We have investigated the interaction of an eccentric orbit planet with a circumstellar disk by means of high-resolution hydrodynamical simulations. We have focused on the planet's mass range from one to a few Jupiter-masses. This study aims at characterizing the mass accretion and the orbital eccentricity evolution of giant planets. We find that the accretion rate depends on the orbital eccentricity of the protoplanet and that the accretion is pulsed on the orbital period, as found in simulations of binary star systems. Most of the mass is accreted while the protoplanet is around the apocenter position. A Jupiter-mass planet with orbital eccentricity e=0.3 accretes at a rate that is 33% higher than the accretion rate of a Jupiter-mass planet on a circular orbit. A 3 Jupiter-mass planet with e=0.1 is able to accrete, during one orbital period, 40% more mass than a similar size planet on a circular orbit. Simulations also indicate that a massive planet tend to sustain eccentricity growth in the disk, even with the planet revolving on a circular orbit, as already found for binary star systems. The interaction of the massive planet with the eccentric disk can then lead to the growth of the planet's orbital eccentricity. These results are consistent with observations of extrasolar planets. In fact, the most massive planets exhibit higher eccentricities than lower mass planets do. GD is supported by the UK Astrophysical Fluids Facility (UKAFF) through a UKAFF Fellowship. SL acknowledges support from NASA grant NNG04GG50G.
AAS/Division for Planetary Sciences Meeting Abstracts #37
- Pub Date:
- December 2005