Astronomy and Astrophysics – Astronomy
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dda....41.1007m&link_type=abstract
American Astronomical Society, DDA meeting #41, #10.07; Bulletin of the American Astronomical Society, Vol. 41, p.939
Astronomy and Astrophysics
Astronomy
Scientific paper
Given the severe challenges in forming giant planets so close to their host star, disk-induced migration is often invoked to explain their small semi-major axes. Migration theory is usually divided into two limiting cases: Type I migration, in which the planet remains embedded in the disk, and Type II migration, in which the planet is sufficiently massive that it clears a gap in the disk in the vicinity of its orbit and follows the viscous evolution of the disk. However, recent hydrodynamic simulations of giant planets in circumstellar disks do not seem to follow this prescription; giant planet migration rates show a dependence on planet mass that is inconsistent with migrration on a constant, viscous timescale (Edgar 2008). We use FARGO to extend the work of Edgar (2008) and Bate (2003) to higher viscosities and larger planet masses and present the results in the context of distinguishing between the standard description of giant planet migration and that of Edgar (2007). Additionally, we present simulations of planets on eccentric orbits and describe how eccentricity modifies giant planet migration.
Ford Eric B.
Moorhead Althea
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