Mr Kevin Ebinger
Core-Collapse Supernovae (CCSNe) occur at the end of the evolution of massive stars. The detailed explosion mechanism of these violent events and their outcomes are still not fully understood. On the one hand multi-dimensional simulations of CCSNe are needed to investigate the underlying explosion mechanism. On the other hand they are currently too expensive to allow broad systematic studies, that are highly required to better understand these events. The PUSH method provides a parametrization framework for spherically symmetric simulations to efficiently study many important aspects of CCSNe: the effects of the shock passage through the star, explosive supernova nucleosynthesis and the progenitor-remnant connection. We calibrate PUSH to reproduce the observed properties of SN 1987A for an appropriate progenitor model and use the method to conduct a broad progenitor study. We discuss the explosion dynamics and energetics for stars of solar metallicity. Furthermore, the explodability of a wide range of progenitors is investigated, together with a possible distinction between low and high compactness progenitors in the explosion and remnant properties.