396 MEMOIRS NATIONAL ACADEMY OF SCIENCES, VOL. XIII. 



A further account of the meteorite was given by Farrington, 4 as follows: 



Some further observations may here be added to the brief account of this meteorite given by the writer in 1902. 

 The approximate place of find of the meteorite was kindly indicated to the writer by Mr. S. A. Sutton, and shown in 

 a plate. No other observations of the fall than those already made by Mr. Sutton and reported by the writer seem 

 to be known. The shape of the meteorite may be described as approximately that of a truncated, four-sided pyra- 

 mid. The base of the pyramid was plainly the rear side of the meteorite in falling. It is the broadest surface of the 

 mass, and has an area of about 144 square inches (900 sq. cm.). In outline it is roughly circular. Mr. Sutton states 

 that this was the surface on which the meteorite rested when found, but this position could have been brought about 

 by an overturn when striking. It was more heavily coated with carbonate of lime when received at the museum than 

 any of the other surfaces. It is nearly flat, though slightly concave, and shows the broad, shallow pits characteristic 

 of these surfaces of meteorites. On the opposite side of the meteorite a surface having the form of a long and narrow 

 isosceles triangle runs nearly parallel to it and the thickness of the meteorite between the two surfaces ranges from 7 to 

 8 inches (18 to 20 cm.). From the parallel surface the meteorite slopes away at angles of 40, 50, 60, and 90, 

 approximately. Three of these surfaces are approximately plane, the others are rounded. The plane surfaces show 

 practically no pits, the others are more or less irregularly pitted. The more symmetrical of these pits are oval in form, 

 from 0.5 to 0.75 inches in their longest diameter; and have a depth about one-fourth as great. All the edges produced 

 by the meeting of different surfaces of the meteorite are rounded. 



Except where it has scaled off in small areas the meteorite is covered with a firmly adherent, dull brown-black 

 crust, rough from the protrusion of thickly scattered metallic grains. These grains are darker in color than the rest of 

 the crust, probably from a coating of iron oxide. When this coating is scraped away, however, the bright nickel- 

 white color of the metallic grains is seen. One of the grains showed bright when the meteorite was received, but it 

 may perhaps have become so through handling. It is the largest single grain to be seen. It has a hemispherical form 

 and a diameter of 5 mm. The shapes of the other metallic grains as they protrude are various. Some are elongated, 

 some nearly circular, and others form small connecting groups. For the most part the grains are independent of each 

 other, but there are two well-defined groups of them extending in irregular lines and standing out like veins. These 

 are not straight in their course but nearly so. The extent of each is about 6 cm. (2.5 inches). One runs from the 

 large grain mentioned above, the other is nearly parallel to it 7 inches (18 cm.) distant. 



Besides being broken by the protrusion of the metallic grains, the crust is seamed and fissured by numerous cracks 

 extending in all directions and varying in extent and depth. The largest has a length of 6 inches (15 cm.), and from 

 this to the minutest fissures all gradations occur. The course of most of the cracks is straight toward the interior of the 

 meteorite, but some run so as to tend to scale off. They give the exterior of the meteorite a "baked " look, and there 

 can be little doubt that they are the result of differential expansion through heat of the interior as compared with the 

 exterior. Scaling of the crust had occurred at various points when the mass reached the museum. Many of these 

 scalings must, on account of their freshness, have occurred very shortly before the meteorite struck the earth or from 

 the force of impact. Most of the surfaces thus exposed were covered with an adherent coating of carbonate of lime 

 when the stone was received at the museum. The lime undoubtedly deposited more readily here on account of the 

 increased capillary attraction afforded by such surfaces. The color of these surfaces was for the most part rusty 

 brown from exposure, but a few were of a greenish-gray color where the carbonate of lime was freshly removed. In 

 addition to these wholly uncrusted surfaces one about 3 inches square had a very thin black crust, much thinner than 

 the average crust. It is evident that at this point a piece scaled off from the meteorite during its passage through the 

 air and time sufficed for only a partial fusing of the freshly exposed surface. 



Internally the substance of the meteorite when freshly broken is of a greenish-gray color and firmly coherent tex- 

 ture so that it takes a good polish. Enough weathering has taken place, however, to give the interior in large part a 

 dark-brown color. The percentage of metallic grains seen on a polished surface is large, so as to seemingly constitute 

 about one-fourth the mass. The metal is uniformly distributed but the grains vary in size and shape. Some having 

 a diameter of 4-5 mm. are discernible. At times they aggregate into veinlike lines. Under the microscope all the 

 striking characters of the spherical chondrites are presented by the meteorite. Chondri of great variety of size and 

 structure make up the principal mass. For the most part the chondri are spherical in form but some are oval and 

 others of unsymmetrical outline. Besides complete chondri, fragments of chondri are to be seen. As was stated 

 in the writer's first paper on the meteorite, enstatite and olivine either singly or in combination chiefly compose 

 the chondri. Diameters of from 0.3 to 0.6 mm. are presented as a rule by the enstatite chondri, but one 3 mm. in 

 diameter was seen in one section. Several of the half-glassy chondri show rounded depressions as if made by the 

 pressure of another chondrus. The olivine chondri are both monosomatic and polysomatic, also porphyritic and 

 lamellar. In dimension they vary as widely as do the enstatite chondri and between about the same limits. The 

 porphyritic individuals of the chondri show, as a rule, well-marked prismatic outlines. Crust sections under the 

 microscope fail to show, except for an outer fusion zone, well-marked zones such as are common in the more porous 

 chondrites. The fusion zone is of a dark, nearly opaque, somewhat blebby and glassy nature, and has a thickness of 

 about 0.08 mm. Succeeding this, toward the interior of the meteorite, a zone about 0.4 mm. in thickness shows 

 scattered opaque impregnations interspersed among unaltered olivine crystals. This zone is not uniform in occurrence, 

 however, and can be seen only at intervals. 



The meteorite is chiefly in the possession of the Field Museum. 



