A core origin for group IVA iron meteorites - A reply to Moren and Goldstein

Details A core origin for group IVA iron meteorites - A reply to Moren and Goldstein A core origin for group IVA iron meteorites - A reply to Moren and Goldstein

Jul 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978e%26psl..40..162w&link_type=abstract

Earth and Planetary Science Letters, vol. 40, no. 2, July 1978, p. 162-167.

Computer Science

4

Cooling, Iron Meteorites, Meteoritic Composition, Concentration (Composition), Diffusion Coefficient, Heat Transfer, Kamacite, Nickel Alloys, Phase Diagrams, Temperature Distribution, Iron, Meteorites, Cooling, Phase Diagrams, Taenite, Iron Meteorites, Phosphorus, Nickel, Diffusion, Temperatures

Scientific paper

Because 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.

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