The orbital evolution of planetesimals due to gas drag and scattering by protoplanets is investigated from a point of view of the comet cloud formation. Gas drag by the gas disk causes planetesimals to spiral inwards to the Sun. On the inward migration, planetesimals encounter protoplanets. Planetesimals which are not captured into the mean motion resonances of protoplanets, can escape from their approach to the protoplanets, and are often largely scattered by the protoplanets. Planetesimals whose aphelion distances become larger by protoplanet scattering are candidates for members of the comet cloud. We demonstrate the above basic processes of planetesimal dynamics by numerical integration of planetesimal orbits.
8th Asian-Pacific Regional Meeting, Volume II
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