Core-collapse supernova (CCSN) explosions mark the end of the life of stars heavier than 10 times the mass of our sun,
they play a crucial role for our understanding of the chemical composition of the universe and they are ideal laboratories
for effects of neutrino and particle physics. Current research in astrophysics, astronomy and cosmochemistry that
makes use of theoretical CCSN models for comparing to observations, still, however, relies predominantly on one-dimensional, i.e. spherically symmetric
parameterized calculations. During the last decade, however, multi-dimensional and nearly parameter-free simulation have become possible. These advances
have demonstrated that multi-dimensional simulations predict a wide variety of conditions
that cannot be found in simple 1D models, but it remains unclear if they can solve some of the disagreements between observations and theoretical supernova models.
This project aims at advancing the state-of-the-art by calculating the detailed composition of CCSN
material (i.e. isotopic nucleosynthesis yields) based on the most recent, first-principles 3D simulations and by providing the results to the community.
Since the landscape of supernova explosions spans a wide range of possible initial conditions, such as a star's initial mass, its initial composition and its environment (e.g. in a multiple system),
a wide range of models needs to explored to capture the whole diversity of possible outcomes. This project, thus, constitutes a fist step, focussing on a few models for single stars, but it aims to provide
the key elements to easily extend the approach to illuminate the full role of supernovae for the origin of the elements.
