Systematics of prompt black-hole formation in neutron star mergers

Bauswein, Andreas; Blacker, Sebastian; Lioutas, Georgios; Soultanis, Theodoros; Vijayan, Vimal; Stergioulas, Nikolaos

doi:10.1103/physrevd.103.123004

Cited by 56 publications

(55 citation statements)

References 126 publications

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“…considering the minimum lapse function is a monotonous decrease of α min [16], cf. middle panel in Fig.…”

Section: B Threshold Mass To Prompt Collapsementioning

confidence: 99%

“…Agathos et al [15] used another set of NR simulations and derived estimates that were based on the tidal deformabilities so that the inspiral GW signal could be connected directly to the measured GW signal. 2 Finally, Bauswein et al [16] presented the first promptcollapse study, in which a mass ratio dependent threshold (up to a mass ratio of q ∼ 1.4) was derived. Very recently, Perego et al [17] also investigated the effect of the massratio on the prompt collapse threshold for non-spinning configurations.…”

Section: Introductionmentioning

confidence: 99%

“…While performing a systematic and detailed variation of the total mass and the mass ratio of the systems, we restrict our study to 3 EOSs, namely ALF2, SLy, and H4. For an investigation focusing on a larger set of EOSs, we refer the interested reader to [16].…”

Section: Introductionmentioning

confidence: 99%

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Investigating the mass-ratio dependence of the prompt-collapse threshold with numerical-relativity simulations

Kölsch,

Dietrich,

Ujevic

et al. 2021

Preprint

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The next observing runs of advanced gravitational-wave detectors will lead to a variety of binary neutron star detections and numerous possibilities for multi-messenger observations of binary neutron star systems. In this context a clear understanding of the merger process and the possibility of prompt black hole formation after merger is important, as the amount of ejected material strongly depends on the merger dynamics. These dynamics are primarily affected by the total mass of the binary, however, the mass ratio also influences the postmerger evolution. To determine the effect of the mass ratio, we investigate the parameter space around the prompt-collapse threshold with a new set of fully relativistic simulations. The simulations cover three equations of state and seven mass ratios in the range of 1.0 ≤ q ≤ 1.75, with five to seven simulations of binary systems of different total mass in each case. The threshold mass is determined through an empirical relation based on the collapse-time, which allows us to investigate effects of the mass-ratio on the threshold mass and also on the properties of the remnant system. Furthermore, we model effects of mass ratio and equation of state on tidal parameters of threshold configurations. 1 For more details, we refer the interested reader to the review article of Bernuzzi [11]. 2 Agathos et al. [15] predict a 10% change that GW170817 led to a prompt-collapse, while GW190425 produced, with a probability of 96%, a BH right after merger [3].

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“…considering the minimum lapse function is a monotonous decrease of α min [16], cf. middle panel in Fig.…”

Section: B Threshold Mass To Prompt Collapsementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Investigating the mass-ratio dependence of the prompt-collapse threshold with numerical-relativity simulations

Kölsch,

Dietrich,

Ujevic

et al. 2021

Preprint

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“…It was shown, for example, that the threshold mass for PC, M th , normalized to M TOV max , linearly correlates with the maximum compactness, defined as C TOV max ≡ GM TOV max /(R TOV max c 2 ), where c and G are the speed of light and the gravitational constant, respectively, as well as with other NS equilibrium properties. More recently, some extensions to asymmetric BNS mergers have been carried out, even if the results and their interpretation are more uncertain [38,41,42].…”

mentioning

confidence: 99%

“…With the exception of the DD2qG EOS, for which n max ∼ 0.8 − 1.2n TOV max , for the heaviest non-PC BNS we observe n max ∼ 0.75 − 0.95n TOV max at the first remnant bounce, with larger values usually associated to q ∼ 1. Two opposite effects influence the evolution of n max with respect to q [41]. On the one hand, for a given M , binaries with smaller q's have smaller orbital angular momentum and the NS cores are more prone to fuse (and thus to increase n max toward n TOV max ) due to the smaller rotational support.…”

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confidence: 99%

Probing the incompressibility of nuclear matter at ultra-high density through the prompt collapse of asymmetric neutron star binaries

Perego,

Logoteta,

Radice

et al. 2021

Preprint

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Using 250 neutron star merger simulations with microphysics, we explore for the first time the role of nuclear incompressibility in the prompt collapse threshold for binaries with different mass ratios. We demonstrate that observations of prompt collapse thresholds, either from binaries with two different mass ratios or with one mass ratio but combined with the knowledge of the maximum neutron star mass or compactness, will constrain the incompressibility at the maximum neutron star density, Kmax to within tens of percent. This, otherwise inaccessible, measure of Kmax can potentially reveal the presence of hyperons or quarks inside neutron stars.

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Dynamics and Equation of State Dependencies of Relevance for Nucleosynthesis in Supernovae and Neutron Star Mergers

Janka

Bauswein

2022

Handbook of Nuclear Physics

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Systematics of prompt black-hole formation in neutron star mergers

Cited by 56 publications

References 126 publications

Investigating the mass-ratio dependence of the prompt-collapse threshold with numerical-relativity simulations

Investigating the mass-ratio dependence of the prompt-collapse threshold with numerical-relativity simulations

Probing the incompressibility of nuclear matter at ultra-high density through the prompt collapse of asymmetric neutron star binaries

Dynamics and Equation of State Dependencies of Relevance for Nucleosynthesis in Supernovae and Neutron Star Mergers

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