We study the consequences of a hadron-quark phase transition (PT) in failing core-collapse supernovae (CCSNe) that 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 . For , 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 , the PCS experiences a second bounce and oscillations for models with . These models emit potent oscillatory neutrino signals with a period of ∼1 ms for tens of milliseconds 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 a third family of compact stars emerging at large entropy induced by the PT.

我们研究了产生恒星质量黑洞 (BH) 的核坍缩超新星 (CCSNe) 中的强子-夸克相变 (PT) 的后果。我们使用 21 个前体模型和包括强子和夸克的混合状态方程 (EoS) 进行了一套球对称中微子传输广义相对论流体动力学模拟。我们发现 PT 对 CCSN 后弹跳动力学的影响是弹跳紧凑性参数的函数。对于，PT 导致原致密星 (PCS) 的第二次动态坍缩。对于具有 的模型，在第二次崩溃后立即开始 BH 形成，而对于具有 的模型，PCS 会经历第二次反弹和振荡. 这些模型在第二次反弹后的几十毫秒内发出周期为 1 ms 的强振荡中微子信号，如果将来检测到，这可以成为 PT 失败 CCSNe 的有力指标。然而，在我们的球对称模拟中，没有发生激波复活并且不可避免地会发生 BH 形成。此外，通过 PCS 的质量特定熵演化图，可以通过在 PT 引起的大熵下出现的第三类致密星的出现来理解祖细胞依赖性。