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Black Hole Formation in Failing Core-Collapse Supernovae
Abstract
Massive stars ( M > 8-10 solar masses) end their lives with the gravitationally-induced collapse of their iron core. While it is likely that most of these events result in a successful core-collapse supernova, some my fail altogether (so called ‘unnovae’) when the protoneutron star in the core exceeds its maximum mass and collapses to a black hole.
In an effort to better understand these failed core-collapse supernovae, we performed a systematic study of black formation in failing core-collapse supernovae. Using a spherically-symmetric, general-relativistic hydrodynamics code and over 100 presupernova models. We study the effects of the choice of nuclear equation of state, zero-age main sequence (ZAMS) mass and metallicity, rotation, and mass loss prescription on BH formation. I will present the results of this study, including a prediction on the percentage of failed core-collapse supernovae and the suggestion that nonaxisymmetric rotational instabilities will limit the birth spin of nascent black holes.