Fusion-Striicturex in Meteorites. 303 



Smith ; Cranbourne, Australia. 1861, by Bertlielot; Goalpara, 

 India, about 1857, examined by Tschermak, who found in it 

 0.85 pr. ct. of a hydro-carbon (0.72 carbon and 0.13 hydrogen); 

 Hessle, near Upsala, January 1, 1869, examined by ISTorden- 

 skjold ; this specimen, di'ied at 110° C, showed 51.6 pr. ct. 

 cai'bon. 



Without entering into details about any of these, I would like 

 to refer once more to the Orgueil meteorite, the analysis of wliicli 

 has previously been given in full. 



Cloez determined in it 6.027 pr. ct. of "humus," and this 

 carbonaceous matter, after drying at 110" C, was found to con- 

 sist- of :* 



Carbou, - - - - 63.45 

 Hydrogen, - . . 5.93 



Oxygen, - - - - 30.57 



100.00 



rather closely resembling the average composition of peat, 

 which may be given as — 



Carbon, - - - - 60.06 



Hydrogen, . . . 6.21 



Oxygen, - - - - 33.78 



100.00 



The presence of carbon in meteorites being thus a well- 

 established fact, the question as to its source naturally next 

 presents itself. 



According to able researches, the carbon in meteorites occurs 

 in two forms, — as graphite, and as small particles, imjDalj^able in 

 nature, scattered through the mineral portion of the mass. 



On the earth, this element occurs in three modifications, as 

 diamond, as graphite, and as coal. Whatever may be the origin 

 claimed for the diamond, as far as graphite and coal are con- 

 cerned, I am aware of no instance where the parentage of either 

 of these cannot be traced to the action of organic life. 



* Phipson : Meteors, AerolUes and Falling Stars, 1867. 



