Following the multi-isotope trail to understanding the formation and early evolution of our Solar System

Isotopic ratios are commonly used to trace the origin of Solar System bodies. This is fundamental but still a highly-debated topic. It is still unclear whether most of the organics are inherited from the cold and dense molecular parent cloud of our Sun, or if they are the result of chemical processing within the solar nebula protoplanetary disk. We will put a particular focus on nitrogen and oxygen fractionation, whereas carbon and deuterium fractionation will be the side products of the project. We will undertake following studies: (1) We will build a first consistent isotopic fractionation chemical network of D, C, N, and O both for the gas phase and surface including spin-state chemistry. (2) We will model the isotopic ratios for a range of protoplanetary disks using a state-of-the-art gas-grain-mantle 3-phase chemical code with proper physical structures.