Speaker
Description
In recent years, it has become apparent that realistic, 3D progenitors can play an important role in the explosions of neutrino-driven core-collapse supernovae. While 3D shell convection simulations have been performed for a number of progenitors, thus far, tests haven't been done for magnetorotational supernova progenitors. These progenitors are expected to be very rapidly rotating and strongly magnetic, and are expected to end their lives in a hypernova explosions.
In this talk, I will present a first 3D magnetohydrodynamic (MHD) simulation of oxygen, neon and carbon shell burning in a rapidly rotating $16 M_\odot$ core-collapse supernova progenitor. I will present key results of this work and discuss their implications on stellar evolution calculations as well as the subsequent supernova explosion.
