演講資訊

摘要：

I will present the currently most comprehensive and self-consistent approach to simulating the late stage of terrestrial planet formation. Our approach begins with simulating the collisional growth of planetesimals and continues with resolving giant impacts using our state-of-the-art SPH code. The approach takes into account all relevant physical processes including the dynamical friction due to the debris and planetesimal disks, migration of planetesimals and embryos, and the perturbation as well as possible migration of giant planets. As the most important step toward a fully comprehensive and realistic model, our approach incorporates SPH simulations into N-body integrations in real time allowing collisions to be simulated accurately as they occur. Results point to several important findings. For instance, in the context of our solar system, almost all simulations produced an Earth-analog. In the context of extrasolar planets, when giant planet migration is considered, rocky super-Earths are produced routinely. The most important finding of our simulations is that while giant planets may affect the inventory of planet-forming material, hence their compositions, they play no role in the mechanics of the formation of rocky planets and the transfer/transport of chemical compounds to them. Formation and delivery of chemical compounds are merely due to the mutual interactions of planetary embryos, a process that occurs even when no giant planet exists. I will present the results of our study and discuss their applications to the formation, composition, and early differentiation of Earth-like planets and rocky super-Earths.