Host: The Japanese Society for Planetary Sciences: Local Organizing Committee for 2006 Fall Meeting
We have investigated the final accretion stage of terrestrial planets from Mars-massprotoplanets that formed through oligarchic growth in a disk comparable to the minimummass solar nebula (MMSN), through N-body simulation including random torques exertedby disk turbulence due to Magneto-Rotational-Instability. For the torques, we used thesemi-analytical formula developed by Laughlin et al. (2004). The damping of orbitaleccentricities (in all runs) and type-I migration (in some runs) due to the tidal interactionswith disk gas are also included.
We have carried out aseries of N-body simulations including the random torques with different gas surface density and strengthof turbulence. We found that the orbital eccentricities pumped up by the turbulent torquesand associated random walks in semimajor axes tend to delay isolation of planets, resultingin more coagulation of planets. The eccentricities are still damped after planets becomeisolated. As a result, the number of final planets decreases with increase in strength ofthe turbulence, while Earth-mass planets with small eccentricities are still formed.
