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On high-temperature formation of iron-rich olivine in the early solar systemA kinetic restriction on the formation of fayalite-rich olivine in equilibrium with the cooling solar-composition gas appears to exist at the low temperature of approximately 500 K. We offer a high-temperature formation mechanism (different from simple condensation) which operates at high hydrogen depletion (up to 300 times) relative to solar abundance. We show how the necessary depletion rate decreases with temperature (thermodynamical equilibrium is suggested). The consequences for planet formation are considered.
Document ID
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Dorofeyeva, V. A.
(Academy of Sciences (USSR) Moscow, Ussr)
Makalkin, A. B.
(Academy of Sciences (USSR) Moscow, Ussr)
Vityazev, A. V.
(Academy of Sciences (USSR) Moscow, Ussr)
Date Acquired
September 6, 2013
Publication Date
January 1, 1993
Publication Information
Publication: Lunar and Planetary Inst., Twenty-fourth Lunar and Planetary Science Conference. Part 1: A-F
Subject Category
Accession Number
Distribution Limits
Work of the US Gov. Public Use Permitted.

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