Merger of binary neutron stars to a black hole: Disk mass, short gamma-ray bursts, and quasinormal mode ringing

By M. Shibata, K. Taniguchi. 2006

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Three-dimensional simulations for the merger of binary neutron stars are performed in the framework of full general relativity. We pay particular attention to the black hole formation case and to the resulting mass of the surrounding disk for exploring the possibility for formation of the central engine of short-duration gamma-ray bursts (SGRBs). Hybrid equations of state are adopted mimicking realistic, stiff nuclear equations of state (EOSs), for which the maximum allowed gravitational mass of cold and spherical neutron stars, M{sub sph}, is larger than 2M{sub {center_dot}}. Such stiff EOSs are adopted motivated by the recent possible discovery of a heavy neutron star of mass {approx}2.1{+-}0.2M{sub {center_dot}}. For the simulations, we focus on binary neutron stars of the ADM mass M > or approx. 2.6M{sub {center_dot}}. For an ADM mass larger than the threshold mass M{sub thr}, the merger results in prompt formation of a black hole irrespective of the mass ratio Q{sub M} with 0.65 or approx. 0.01M{sub {center_dot}} irrespective of Q{sub M}. Gravitational waves are computed in terms of a gauge-invariant wave extraction technique. In the formation of the hypermassive neutron star, quasiperiodic gravitational waves of frequency between 3 and 3.5 kHz are emitted irrespective of EOSs. The effective amplitude of gravitational waves can be > or approx. 5x10{sup -21} at a distance of 50 Mpc, and hence, it may be detected by advanced laser-interferometers. For the black hole formation case, the black hole excision technique enables a long-term computation and extraction of ring-down gravitational waves associated with a black hole quasinormal mode. It is found that the frequency and amplitude are {approx_equal}6.5-7 kHz and {approx}10{sup -22} at a distance of 50 Mpc for the binary of mass M{approx_equal}2.7-2.9M{sub {center_dot}}.« less

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/1e8b38530beeb49bb3b49139ecdf618805545636

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Citations in the corpus

The Einstein Toolkit: a community computational infrastructure for relativistic astrophysics (2011, background): “The first fully general relativistic (GR) simulations of merging NS–NS binaries were reported in 1999, with further advances over the next few years [1–5].”
Short-hard gamma-ray bursts (2007, methodology): “In the simulation by Shibata & Taniguchi (2006), GW radiation is one of the main channels through which the central object loses angular momentum and ultimately collapses.”
Time-dependent models of accretion discs formed from compact object mergers (2008, background): “However, simulations show that when (and if) collapse actually occurs depends on the mass of the central NS and its ability to transport angular momentum to the surrounding disk (Shibata et al. 2005; Shibata & Taniguchi 2006; Shibata et al. 2006).”
THE MISSING LINK: MERGING NEUTRON STARS NATURALLY PRODUCE JET-LIKE STRUCTURES AND CAN POWER SHORT GAMMA-RAY BURSTS (2011, background): “…have made it possible to compute the full evolution, from large binaryseparations up to black-hole (BH) formation, without and with magnetic fields (Shibata & Taniguchi 2006; Baiotti et al. 2008; Anderson et al. 2008; Liu et al. 2008; Giacomazzo et al. 2009, 2011), and with idealized or realistic…”
Cosmological Fast Radio Bursts from Binary Neutron Star Mergers (2013, background): “This is possible if short GRBs are strongly beamed, and/or they are produced by rarer events such as large mass ratio binaries, mergers resultingin a hypermassive neutron star (HMNS) supported by rotation, or NS-BH/BH-BH mergers (Shibata & Taniguchi 2006; Faber & Rasio 2012).”
Gravitational waves and non-axisymmetric oscillation modes in mergers of compact object binaries (2011, methodology): “…distinguishable in the GW signal and could be used for characterizing the hypermassive compact object (Zhuge et al. 1994; Oechslin et al. 2002; Shibata & Uryū2002; Shibata et al. 2005; Shibata & Taniguchi 2006; Oechslin & Janka 2007; Baiotti et al. 2008; Kiuchi et al. 2009; Bauswein et al.2010).”
Production of the entire range of r-process nuclides by black hole accretion disc outflows from neutron star mergers (2016, background): “A relatively massive disc (∼ 0.1M ) can be formed following a NS–NS merger, as part of the process by which the HMNS sheds angular momentum outwards prior to collapsing into a BH (e.g. Shibata & Taniguchi 2006).”
Properties of the Binary Neutron Star Merger GW170817 (2018, background): “Soft EOSs and large masses result in the prompt formation of a black hole immediately after the merger [144].”
A Magnetar Origin for the Kilonova Ejecta in GW170817 (2018, background): “…& Metzger 2017; Perego et al. 2017; Rezzolla et al. 2017; Ruiz et al. 2018), then the formation of a torus generically results from the outward transport of angular momentum, which removes centrifugal support and results in the collapse of the HMNS to a black hole (e.g., Shibata & Taniguchi 2006).”
Short GRBs with Extended Emission from Magnetar Birth: Jet Formation and Collimation (2011, background): “…binary could also leave a stable NS remnant, provided that either (1) the total mass of the binary is low and/or the NS equation of state is stiff (Shibata & Taniguchi 2006); (2) the proto-NS forms in a meta-stable state supported by differential rotation (Baumgarte, Shapiro & Shibata 2000;…”
Long-term GRMHD simulations of neutron star merger accretion discs: implications for electromagnetic counterparts (2018, background): “This requires the mass of the remnant to exceed a certain threshold that depends on the dense matter EOS (e.g., Shibata & Taniguchi 2006).”