Three-Dimensional Hydrodynamic Simulations of Convective Nuclear Burning In Massive Stars Near Iron Core Collapse

Understand

Non-spherical structure in massive stars at the point of iron core collapse can have a qualitative impact on the properties of the ensuing core-collapse supernova explosions and the multi-messenger signals they produce.

• Strong perturbations can aid successful explosions by strengthening turbulence in the post-shock region.
• Here, we report on a set of $4\pi$ 3D hydrodynamic simulations of O- and Si-shell burning in massive star models of varied initial masses using MESA and the FLASH simulation framework.
• We evolve four separate 3D models for roughly the final ten minutes prior to, and including, iron core collapse.