Orbital Migration of Protoplanets

Details Orbital Migration of Protoplanets Orbital Migration of Protoplanets

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..249t&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Computer Science

Scientific paper

We performed global 2D-hydrodynamical simulations to calculate gravitational torques on a protoplanet embedded in a protoplanetry disk and compared the results with those by previous linear calculations. The results are as follows. (1)For a small planet, whose Hill radius is much less than the disk scale height, the planet migrates inward as the previous linear theory predicts. (2)For a more massive planet, the migration speed is slower than that by the linear theory. (3)If the mass of a planet is larger than the critical value, which depends upon disk parameters, the planet migrates outward. Our conclusion is that planets do not always spiral toward the central star, but large planets move outward.

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