Turbulence in core-collapse supernovae

David Radice, Ernazar Abdikamalov, Christian D. Ott, Philipp Mösta, Sean M. Couch, Luke F. Roberts

Research output: Contribution to journalReview article

17 Citations (Scopus)

Abstract

Multidimensional simulations show that non-radial, turbulent, fluid motion is a fundamental component of the core-collapse supernova explosion mechanism. Neutrino-driven convection, the standing accretion shock instability, and relic-perturbations from advanced nuclear burning stages 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.

Original languageEnglish
Article number053003
JournalJournal of Physics G: Nuclear and Particle Physics
Volume45
Issue number5
DOIs
Publication statusPublished - Apr 9 2018

Keywords

  • astrophysical turbulence
  • methods: numerical
  • supernovae

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

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