Magnetic field generation by the stationary accretion shock instability

TL;DR

This paper investigates how the stationary accretion shock instability (SASI) can generate strong magnetic fields in supernova environments without rotation, potentially impacting explosion mechanisms.

Contribution

It demonstrates that SASI alone can amplify magnetic fields to significant strengths in supernova-like conditions, a novel insight into supernova dynamics.

Findings

SASI can produce magnetic fields of about 10^{15} G

Magnetic field amplification occurs on relevant supernova timescales

Magnetic fields are generated without the need for stellar rotation

Abstract

By adding a weak magnetic field to a spherically symmetric fluid configuration that caricatures a stalled shock in the post-bounce supernova environment, we explore the capacity of the stationary accretion shock instability (SASI) to generate magnetic fields. The SASI develops upon perturbation of the initial condition, and the ensuing flow generates--{\em in the absence of rotation}--dynamically significant magnetic fields ($\sim 10^{15}$ G) on a time scale that is relevant for the explosion mechanism of core-collapse supernovae. We describe our model, present some recent results, and discuss their potential relevance for supernova models.