J. L. Smith — Carbon Compounds in Meteorites. 391 



are but four of them yet known, viz: that which fell at Alais 

 in 1806, that at Kold-Bokeveldt in 1888, that at Kaba in 1857, 

 and that at Orgueil in 1864. They contain, respectively, about 

 3, 2, 0"6, and 6 per cent of carbonaceous matter. 



I would here remark that the Alais, Kold-Bokeveldt, and 

 Orgueil are more closely allied to each other than to the Kaba 

 The predominating mineral constituents are about 



OrgTieil, 



Sihca ;n'22 30-80 



Magnesia 22-21 22-20 



Iron protoxide. -29 -03 29-94 



If we now contrast these mineral constituents with those pre- 

 dominating in well-known meteoric stones, a most striking fact 

 presents itself — one not commonly realized by those engaged in 

 the study of these bodies. It is seen on comparing the above 

 with the following tables : 



Silica 35-30 38-13 47-30 4730 50-08 40-61 



Magnesia 31-76 17-67 24-53 24-53 20-14 36-34 



Iron protoxide 26-70 29-44 28-03 28-03 19-85 19-21 



From these tabular statements, it will be seen that, deducting 

 the small amount of carbon contained in the black meteorites, 

 the mass of mineral matter constituting them is about the same, 

 and corresponds thus with the so-called common type of me- 

 teoric stones ; and hence the mineral matter to which these con- 

 stituents belong must be the same in the two classes of meteor- 

 ites, viz : olivines and pyroxenes, differing only in the more or 

 npact form of these mi r 



writings of g 

 3 find little si 



e stress laid on these facta Thus, M. Meunier, 

 L paper on the origin of meteorites, published in the Cosmos 

 of December, 1869. expresses his amazement that I should speak 

 of the circumscribed uniformity of the composition of meteor- 

 ites as evidence of a circumscribed cosmical origin of these 

 bodies, both with reference to the sphere or spheres whence 

 they come, as well as their rock structure. He takes so opposite 

 a view as to say (p. 9), " So far from the meteorites showing 

 such a resemblance, we can establish between meteoric iron, 

 olivine meteorites, aluminous meteorites, and carbonaceous me- 

 teorites, dift'erences as great as between the most different 

 terrestrial rocks." An assertion which would include all the 

 ranges of rocks and sedimentary deposits from the basalt and 



granite to the cretaceous and tertiary deposits. 



Let any one look at the above table, and say whether < 



