392 J. L. Smith—Mass of Meteorie Iron. 
owing to its unusual weight, he preserved it. The earth pene- 
trated consisted of stiff clay beneath four inches of black soil, 
so that the mass was imbedded in the clay. This clay was 
colored by oxide of iron, arising from a slight decomposition of 
the surface of the meteorite, the iron being one of those that 
decomposes but slightly from atmospheric agencies. This me- 
teorite was lost sight of for a number of years, having fallen 
into the hands of those not interested in matters of natu 
history, and only recently was sent to me for examinati 
The form of the meteorite is an irregular elongated oval, and 
it has the indentations of the surface found on most meteoric 
irons. Its weight is four kilograms. The alteration at surface 
is very slight, considering the length of time it must have re- 
mained beneath the surface of the svil, and fresh cut surfaces 
retain perfectly their brightness. The specific gravity is 7°821. 
The composition of the meteorite is as follow 
WOR 20 foe ee eee 87 02 
TORR oo ia ee 12°29 
WOUGIb ceo hae ee e e 6 
Phosphorus ---- .--- "02 
vn gitaeg Sagi = PEt SC etWas BTV stoner sapere pana rea Fal a trace. 
op 
A polished surface, when treated with nitric acid or bromine 
water, does not give the slightest indication of Widmanstattian 
figures, so characteristic of most meteoric irons. It hence be- 
longs to that class of irons which are rich in nickel and yet 
give no signs of such figures, to which belong the Cape of Good 
Hope iron of 1798, containing 15 per cent of nickel and 2° per 
cent of cobalt, and also a more recent California i iron, called the 
hingle Springs iron, containing 17 per cent of nickel and ‘6 of 
cobalt. Of the same kind is the Octibbeha meteorite, containing 
the very large amount of 59-7 per cent of nickel. Besides the 
above, there are certain irons containing much less nickel that 
are also without these figures, as the Nelson County, Braunau, ete. 
he phenomena “ct the so-called Widmanstittian figures in 
connection with meteoric irons is one of considerable interest, 
and as yet ene» a satisfactory sectatation At one time it 
was supposed to e from the accumulation in the lines of the 
oe of an alloy y the in nickel than the mass of the iron. 
hs Pyne it has been supposed to arise from the accumula- 
osphide of nickel and iron (schreibersite), along 
bem Bnes ‘of F onsetalling tion in the mass. But neither of 
these hypotheses serve to explain the varied features of these 
pee or the total absence of them, as in the present instance. 
y own conviction is, that we shall not arrive at a satisfactory 
explanation until our knowledge of the effect of a minute 
quantity of substances in the iron is better understood 
than now; a eth bel srhich Pasi pure and technical chemistry 
are now studying interest, in order to discover sisi 
eae en Ne ee ae 
