Speaker
Description
Recent advancements in core-collapse supernova modeling are revealing a new black hole (BH) formation channel in which a BH forms within about a second of shock revival yet still results in a successful supernova. The limited body of literature on these black hole supernovae (BHSNe) has mostly focused on highly massive, compact progenitors. I will present a sample of ~40 stars between 19 and 75 solar masses, evolved in two dimensions from core-collapse to hours after BH formation. We find a remarkably wide occurrence of BHSN outcomes and characterize the properties of their explosions and BH remnants. We demonstrate the impact of uncertainty in the nuclear equation of state on these properties as well as on the composition of the ejecta that escape the BH. Building on these 2D results, I will present a 3D BHSN simulation of a 39 solar mass progenitor.
