Orbital Architecture of Planetary Systems Formed by Gravitational Scattering and Collision

Presenter: Eiichiro KOKUBO
We investigate the formation of planets from protoplanets using N-body simulations. The goal of this study is to obtain the basic scaling laws for the
orbital architecture of planetary systems formed by gravitational scattering and collision among protoplanets, in other words, the final state of accretionary evolution of self-gravitating bodies. We systematically change the system parameters of initial protoplanet systems such as the total mass, mean semimajor axis and angular momentum deficit and investigate their effects on final planetary
systems. We find that the orbital architecture can be scaled by the Hill radius of planets and the ratio of the physical radius to the Hill radius. The mean eccentricity increases with the mean orbital separation and the final state is determined by the physical to Hill radius ratio.