Progenitor Dependence of Hadron-quark Phase Transition in Failing Core-collapse Supernovae

TL;DR

This study investigates how a hadron-quark phase transition influences the dynamics of failing core-collapse supernovae, revealing progenitor-dependent collapse behaviors and potential neutrino signals indicative of the phase transition.

Contribution

It introduces a comprehensive simulation analysis of the hadron-quark phase transition effects across multiple progenitors, highlighting progenitor dependence and observable neutrino signatures.

Findings

Phase transition causes a second collapse in certain progenitors.

Neutrino signals with ms-period oscillations can indicate the phase transition.

No shock revival; black hole formation is inevitable in these models.

Abstract

We study the consequences of a hadron-quark phase transition (PT) in failing core-collapse supernovae (CCSNe) which give birth to stellar-mass black holes (BH). We perform a suite of neutrino-transport general-relativistic hydrodynamic simulations in spherical symmetry with 21 progenitor models and a hybrid equation of state (EoS) including hadrons and quarks. We find that the effect of the PT on the CCSN postbounce dynamics is a function of the bounce compactness parameter $\xi_{2.2}$. For $\xi_{2.2}\gtrsim0.24$, the PT leads to a second dynamical collapse of the protocompact star (PCS). While BH formation starts immediately after this second collapse for models with $\xi_{2.2}\gtrsim0.51$, the PCS experiences a second bounce and oscillations for models with $0.24\lesssim\xi_{2.2}\lesssim0.51$. These models emit potent oscillatory neutrino signals with a period of $\sim$ms for tens of ms after the second bounce, which can be a strong indicator of the PT in failing CCSNe if detected in the future. However, no shock revival occurs and BH formation inevitably takes place in our spherically-symmetric simulations. Furthermore, via a diagram of mass-specific entropy evolution of the PCS, the progenitor dependence can be understood through the appearance of third-family of compact stars emerging at large entropy induced by the PT.