Equation of State and Progenitor Dependence of Stellar-mass Black Hole Formation

Schneider, André da Silva; O’Connor, Evan; Granqvist, Elvira; Betranhandy, Aurore; Couch, Sean M.

doi:10.3847/1538-4357/ab8308

Cited by 56 publications

(31 citation statements)

References 131 publications

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“…Recent systematic studies in spherical symmetry have explored the dependencies of various progenitor models and nuclear equations of state (EOSs) on the explodability and the remnant properties such as newly born BH masses (e.g. O'Connor & Ott 2011; Ugliano et al 2012;Sukhbold et al 2016;Ebinger et al 2019;da Silva Schneider et al 2020;Warren et al 2020). Pan et al (2018) performed two-dimensional (2D) axisymmetric core-collapse simulations for a BH-forming progenitor with various EOSs to investigate the impacts of EOSs on the BH formation as well as on the GW and neutrino emission.…”

Section: Introductionmentioning

confidence: 99%

Characteristic time variability of gravitational-wave and neutrino signals from three-dimensional simulations of non-rotating and rapidly rotating stellar core collapse

Shibagaki

Kuroda

Kotake

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present results from full general relativistic three-dimensional hydrodynamics simulations of stellar core collapse of a 70 M⊙ star with spectral neutrino transport. To investigate the impact of rotation on non-axisymmetric instabilities, we compute three models by parametrically changing the initial strength of rotation. The most rapidly rotating model exhibits a transient development of the low-T/|W| instability with one-armed spiral flow at the early postbounce phase. Subsequently, the two-armed spiral flow appears, which persists during the simulation time. The moderately rotating model also shows the growth of the low-T/|W| instability, but only with the two-armed spiral flow. In the nonrotating model, a vigorous activity of the standing accretion-shock instability (SASI) is only observed. The SASI is first dominated by the sloshing mode, which is followed by the spiral SASI until the black hole formation. We present a spectrogram analysis of the gravitational waves (GWs) and neutrinos, focusing on the time correlation. Our results show that characteristic time modulations in the GW and neutrino signals can be linked to the growth of the non-axisymmetric instabilities. We find that the degree of the protoneutron star (PNS) deformation, depending upon which modes of the non-axisymmetric instabilities develop, predominantly affects the characteristic frequencies of the correlated GW and neutrino signals. We point out that these signals would be simultaneously detectable by the current-generation detectors up to ∼10 kpc. Our findings suggest that the joint observation of GWs and neutrinos is indispensable for extracting information on the PNS evolution preceding the black hole formation.

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Section: Introductionmentioning

confidence: 99%

Characteristic time variability of gravitational-wave and neutrino signals from three-dimensional simulations of non-rotating and rapidly rotating stellar core collapse

Shibagaki

Kuroda

Kotake

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…One such scenario arises in the core-collapse supernova and proto-neutron star context, where a hot proto-neutron star is formed during the contraction of the supernova progenitor and subsequent gravitational detachment of the remnant from the expanding ejecta [1][2][3][4][5][6][7]. A related scenario arises in the case of stellar black-hole formation when the progenitor mass is so large (typically tens of solar masses) that the formation of a stable compact object is not possible and a black hole is inevitably formed [8][9][10][11]. Finally, the binary neutron star mergers offer yet another scenario where finite temperature nuclear and hypernuclear matter play an important role [12][13][14][15].…”

Section: Introductionmentioning

confidence: 99%

Equation of State and Composition of Proto-Neutron Stars and Merger Remnants with Hyperons

Sedrakian

Harutyunyan

2021

Universe

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Finite-temperature equation of state (EoS) and the composition of dense nuclear and hypernuclear matter under conditions characteristic of neutron star binary merger remnants and supernovas are discussed. We consider both neutrino free-streaming and trapped regimes which are separated by a temperature of a few MeV. The formalism is based on covariant density functional (CDF) theory for the full baryon octet with density-dependent couplings, suitably adjusted in the hypernuclear sector. The softening of the EoS with the introduction of the hyperons is quantified under various conditions of lepton fractions and temperatures. We find that Λ, Ξ−, and Ξ0 hyperons appear in the given order with a sharp density increase at zero temperature at the threshold being replaced by an extended increment over a wide density range at high temperatures. The Λ hyperon survives in the deep subnuclear regime. The triplet of Σs is suppressed in cold hypernuclear matter up to around seven times the nuclear saturation density, but appears in significant fractions at higher temperatures, T≥20 MeV, in both supernova and merger remnant matter. We point out that a special isospin degeneracy point exists where the baryon abundances within each of the three isospin multiplets are equal to each other as a result of (approximate) isospin symmetry. At that point, the charge chemical potential of the system vanishes. We find that under the merger remnant conditions, the fractions of electron and μ-on neutrinos are close and are about 1%, whereas in the supernova case, we only find a significant fraction (∼10%) of electron neutrinos, given that in this case, the μ-on lepton number is zero.

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“…The death of a massive star can give birth to a stellar-mass black hole (BH) if it fails to explode as a core-collapse supernova (CCSN) (Sumiyoshi et al 2006;O'Connor & Ott 2011). The process of this BH formation channel has been studied with neutrino-transport hydrodynamic simulations in great detail (Sumiyoshi et al 2007;O'Connor & Ott 2011;Kuroda et al 2018;Pan et al 2020;Walk et al 2020;Schneider et al 2020). As in a successful CCSN, the collapse of the progenitor's iron core produces a protocompact star (PCS) which rebounds due to the stiffening of the nuclear matter equation of state (EoS) just above nuclear saturation density (ρ sat 2.7×10 14 g cm −3 ) (Burrows & Vartanyan 2021).…”

Section: Introductionmentioning

confidence: 99%

“…However, in a failing CCSN, shock revival does not arise to unbind the stellar envelope. Thus, the PCS continu-ously grows through accretion and inevitably collapses into a BH once its mass exceeds the maximum compact star mass allowed by the EoS (Schneider et al 2020).…”

Section: Introductionmentioning

confidence: 99%

“…This property is believed to be important for the shock revival after the PT-induced collapse in CCSNe (Hempel et al 2016). From the CCSN side, it is known that the specific entropy of the PCS is related to the progenitor compactness and impacts the BH formation process (Schneider et al 2020). Therefore, the effect of the PT can be progenitor dependent and this has not been systematically studied before.…”

Section: Introductionmentioning

confidence: 99%

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

Zha,

O'Connor,

Schneider

2021

Preprint

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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 neutrinotransport 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 ξ 2.2 . For ξ 2.2 0.24, 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 ξ 2.2 0.51, the PCS experiences a second bounce and oscillations for models with 0.24 ξ 2.2 0.51. These models emit potent oscillatory neutrino signals with a period of ∼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.

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Equation of State and Progenitor Dependence of Stellar-mass Black Hole Formation

Cited by 56 publications

References 131 publications

Characteristic time variability of gravitational-wave and neutrino signals from three-dimensional simulations of non-rotating and rapidly rotating stellar core collapse

Characteristic time variability of gravitational-wave and neutrino signals from three-dimensional simulations of non-rotating and rapidly rotating stellar core collapse

Equation of State and Composition of Proto-Neutron Stars and Merger Remnants with Hyperons

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

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