Dynamics and neutrino signal of black hole formation in non-rotating failed supernovae. II. progenitor dependence

TL;DR

This study investigates how different progenitor stars influence black hole formation and neutrino signals during stellar collapse, revealing that progenitor density profiles significantly affect the neutrino burst duration and characteristics.

Contribution

It demonstrates the progenitor dependence of black hole formation dynamics and neutrino signals using general relativistic simulations across multiple stellar models.

Findings

Black hole formation occurs within 0.4-1.5 seconds after core bounce.

Progenitor density profiles determine accretion rates and neutrino burst durations.

Neutrino burst features can potentially reveal progenitor properties.

Abstract

We study the progenitor dependence of the black hole formation and its associated neutrino signals from the gravitational collapse of non-rotating massive stars, following the preceding study on the single progenitor model in Sumiyoshi et al. (2007). We aim to clarify whether the dynamical evolution toward the black hole formation occurs in the same manner for different progenitors and to examine whether the characteristic of neutrino bursts is general having the short duration and the rapidly increasing average energies. We perform the numerical simulations by general relativistic neutrino-radiation hydrodynamics to follow the dynamical evolution from the collapse of pre-supernova models of 40Msun and 50Msun toward the black hole formation via contracting proto-neutron stars. For the three progenitor models studied in this paper, we found that the black hole formation occurs in ~0.4-1.5 s after core bounce through the increase of proto-neutron star mass together with the short and energetic neutrino burst. We found that density profile of progenitor is important to determine the accretion rate onto the proto-neutron star and, therefore, the duration of neutrino burst. We compare the neutrino bursts of black hole forming events from different progenitors and discuss whether we can probe clearly the progenitor and/or the dense matter.