Turbulence in Core-Collapse Supernovae

Understand

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.