Toward an Accurate Model of the Formation and Composition of Terrestrial Planets

We have developed a comprehensive methodology to model the formation of terrestrial planets and their composition. Using a combination of SPH and N-body codes, we model the collisions and growth of embryos to planetary bodies accurately. We simulate collisions directly, and for the first time, consider the loss of volatiles (e.g., water) due to the heat of the impact, mass-removal during collisions, and ice-sublimation during orbital evolution of bodies. Our results present a more accurate and quantifiable estimate of the composition of terrestrial planets, and are informed directly from their geological evolution. Our methodology also tracks the transfer of water and volatiles from one body to another, self-consistently.