One of the most surprising properties of extrasolar planets is the eccentricity of their orbits, which vary from nearly circular (e ∼ 0) to highly eccentric ones (up to e ∼ 0.9). Planet-planet scattering with no gas disk has successfully reproduced the observed eccentricity distribution. However, this scenario alone cannot explain the distribution of planetary semi-major axes if giant planets form outside of ∼ 1 AU. Taking into account the effects of a residual gas disk after planet formation, we investigate the onset of dynamical instability in young planetary systems. Using a hybrid symplectic integrator + gas dynamics code, we demonstrate how planet-disk interactions along with planet-planet dynamical interactions could explain both the observed semi-major axis and eccentricity distributions of extrasolar planets.
|Original language||English (US)|
|Title of host publication||Extreme Solar Systems|
|Editors||D Fischer, Frederic A Rasio, S E Thorsett, A Wolszczan|
|Publisher||Astronomical Society of the Pacific|
|Number of pages||7|
|State||Published - 2008|
|Name||Astronomical Society of the Pacific Conference Series|