Turbulence in Core-Collapse Supernovae
Abstract
Multidimensional simulations show that non-radial, turbulent, fluid motion is a fundamental component of the core-collapse supernova (CCSN) explosion mechanism. Neutrino-driven convection, the standing accretion shock instability, and relic-perturbations from advanced stages of nuclear burning can all impact the outcome of core collapse in a qualitative and quantitative way. Here, we review the current understanding of these phenomena and their role in the explosion of massive stars. We also discuss the role of protoneutron star convection and of magnetic fields in the context of the delayed neutrino mechanism.
Cite
@article{arxiv.1710.01282,
title = {Turbulence in Core-Collapse Supernovae},
author = {David Radice and Ernazar Abdikamalov and Christian D. Ott and Philipp Moesta and Sean M. Couch and Luke F. Roberts},
journal= {arXiv preprint arXiv:1710.01282},
year = {2018}
}
Comments
27 pages, 8 figures. Invited review for J. Phys. G special issue: "Focus on microphysics in core-collapse supernovae: 30 years since SN1987A". Accepted version