Hydrodynamics of core-collapse supernovae and their progenitors

TL;DR

This paper reviews recent progress and challenges in understanding the multi-dimensional fluid dynamics involved in core-collapse supernovae and their progenitors, emphasizing simulation advancements and physical realism.

Contribution

It provides a comprehensive overview of recent developments in 3D supernova simulations, highlighting progress in shock revival mechanisms and the integration of multi-dimensional phenomena.

Findings

Successful 3D supernova models have been developed.

Progress in understanding shock revival mechanisms.

Identification of challenges in simulation realism.

Abstract

Multi-dimensional fluid flow plays a paramount role in the explosions of massive stars as core-collapse supernovae. In recent years, three-dimensional (3D) simulations of these phenomena have matured significantly. Considerable progress has been made towards identifying the ingredients for shock revival by the neutrino-driven mechanism, and successful explosions have already been obtained in a number of self-consistent 3D models. These advances also bring new challenges, however. Prompted by a need for increased physical realism and meaningful model validation, supernova theory is now moving towards a more integrated view that connects multi-dimensional phenomena in the late convective burning stages prior to collapse, the explosion engine, and mixing instabilities in the supernova envelope. Here we review our current understanding of multi-D fluid flow in core-collapse supernovae and their progenitors. We start by outlining specific challenges faced by hydrodynamic simulations of core-collapse supernovae and of the late convective burning stages. We then discuss recent advances and open questions in theory and simulations.