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A core origin for group IVA iron meteorites - A reply to Moren and GoldsteinBecause uncertainties in experimental data are large, one has considerable latitude in choosing the input parameters needed to calculate iron meteorite cooling rates. The best way to test input parameters is by examining their ability to yield the observed properties of the meteorites. Our phase diagram yields fits to kamacite profiles that are superior to those based on the Moren-Goldstein phase diagram. Our method of allowing for the effect of P on the Ni diffusion coefficient takes into account the enhancement in this effect with decreasing temperature; Moren and Goldstein use a relationship derived for a temperature of 1100 C, well outside the 700-350 C range where kamacite growth occurs. Use of our input parameters yields cooling rates in IVA irons that are independent of composition, consistent with a core origin. Since the fractionation of siderophiles in group IVA also indicates a core origin, we conclude that this is the correct model for this group.
Document ID
19780062044
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Willis, J.
(California Univ. Los Angeles, CA, United States)
Wasson, J. T.
(California, University Los Angeles, Calif., United States)
Date Acquired
August 9, 2013
Publication Date
July 1, 1978
Publication Information
Publication: Earth and Planetary Science Letters
Volume: 40
Issue: 2, Ju
Subject Category
Lunar And Planetary Exploration
Accession Number
78A45953
Funding Number(s)
CONTRACT_GRANT: NGR-05-007-329
Distribution Limits
Public
Copyright
Other

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