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Precondensed matter - Key to the early solar systemExplicit astrophysical details are developed for the hypothesis that chemical and isotopic anomalies in primitive solar-system samples reflect routine initial chemical conditions within precondensed matter. The central feature of this theory concerns the chemical state of presolar dust, which is regarded as never having been vaporized in the region where the most chemically primitive samples (carbonaceous meteorites) accumulated. It is suggested that the initial chemical state of heavy atoms during meteorite and planetary accumulation was distributed between a refractory-mineral component from high-temperature condensation and a volatile component resulting from cold matter adhering to preexisting grains. Thermal conditions in the solar nebula are considered along with the existence of supernova condensates and other thermal condensates in the interstellar dust. Fractionation into volatile and refractory elements is idealized in terms of four distinct interstellar components, and the fractionated precondensed matter is described.
Document ID
19790029789
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Clayton, D. D.
(Rice University Houston, Tex., United States)
Date Acquired
August 9, 2013
Publication Date
October 1, 1978
Subject Category
Astrophysics
Accession Number
79A13802
Funding Number(s)
CONTRACT_GRANT: NSF AST-74-20076
CONTRACT_GRANT: NSG-7361
Distribution Limits
Public
Copyright
Other

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