May, 1902. METEORITE StupDIES, I—FARRINGTON. 289 
The natural surface of the more conical part (Brus/seite) of the 
meteorite as it is at present joined together, is for the most part deeply 
pitted with characteristic meteoritic thumb-marks (piezoglypten). 
These pits vary considerably, as would be expected, in form and size, 
but still exhibit a certain uniformity. The majority have the form of 
an elongated ellipse whose major axis is about twice the length of its 
minor. The following dimensions may be considered as representing 
a fair average of the size of the pits: Major axis, 3.2 cm. (1 in.) 
Minor axis, 1.5 cm. (5gin.) Depth, 3 to 1omm. (% to 3gin.) The 
depression of each pit generally slopes uniformly toward the center of 
the ellipse, but often there are to be found pits, the deepest point of 
which is quite eccentrically placed and which have a more or less con- 
ical shape. Some pits have a nearly circular outline as contrasted 
with the more common ellipsoidal one. These circular pits are 
usually of small size, but one of large size and unusual depth is to be 
found at the point in the meteorite where the two planes A and C cut 
eachother. This pit has for the most part the shape of a deep regular 
bowl, although the regularity of one portion is broken by two smaller 
conical pits. The depth of this pit is 3.2 cm. (1%in.) and its diameter 
6.4.cm. (2% in.) The point of junction of the planes is almost exactly 
at the center of the pit. It is evident that this was a point of weak- 
ness in the stone at which the erosive action of heat and friction pro- 
duced during the passage of the mass through the atrnosphere worked 
more rapidly than on other parts of thesurface. Its occurrence at the 
point of junction of the planes is pretty good evidence that the latter 
existed in the stone previous to its entry into the atmosphere. This 
fact has also a bearing on the disputed question as to the origin of the 
pits in general. It shows that they owe their origin chiefly to an 
excavation by heat and pressure of the softer or more friable parts 
of the surface of the mass which is acted upon. Wherever there is 
a point of weakness there a pit will be formed. Vice versa, where 
a pit is formed, there was a point of weakness. 
The rear side (Rickseite) of the stone is not pitted. It has a 
well developed crust, but the encrusted surface exhibits no marked 
depressions or elevations. The only portion of the meteorite as now 
restored which illustrates the Rickseite is that appearing in the upper 
right hand part of Plate XLIII (Frontispiece). Here the surface is 
slightly undulating, but there are no pits. 
The color of the crust of the meteorite is in general dark brown, 
but varies from almost black to light brown. At a little distance it 
appears perfectly smooth and in places shining, but on close examin- 
ation it is seen to be quite uniformly and coarsely stippled by the pro- 
