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Iron - Whence it came, where it wentDeterminations of the abundances of iron and related elements in the photosphere, chromosphere, and corona of the sun as well as in solar and galactic cosmic rays are reviewed and compared with abundances derived from meteoritic data. Observed solar system abundances are found to be in accord with predictions of nucleosynthesis under either hydrostatic or explosive conditions but cannot yet be used to define these processes uniquely. The distribution of iron among planets and meteorites can probably be adequately modelled by condensation and fragmentation under equilibrium conditions above about 700 K, but below that temperature it is likely that inhibited solid-state diffusion perturbed attainment of equilibrium. Pertinent factors which are presently unknown include the mechanism responsible for metal-silicate fractionation, the grain size achieved by metallic iron in the nebula, and whether iron-bearing silicate formed prior to accretion.
Document ID
19770052167
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Kerridge, J. F.
(California, University Los Angeles, Calif., United States)
Date Acquired
August 9, 2013
Publication Date
February 1, 1977
Publication Information
Publication: Space Science Reviews
Volume: 20
Subject Category
Lunar And Planetary Exploration
Accession Number
77A35019
Funding Number(s)
CONTRACT_GRANT: NGL-05-009-005
CONTRACT_GRANT: NSG-7121
CONTRACT_GRANT: NGR-05-007-289
Distribution Limits
Public
Copyright
Other

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