Host: The Japanese Society for Planetary Sciences: Local Organizing Committee for 2007 Fall Meeting
We have investigated accretion of terrestrial planets from planetesimals around M dwarfs through N-body simulations including the effect of tidal interaction with disk gas. N-body simulations start from 5,000-10,000 planetesimals. Their self-gravity is calculated with GRAPE-6. Tidal damping of orbital eccentricity, inclination and semimajor axis is calculated with forces in equations of motion that are obtained by the linear theory.
Because of the low luminosity of M dwarfs, their terrestrial planet regions are located near central stars (< 0.3AU) and habitable zones (HZ) are ~0.1AU. Accordingly, the formation of terrestrial planets around M dwarfs would differ from that around G dwarfs. Orbital decay due to the tidal interaction with disk gas (type I migration) and aerodynamical gas drag is much more efficient in such inner regions than that in HZs around solar-type stars. Furthermore, the terrestrial planet accretion would be affected by the disk inner edge (~ 0.05AU). Planetary embryos and planetesimals that migrate from outer regions pile up there and they would affect accretion in HZs. We will present preliminary results of N-body simulations.
