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Title:
Evolution of Giant Planets in Eccentric Disks
Authors:
D'Angelo, Gennaro; Lubow, Stephen H.; Bate, Matthew R.
Affiliation:
AA(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL, UK; and Space Science and Astrobiology Division, NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035 ), AB(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 ), AC(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL, UK )
Publication:
The Astrophysical Journal, Volume 652, Issue 2, pp. 1698-1714. (ApJ Homepage)
Publication Date:
12/2006
Origin:
UCP
Astronomy Keywords:
Accretion, Accretion Disks, Hydrodynamics, Methods: Numerical, Stars: Planetary Systems: Formation
DOI:
10.1086/508451
Bibliographic Code:
2006ApJ...652.1698D

Abstract

We investigate the interaction between a giant planet and a viscous circumstellar disk by means of high-resolution, two-dimensional hydrodynamic simulations. We consider planetary masses that range from 1 to 3 Jupiter masses (MJ) and initial orbital eccentricities that range from 0 to 0.4. We find that a planet can cause eccentricity growth in a disk region adjacent to the planet's orbit, even if the planet's orbit is circular. Disk-planet interactions lead to growth in a planet's orbital eccentricity. The orbital eccentricities of a 2MJ and a 3MJ planet increase from 0 to 0.11 within about 3000 orbits. Over a similar time period, the orbital eccentricity of a 1MJ planet grows from 0 to 0.02. For a case of a 1MJ planet with an initial eccentricity of 0.01, the orbital eccentricity grows to 0.09 over 4000 orbits. Radial migration is directed inward but slows considerably as a planet's orbit becomes eccentric. If a planet's orbital eccentricity becomes sufficiently large, e>~0.2, migration can reverse and so be directed outward. The accretion rate toward a planet depends on both the disk and the planetary orbital eccentricity and is pulsed over the orbital period. Planetary mass growth rates increase with planetary orbital eccentricity. For e~0.2, the mass growth rate of a planet increases by ~30% above the value for e=0. For e>~0.1, most of the accretion within the planet's Roche lobe occurs when the planet is near the apocenter. Similar accretion modulation occurs for flow at the inner disk boundary, which represents accretion toward the star.
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