Evolution of planetary systems emerging out of gas disks
Meeting Room 2, CMS
Previous N-body simulations of multiple planetary systems without a gas disk have successfully reproduced the observed eccentricity distribution by assuming that the planetary systems are dynamically "active" when the gas disk dissipates. The planet-planet interactions alone, however, cannot explain the semi-major axis distribution. We numerically study the evolution of planetary systems as the gas disk dissipates by using a hybrid N-body and 1D gas disk code, and highlight disk's role in shaping the planetary systems.