Neutrino-driven massive stellar explosions in 3D fostered by magnetic fields via turbulent $\alpha$-effect

TL;DR

This study uses 3D simulations to show that magnetic field amplification via the turbulent $ ext{α}$-effect in rotating, magnetized progenitors significantly aids shock revival in core-collapse supernovae, highlighting the role of magnetic turbulence.

Contribution

It demonstrates the exponential amplification of magnetic fields through the $ ext{α}$-effect in 3D supernova models, linking turbulence, magnetic fields, and shock revival.

Findings

Magnetic fields grow exponentially in the gain region due to the $ ext{α}$-effect.

Rotation enhances the magnetic field amplification and accelerates shock revival.

Magnetic turbulence near the poles promotes neutrino-driven shock revival.

Abstract

We investigate the influence of magnetic field amplification on the core-collapse supernovae in highly magnetized progenitors through three-dimensional simulations. By considering rotating models, we observe a strong correlation between the exponential growth of the magnetic field in the gain region and the initiation of shock revival, with a faster onset compared to the non-rotating model. We highlight that the mean magnetic field experiences exponential amplification as a result of $\alpha$-effect in the dynamo process, which works efficiently with the increasing kinetic helicity of the turbulence within the gain region. Our findings indicate that the significant amplification of the mean magnetic fields leads to the development of locally intense turbulent magnetic fields, particularly in the vicinity of the poles, thereby promoting the revival of the shock by neutrino heating.