Volatile Element Chemistry during Metamorphism of Ordinary Chondritic Material and Some of its Implications for the Composition of Asteroids

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dc.creatorSchaefer, Laura
dc.creatorFegley Jr, Bruce
dc.date2008-01-07
dc.date.accessioned2026-07-07T08:53:04Z
dc.date.available2026-07-07T08:53:04Z
dc.descriptionWe used chemical equilibrium calculations to model thermal metamorphism of ordinary chondritic material as a function of temperature, pressure, and trace element abundance and use our results to discuss volatile mobilization during thermal metamorphism of ordinary chondrite parent bodies. The calculations include ~1,700 solids and gases of 40 elements. We compiled trace element abundances in H-, L-, and LL-chondrites for the elements Ag, As, Au, Bi, Cd, Cs, Cu, Ga, Ge, In, Pb, Rb, Sb, Se, Sn, Te, Tl, and Zn, and identified abundance trends as a function of petrographic type within each class. We found that abundance patterns within the H- and L- chondrites are consistent with mobilization of volatile elements in an onionshell-type parent body. LL-chondrites have more complex abundance patterns that may support a rubble-pile model for the LL-chondrite parent body. We calculated volatility sequences for the trace elements in the ordinary chondritic material, which differs significantly from the solar nebula volatility sequence.
dc.description64 pages, 14 figures, 5 tables; submitted to Icarus
dc.identifierhttps://arxiv.org/abs/0801.1099
dc.identifierhttp://arxiv.org/abs/0801.1099
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/145494
dc.subjectAstrophysics
dc.titleVolatile Element Chemistry during Metamorphism of Ordinary Chondritic Material and Some of its Implications for the Composition of Asteroids
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