Accretion Of Terrestrial Planets From A Compact Planetesimal Disk

Details Accretion Of Terrestrial Planets From A Compact Planetesimal Disk Accretion Of Terrestrial Planets From A Compact Planetesimal Disk

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.4208m&link_type=abstract

American Astronomical Society, DPS meeting #39, #42.08; Bulletin of the American Astronomical Society, Vol. 39, p.497

Astronomy and Astrophysics

Astronomy

Scientific paper

Remnant planetesimals might have played an important role to reduce enhanced orbital eccentricities of the terrestrial planets after their formation via giant impacts. However, the population and the size distribution of remnant planetesimals during and after the giant impact stage are unknown, because simulations of planetary accretion in the runaway growth and giant impact stages have been conducted rather independently. Here we report results of direct N-body simulations through formation of terrestrial planets beginning from a compact planetesimal disk. Fixing the total mass and angular momentum to be those for the current terrestrial planets, we vary the width (0.3 and 0.5AU) and the number of planetesimals (1000-5000) of the initial planetesimal disk. We find that, in most of the cases, a planetesimal disk results in three planets with similar size, and sometimes with a fourth small planet near the location of Mars. Since sufficient amount planetesimals remain even after giant impacts of protoplanets, orbital eccentricities of final planets are, in most of the cases, as small as those of the current Earth and Venus. Final eccentricities are likely to increase with the initial mass and surface density of planetesimals, though the dependence on the initial mass is very weak.

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