Direct Simulation of Planet Formation with a Million Planetesimals: First Results

Details Direct Simulation of Planet Formation with a Million Planetesimals: First Results Direct Simulation of Planet Formation with a Million Planetesimals: First Results

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998baas...30r1052r&link_type=abstract

American Astronomical Society, DPS meeting #30, #21.P13; Bulletin of the American Astronomical Society, Vol. 30, p.1052

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We present the first results from our direct simulations of planet formation using N = 10(6) rocky particles (see also BAAS 30, 765 and BAAS 29, 1027). Currently ~ 1000 yr of evolution have been simulated under the assumption of perfect accretion in a 4.7 M_⊕ disk that extends from 0.8 to 3.8 AU with a surface density distribution Sigma ~ r(-3/2) . The four present-day giant planets are included as perturbers. The disk was started cold, allowing the growth of resonance gaps and spiral density waves due to the giant planets to be seen clearly. We are in the process of testing a scheme to improve the speed of the method by at least an order of magnitude by exploiting the near-Keplerian nature of the planetesimal orbits. Preliminary results from this improvement are presented. We also present a simulation of the formation of the Galilean satellites using N = 10(5) icy particles in a 0.065 M_⊕ disk extending from 3 x 10(5) to 2.3 x 10(6) km around Jupiter and having the same r(-3/2) density law. Particles are allowed to merge following a collision only if their rebound velocity is less than their mutual escape velocity, and if the spin of the resulting merged body does not exceed the classical breakup limit; otherwise the particles bounce and lose a fixed fraction of their relative energy. Fragmentation has not been implemented at this time. We find that this system evolves very quickly, with ~ 33% of the particles having merged after only ~ 150 d, or about 80 Io orbits. This simple model begins with a uniform population of 100 km radius planetesimals and ignores gas dynamics. The applicability of this model toward the actual formation of giant planet moons is discussed.

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