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起源（见本项目第一阶段），还取决于鹅卵石、星子和行星胚胎在成为地球一部分的过程中的演变。鹅卵石在冰线处部分蒸发了其挥发性成分，而星子可能已经分化，这对碰撞后和地球最终形成过程中星子的挥发性成分产生了严重影响。基于我们在第一阶段的结果，例如，鹅卵石的流动和积聚，星子的形成以及使用TWO-POP-PY代码和LIPAD将混合物合并到行星胚胎中，我们现在想集中在A：更好地模拟雪线上的鹅卵石的命运；B：研究LIPAD代码中预测的碰撞，使用实际的SPH模拟碰撞星子和行星胚胎，以更好地跟踪它们的化学成分。结合我们从同事那里了解到的地球的化学/矿物学/地质记录，我们将把太阳星云的特性与使地球适宜居住的化学混合物联系起来。

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.