4:30 PM - 4:45 PM
[PPS07-16] Collisional fragmentation of planetesimals in the giant impact stage
Keywords:Planet formation, collisional fragmentation
Mars-sized protoplanets formed in a protoplanetary disk further grow to be terrestrial planets via mutual collisions between protoplanets or "giant impacts" after gas depletion, which are believed to from the terrestrial planets in the solar system. The resultant planets mainly have eccentricities much larger than those of Earth and Venus, so that the dynamical friction of a planetesimal disk is needed for eccentricity damping. However, planetesimals stirred by planets are dynamically so hot that collisional fragmentation of planetesimals inhibits the dynamical friction. Therefore, the N-body simulation including collisional fragmentation as well as dynamical friction is required for the investigation of giant impact stage. We newly develop the N-body code with protoplanets and super particles representing planetesimals and smaller fragments. Through the simulations with the code, we give constrains on the total mass and radii of planetesimals remaining in the giant impact stage.