A Parameterized Neutrino Emission Model to Study Mass Ejection in Failed Core-collapse Supernovae

Understand

Some massive stars end their lives as \textit{failed} core-collapse supernovae (CCSNe) and become black holes (BHs).

• Although in this class of phenomena the stalled supernova shock is not revived, the outer stellar envelope can still be partially ejected.
• This occurs because the hydrodynamic equilibrium of the star is disrupted by the gravitational mass loss of the protoneutron star (PNS) due to neutrino emission.
• We develop a simple model that emulates PNS evolution and its neutrino emission and use it to simulate failed CCSNe in spherical symmetry for a wide range of progenitor stars.