THE FATE OF THE COMPACT REMNANT IN NEUTRON STAR MERGERS

Fryer, Chris L.; Belczynski, Krzysztoff; Ramirez-Ruiz, Enrico; Rosswog, Stephan; Shen, Gang; Steiner, Andrew W.

doi:10.1088/0004-637X/812/1/24

Title: THE FATE OF THE COMPACT REMNANT IN NEUTRON STAR MERGERS

Journal Article · Sat Oct 10 00:00:00 EDT 2015 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/812/1/24· OSTI ID:22518864

Fryer, Chris L. ^[1]; Belczynski, Krzysztoff ^[2]; Ramirez-Ruiz, Enrico ^[3]; Rosswog, Stephan ^[4]; Shen, Gang ^[5]; Steiner, Andrew W. ^[6]

Department of Physics, The University of Arizona, Tucson, AZ 85721 (United States)
Astronomical Observatory, University of Warsaw, Al Ujazdowskie 4, 00-478 Warsaw (Poland)
Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064 (United States)
The Oskar klein Center, Department of Astronomy, AlbaNova, Stockholm University, SE-106 91 Stockholm (Sweden)
Institute for Nuclear Theory, University of Washington, Seattle, WA 98195 (United States)
Department of Physics and Astronomy, University of Tennessee, Knoxville, TN 37996 (United States)

Neutron star (binary neutron star and neutron star–black hole) mergers are believed to produce short-duration gamma-ray bursts (GRBs). They are also believed to be the dominant source of gravitational waves to be detected by the advanced LIGO and advanced VIRGO and the dominant source of the heavy r-process elements in the universe. Whether or not these mergers produce short-duration GRBs depends sensitively on the fate of the core of the remnant (whether, and how quickly, it forms a black hole). In this paper, we combine the results of Newtonian merger calculations and equation of state studies to determine the fate of the cores of neutron star mergers. Using population studies, we can determine the distribution of these fates to compare to observations. We find that black hole cores form quickly only for equations of state that predict maximum non-rotating neutron star masses below 2.3–2.4 solar masses. If quick black hole formation is essential in producing GRBs, LIGO/Virgo observed rates compared to GRB rates could be used to constrain the equation of state for dense nuclear matter.

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OSTI ID:: 22518864

Journal Information:: Astrophysical Journal, Vol. 812, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X

Country of Publication:: United States

Language:: English

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Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A Abbott, B. P.; Abbott, R.; Abbott, T. D. Bristol : Institute of Physics Publishing https://doi.org/10.15488/2271	text	January 2017
On the Rate and on the Gravitational Wave Emission of Short and Long GRBs Ruffini, R.; Rodriguez, J.; Muccino, M. The Astrophysical Journal, Vol. 859, Issue 1 https://doi.org/10.3847/1538-4357/aabee4	journal	May 2018
Neutron-star Radius Constraints from GW170817 and Future Detections Bauswein, Andreas; Just, Oliver; Janka, Hans-Thomas The Astrophysical Journal, Vol. 850, Issue 2 https://doi.org/10.3847/2041-8213/aa9994	journal	November 2017
Equations of state for supernovae and compact stars Micaela, Oertel,; Matthias, Hempel,; Thomas, Klähn, American Physical Society https://doi.org/10.5451/unibas-ep58112	text	January 2017
Questions Related to the Equation of State of High-Density Matter Miller, M. Coleman Universe, Vol. 5, Issue 5 https://doi.org/10.3390/universe5050100	journal	April 2019
Compact Binary Merger Rates: Comparison with LIGO/Virgo Upper Limits Belczynski, Krzysztof; Repetto, Serena; Holz, Daniel E. arXiv https://doi.org/10.48550/arxiv.1510.04615	text	January 2015
On the rate and on the gravitational wave emission of short and long GRBs Ruffini, R.; Rodriguez, J.; Muccino, M. arXiv https://doi.org/10.48550/arxiv.1602.03545	text	January 2016
Bounds on the speed of sound in dense matter, and neutron star structure Moustakidis, Ch. C.; Gaitanos, T.; Margaritis, Ch. arXiv https://doi.org/10.48550/arxiv.1608.00344	text	January 2016
The Properties of Short gamma-ray burst Jets Triggered by neutron star mergers Murguia-Berthier, Ariadna; Ramirez-Ruiz, Enrico; Montes, Gabriela arXiv https://doi.org/10.48550/arxiv.1609.04828	text	January 2016
Semi-analytic derivation of the threshold mass for prompt collapse in binary neutron star mergers Bauswein, Andreas; Stergioulas, Nikolaos arXiv https://doi.org/10.48550/arxiv.1702.02567	text	January 2017
Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers Wollaeger, Ryan T.; Korobkin, Oleg; Fontes, Christopher J. arXiv https://doi.org/10.48550/arxiv.1705.07084	text	January 2017
Evidence for a maximum mass cut-off in the neutron star mass distribution and constraints on the equation of state Alsing, Justin; Silva, Hector O.; Berti, Emanuele arXiv https://doi.org/10.48550/arxiv.1709.07889	text	January 2017
Constraining the Maximum Mass of Neutron Stars From Multi-Messenger Observations of GW170817 Margalit, Ben; Metzger, Brian arXiv https://doi.org/10.48550/arxiv.1710.05938	text	January 2017
Neutron-star radius constraints from GW170817 and future detections Bauswein, Andreas; Just, Oliver; Janka, Hans-Thomas arXiv https://doi.org/10.48550/arxiv.1710.06843	text	January 2017
GW170817 and the prospect of forming supramassive remnants in neutron star mergers Ma, Peng-Xiong; Jiang, Jin-Liang; Wang, Hao arXiv https://doi.org/10.48550/arxiv.1711.05565	text	January 2017
Nuclear Equation of state for Compact Stars and Supernovae Burgio, G. Fiorella; Fantina, Anthea F. arXiv https://doi.org/10.48550/arxiv.1804.03020	text	January 2018
The Multi-Messenger Matrix: the Future of Neutron Star Merger Constraints on the Nuclear Equation of State Margalit, Ben; Metzger, Brian D. arXiv https://doi.org/10.48550/arxiv.1904.11995	text	January 2019
Relation between gravitational mass and baryonic mass for non-rotating and rapidly rotating neutron stars Gao, He; Ai, Shun-Ke; Cao, Zhou-Jian arXiv https://doi.org/10.48550/arxiv.1905.03784	preprint	January 2019

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Title: THE FATE OF THE COMPACT REMNANT IN NEUTRON STAR MERGERS

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