MIGRATION OF PLANETS EMBEDDED IN A CIRCUMSTELLAR DISK
- 10 June 2011
- journal article
- Published by American Astronomical Society in The Astrophysical Journal
- Vol. 735 (1), 29
- https://doi.org/10.1088/0004-637x/735/1/29
Abstract
Planetary migration poses a serious challenge to theories of planet formation. In gaseous and planetesimal disks, migration can remove planets as quickly as they form. To explore migration in a planetesimal disk, we combine analytic and numerical approaches. After deriving general analytic migration rates for isolated planets, we use N-body simulations to confirm these results for fast and slow migration modes. Migration rates scale as m –1 (for massive planets) and (1 + (e H/3)3)–1, where m is the mass of a planet and e H is the eccentricity of the background planetesimals in Hill units. When multiple planets stir the disk, our simulations yield the new result that large-scale migration ceases. Thus, growing planets do not migrate through planetesimal disks. To extend these results to migration in gaseous disks, we compare physical interactions and rates. Although migration through a gaseous disk is an important issue for the formation of gas giants, we conclude that migration has little impact on the formation of terrestrial planets.Keywords
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