A 3D Simulation of a Neutrino-Driven Supernova Explosion Aided By Convection and Magnetic Fields

TL;DR

This study uses 3D neutrino magnetohydrodynamics simulations to show that magnetic fields, amplified by convection, can support supernova explosions even without rapid rotation, highlighting a potential subsidiary role of magnetism.

Contribution

First 3D simulation demonstrating the amplification of magnetic fields via a small-scale dynamo in neutrino-driven supernovae without rapid rotation.

Findings

Magnetic fields reach ~50% of kinetic energy in the gain region.

Magnetic fields support the development of supernova explosions.

Magnetic effects are significant even without rapid progenitor rotation.

Abstract

We study the impact of a small-scale dynamo in core-collapse supernovae using a 3D neutrino magnetohydrodynamics simulation of a $15 M_\odot$ progenitor. The weak seed field is amplified exponentially in the gain region once neutrino-driven convection develops, and remains dominated by small-scale structures. About $250\, \mathrm{ms}$ after bounce, the field energy in the gain region reaches $\mathord{\sim} 50\%$ of kinetic equipartition. This supports the development of a neutrino-driven explosion with modest global anisotropy, which does not occur in a corresponding model without magnetic fields. Our results suggest that magnetic fields may play a beneficial subsidiary role in neutrino-driven supernovae even without rapid progenitor rotation. Further investigation into the nature of magnetohydrodynamic turbulence in the supernova core is required.