Turbulence in Core-Collapse Supernovae

TL;DR

This paper reviews the role of turbulence, convection, and magnetic fields in the core-collapse supernova explosion mechanism, emphasizing their impact on the dynamics and outcomes of massive star explosions.

Contribution

It provides a comprehensive overview of multidimensional turbulence phenomena and their influence on supernova explosions, integrating recent simulation insights and theoretical understanding.

Findings

Turbulence significantly affects supernova explosion dynamics.

Neutrino-driven convection and instabilities are crucial for explosion success.

Magnetic fields and protoneutron star convection also play important roles.

Abstract

Multidimensional simulations show that non-radial, turbulent, fluid motion is a fundamental component of the core-collapse supernova (CCSN) explosion mechanism. Neutrino-driven convection, the standing accretion shock instability, and relic-perturbations from advanced stages of nuclear burning can all impact the outcome of core collapse in a qualitative and quantitative way. Here, we review the current understanding of these phenomena and their role in the explosion of massive stars. We also discuss the role of protoneutron star convection and of magnetic fields in the context of the delayed neutrino mechanism.