Turbulence and magnetic field amplification from spiral SASI modes in core-collapse supernovae

TL;DR

This paper investigates how spiral SASI modes in core-collapse supernovae induce turbulence and amplify magnetic fields through small-scale dynamo action, impacting supernova explosion mechanisms and neutron star properties.

Contribution

It demonstrates the development of turbulence from SASI-induced instabilities and shows magnetic field amplification via small-scale dynamo in supernova environments.

Findings

Turbulence arises from secondary SASI instabilities.

Magnetic fields are amplified through a small-scale dynamo.

Turbulence influences the evolution of SASI and supernova dynamics.

Abstract

The stationary accretion shock instability (SASI) plays a central role in modern simulations of the explosion phase of core-collapse supernovae (CCSNe). It may be key to realizing neutrino powered explosions, and possibly links birth properties of pulsars (e.g., kick, spin, and magnetic field) to supernova dynamics. Using high-resolution magnetohydrodynamic simulations, we study the development of turbulence, and subsequent amplification of magnetic fields in a simplified model of the post-bounce core-collapse supernova environment. Turbulence develops from secondary instabilities induced by the SASI. Our simulations suggest that the development of turbulence plays an important role for the subsequent evolution of the SASI. The turbulence also acts to amplify weak magnetic fields via a small-scale dynamo.