Accretion in the inner nebula - The relationship between terrestrial planetary compositions and meteorites

Computer Science

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Meteoritic Composition, Planetary Composition, Solar System Evolution, Terrestrial Planets, Abundance, Accretion Disks, Asteroids, Lunar Composition, Protoplanets, Solar Activity

Scientific paper

The bulk compositions of the terrestrial planets are assessed. Venus and earth probably have similar bulk compositions, but Mars is enriched in volatile elements. The inner planets are all depleted in volatile elements, as shown by K/U ratios, relative to most meteorites and the CI primordial values. Terrestrial upper-mantle Mg/Si ratios are high compared with CI data. If they are representative of the bulk earth, then the earth accreted from a segregated suite of planetesimals that had nonchondritic major element abundances. The CI meteorite abundances, despite aqueous alteration, match the solar data and provide the best estimate for the composition of the solar nebula, including the iron abundance. There appears to have been little mixing between meteorite and planetary formation zones, as shown by the oxygen isotope variations, lack of mixing of meteorite groups, and differences in K/U ratios. In summary, it appears that the final accretion of planets did not result in widespread homogenization, and that mixing zones were not more than about 0.3 AU wide. Although the composition of the moon is unique and its origin due to an essentially random event, its presence reinforces the planetesimal hypothesis and the importance of stochastic processes during planetary accretion in the inner solar system.

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