Abstract DGP2026-35

Supernova explosions eject large amounts of material and newly made metals into interstellar space. Some of the ejecta is rapidly converted to dust, which can be incorporated in meteorites and early aggregates with their anomalous isotopic signatures. Meteorites can be analyzed using mass spectroscopy, where precise measurements have revealed various isotopic anomalies, the origin of which can be traced back to dust particles from supernovae that have merged with the meteorite's parent body during accretion processes. Because the presolar grains have preserved the chemical composition of the environment in which they formed, the anomalies caused by these particles carry important information about the formation of the Solar System and the relationships between the planets. To understand the origin of these anomalies, I compare data from mass spectroscopy of meteorites with theoretical supernova models. In my work I investigated the origin of Ni anomalies found in meteorites and I confirmed the obtained results by a similar analysis of Fe. For the analysis, I have used 6 different sets of core-collapse supernova models from the literature.