Progenitors of Core-Collapse Supernovae

TL;DR

This paper reviews the evolution of massive stars leading to core-collapse supernovae, discussing properties at collapse, effects of metallicity and rotation, uncertainties in modeling, and insights from 3D hydrodynamic simulations.

Contribution

It provides a comprehensive review of massive star evolution, highlights uncertainties in convection modeling, and presents new 3D simulations informing 1D stellar models.

Findings

3D hydrodynamic simulations of convection in carbon burning.

Insights into convective boundary mixing for 1D models.

Discussion of uncertainties in massive star evolution modeling.

Abstract

Massive stars have a strong impact on their surroundings, in particular when they produce a core-collapse supernova at the end of their evolution. In these proceedings, we review the general evolution of massive stars and their properties at collapse as well as the transition between massive and intermediate-mass stars. We also summarise the effects of metallicity and rotation. We then discuss some of the major uncertainties in the modelling of massive stars, with a particular emphasis on the treatment of convection in 1D stellar evolution codes. Finally, we present new 3D hydrodynamic simulations of convection in carbon burning and list key points to take from 3D hydrodynamic studies for the development of new prescriptions for convective boundary mixing in 1D stellar evolution codes.