Oxidized H, L, and LL chondrites

Details Oxidized H, L, and LL chondrites Oxidized H, L, and LL chondrites

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994metic..29r.486k&link_type=abstract

Meteoritics (ISSN 0026-1114), vol. 29, no. 4, p. 486-487

Computer Science

Chondrites, Kamacite, Meteoritic Composition, Solar Corona, Troilite, Carburizing, Electron Probes, Magnetite, Oxidation, Scanning Electron Microscopy

Scientific paper

The association consisting predominantly of massive magnetite, carbides, kamacite, troilite and accessory taenite, and pentlandite was previously described in LL3.0 Semarkona, LL3.7 ALHA 77278, LL3.2/3.7 Ngawi, and in the Study Butte H regolith breccia. Taylor et al. suggested that this mineral assemblage formed in the solar nebula by condensation of Cr, Si, and P-rich metal; reaction of metal with S at 700 K resulting in the formation of troilite; carbonization of metal-troilite assemblages at less than 450 K; accretion of fine-grained silicate matrix material; oxidation of metal-troilite-carbide assemblages at about 400 K and formation of magnetite; and additional accretion of magnetite. Hutchison et al. concluded that the carbide-magnetite-metal assemblage in Semarkona formed in the solar nebula and then underwent accretion followed/accompanied by mild brecciation, a second period of magnetite crystallization, crystallization of carbide veins, and hydrous alteration and resorption of some magnetite. We studied 122 type 3 ordinary chondrites (OC) using optical microscopy, scanning electron microscopy, and electron-probe microanalysis and found that 19 of them contain abundant Fe, Ni carbides associated with metallic Fe-Ni, troilite, and, in many cases, massive magnetite. The presence of massive magnetite, Ni-rich metal, and Co-rich kamacite in 14% of H, 16% of L, and 17% of LL type 3 chondrites suggests that these meteorites experienced significant oxidation. The carbides have variable compositions within individual chondrites and were possibly formed by carburization of metallic Fe-Ni by Co-rich vapor. Carburization and oxidation of metallic Fe, Ni could take place at low temperatures in the solar nebula or on a parent body during its degassing.

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