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

TL;DR

This paper presents a simple, parameterized model to simulate mass ejection in failed core-collapse supernovae, exploring how progenitor and dense matter properties influence ejecta characteristics.

Contribution

It introduces a novel, adaptable model for PNS evolution and neutrino emission in failed CCSNe, enabling extensive simulation across diverse progenitors and EOS assumptions.

Findings

Mass ejection varies with progenitor properties and EOS.

Ejecta energy and mass depend on PNS collapse timing.

Model can help interpret future failed CCSN observations.

Abstract

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. Our model allows us to study mass ejection of failed CCSNe where the PNS collapses into a BH within $\sim100\,{\rm ms}$ and up to $\sim10^6\,{\rm s}$. We perform failed CCSNe simulations for 262 different pre-SN progenitors and determine how the energy and mass of the ejecta depend on progenitor properties and the equation of state (EOS) of dense matter. In the case of a future failed CCSN observation, the trends obtained in our simulations can be used to place constraints on the pre-SN progenitor characteristics, the EOS, and on PNS properties at BH formation time.