Condensation and the composition of iron meteorites

Details Condensation and the composition of iron meteorites Condensation and the composition of iron meteorites

Oct 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978e%26psl..41..128s&link_type=abstract

Earth and Planetary Science Letters, vol. 41, no. 2, Oct. 1978, p. 128-138.

Computer Science

11

Condensation, Iron Meteorites, Meteoritic Composition, Pressure Effects, Protostars, Abundance, Gallium, Germanium, Nebulae, Nickel, Temperature Effects, Pressure, Condensation, Composition, Iron Meteorites, Temperatures, Abundance, Equilibrium, Nickel, Gallium, Germanium, Samples, Meteorite, Gases, Atmosphere, Sulfur, Carbon, Phosphorus, Metals, Mineralogy

Scientific paper

The condensation and accretion conditions for the four major iron meteorite groups and group IVB are calculated on the assumption of equilibrium condensation in the primordial nebula. It is found that there are two temperature regions at which the Ni contents of the above-mentioned groups can be produced by equilibrium processes: soon after condensation of the metal, and below 750 K. The Ga and Ge contents of IAB, IIAB and IIIAB are too high for early condensates and these most probably formed over the lower-temperature region. The Ni, Ga and Ge contents of IVA can be explained by its parent body also being an early condensate but at different pressures from IVB. Trace elements and S abundance in IVA, however, suggest that it accreted at similar temperatures to IAB, IIAB, and IIIAB. The abundance of C in IAB suggests that it formed at about 0.0001 atm, so that IIAB formed in regions at 0.000005 atm and IVA at 0.00000001 atm.

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