 2 3 4 5 6 7 8 9 10 11 12 
 A. M. P. M. 
 
 Curve of Meteorite Falls by Hours. 
 
, 
 
 a 
 
 B