Condensation of planets from protolunar disks after giant impacts

Giant impacts are crucial in early solar systems; their outcome is the formation of large protolunar disks. Using molecular dynamics simulations, we study the behavior of a silicate fluid with bulk silicate Earth's composition under typical impact conditions. We find that the Earth's protolunar disk reached a supercritical state. Then we follow the chemical evolution of the disk during its cooling. Liquids and gases separate according to the liquid-vapor dome. As the liquid rains towards the center, the leftover gas forms a hot dense atmosphere. Oxidized phases like SiO, O, O2, MgO, and cations like Na and Mg dominate the gas phase. Our simulations uncover a plethora of other phases present in the system, with lifetimes that allow them to play a role in the chemical and isotopic exchanges.