Identifying the origin of Earth's building material: Where do the earth building Planetesimals and Pebbles originate from? A numerical approach of the accretion phase of the earth.

地球的化学成分不仅取决于其建筑材料的来源(见本项目第一阶段)，还取决于鹅卵石、小行星和行星胚胎在成为地球一部分的过程中的进化。鹅卵石在冰线上部分蒸发了它们的挥发性成分，行星体可能已经分化，这对碰撞后和地球最终形成过程中星体的挥发性成分产生了严重影响。基于我们第一阶段的结果，例如卵石通量和吸积、行星小的形成以及使用Two-POP-PY程序和LIPAD将混合物并入行星胚胎，我们现在想重点关注A：更好地模拟雪线上鹅卵石的命运和B：研究LIPAD程序中预测的碰撞与实际SPH模拟的碰撞小行星和行星胚胎，以更好地跟踪它们的化学成分。结合我们从同事那里学到的地球的化学/矿物学/地质记录，我们将把太阳星云的特性与使地球宜居的化学鸡尾酒联系起来。

The chemical composition of Earth is not only determined by the origin of its building material (see Phase 1 of this project), but also by the evolution of the pebbles, planetesimals and planetary embryos on their way to become part of Earth. Pebbles partially evaporate their volatile content at the ice lines and planetesimals may already differentiate, which has severe impact on the volatile content of planetesimals after collisions and during the final build up of earth. Based on our results from Phase 1, e.g. pebble flux and accretion, planetesimal formation and incorporation of the mix into planetary embryos using the TWO-POP-PY code and LIPAD we now want to focus on A: a better modelling of the fate of pebbles at the snow line and B: study the collisions as predicted in the LIPAD code with actual SPH simulations of colliding planetesimals and planetary embryos, to keep better track of their chemical constituents. In combination with the chemical/ mineralogical/ geological record of the Earth as we learn from our colleagues, we will link the Solar Nebula properties to the chemical cocktail that made Earth habitable.