Did iron meteorites form in the asteroid belt - Evidence from thermodynamic models

Details Did iron meteorites form in the asteroid belt - Evidence from thermodynamic models Did iron meteorites form in the asteroid belt - Evidence from thermodynamic models

Dec 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979icar...40..471s&link_type=abstract

(Asteroids and Planet X Meeting, University of Arizona, Tucson, Ariz., March 1979.) Icarus, vol. 40, Dec. 1979, p. 471-483.

Other

Asteroid Belts, Astronomical Models, Iron Meteorites, Planetary Evolution, Planetary Nebulae, Thermodynamics, Abundance, Chondrites, Condensing, Meteoritic Composition, Oxidation, Solar System, Trace Elements, Vapor Phases

Scientific paper

The major iron meteorite groups are defined essentially by their Ga, Ge, and Ni contents. It now seems clear that the differences between their abundances of Ga and Ge were produced by the process of condensation and accretion in the primordial solar nebula. The simplest interpretation of the Ni abundance, and its variations between the groups, is also that is was fixed during condensation and accretion and it reflects the oxidation state of the nebula during condensation and accretion. The abundance patterns of 17 other trace elements have been examined and are consistent with this model. It is believed to be the simplest model published and most consistent with analogous calculations for the chondrites. If it is correct, then the iron meteorite groups formed over a very wide range of pressures, 10 to the -4th to 10 to the -8th power atm. Such a range could only be found in a restricted region of the nebula, such as the asteroid belt, if a complex accretion sequence inside a protoplanet occurred. More likely, the iron meteorites were formed in widely dispersed regions of the nebula and only one group formed in the asteroid belt, probably group IIIAB. Groups IAB and IIAB formed near the Sun, and group IVA formed beyond the orbit of Jupiter.

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