Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.245...30b&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 245, July 1, 1990, p. 30-39. Research supported by the
Astronomy and Astrophysics
Astronomy
26
Computerized Simulation, Many Body Problem, Planetary Evolution, Terrestrial Planets, Astronomical Models, Gravitational Effects, Protoplanets, Solar System
Scientific paper
Numerical simulations of the last stage of terrestrial planetary formation are performed using an N-body code similar to that of Lecar and Aarseth (1986). An improved treatment of collisions has been applied, which allows fragmentation and cratering, as well as accretion. Initial models consist of 200 bodies of total mass 2.3 x 10 to the 28th g, distributed in a two-dimensional ring of size 1 AU with initial circular orbits about the sun. Planetary embryos begin to form by accretion in the early stages when the relative velocities are small. Eventually, a small number of massive embryos emerge, and subsequently accrete nearly all the fragments. Final configurations of three different models yield four principal bodies with moderate eccentricities on a time-scale of 500,000 yr.
Aarseth Sverre J.
Beauge Christian
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