Three-dimensional simulations of rapidly rotating core-collapse supernovae: finding a neutrino-powered explosion aided by non-axisymmetric flows

TL;DR

This study uses 3D simulations to show that rapid rotation and non-axisymmetric flows can trigger neutrino-powered supernova explosions in massive stars that would otherwise fail, highlighting the importance of 3D effects.

Contribution

First 3D simulations demonstrating rotation-assisted supernova explosions driven by non-axisymmetric instabilities and spiral flows.

Findings

Rotation can enable explosions in otherwise failing models.

Non-axisymmetric instabilities enhance energy transport to the shock.

Explosion is stronger perpendicular to the rotational axis.

Abstract

We report results from a series of three-dimensional (3D) rotational core-collapse simulations for $11.2$ and 27 $M_{/odot}$ stars employing neutrino transport scheme by the isotropic diffusion source approximation. By changing the initial strength of rotation systematically, we find a rotation-assisted explosion for the 27$M_{/odot}$ progenitor, which fails in the absence of rotation. The unique feature was not captured in previous two-dimensional (2D) self-consistent rotating models because the growing non-axisymmetric instabilities play a key role. In the rapidly rotating case, strong spiral flows generated by the so-called low $T/|W|$ instability enhance the energy transport from the proto-neutron star (PNS) to the gain region, which makes the shock expansion more energetic. The explosion occurs more strongly in the direction perpendicular to the rotational axis, which is different from previous 2D predictions.