From: arXiv.org e-Print archive
Posted: Tuesday, March 10, 2015
Alessandra Mastrobuono-Battisti, Hagai B. Perets, Sean N. Raymond
(Submitted on 25 Feb 2015)
Most of the properties of the Earth-Moon system can be explained by a collision between a planetary embryo and the growing Earth late in the accretion process. Simulations show that most of the material that eventually aggregates to form the Moon originates from the impactor. However, analysis of the terrestrial and lunar isotopic composition show them to be highly similar. In contrast, the compositions of other solar system bodies are significantly different than the Earth and Moon. This poses a major challenge to the giant impact scenario since the Moon-forming impactor is then thought to also have differed in composition from the proto-Earth. Here we track the feeding zones of growing planets in a suite of simulations of planetary accretion, in order to measure the composition of Moon-forming impactors.
We find that different planets formed in the same simulation have distinct compositions, but the compositions of giant impactors are systematically more similar to the planets they impact. A significant fraction of planet-impactor pairs have virtually identical compositions. Thus, the similarity in composition between the Earth and Moon could be a natural consequence of a late giant impact.
Comments: 34 pages, 7 Figures, 4 Tables. Accepted for publication in Nature
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:1502.07346 [astro-ph.EP] (or arXiv:1502.07346v1 [astro-ph.EP] for this version)
From: Alessandra Mastrobuono Battisti
[v1] Wed, 25 Feb 2015 21:00:07 GMT (3991kb)
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