Remnant massive neutron stars of binary neutron star mergers: Evolution process and gravitational waveform

By K. Hotokezaka, Kentaro Kiuchi, K. Kyutoku, Takayuki Muranushi, Y. Sekiguchi, M. Shibata, K. Taniguchi. 2013

175 citations recorded by the source corpus.

Massive (hypermassive and supramassive) neutron stars are likely to be often formed after the merger of binary neutron stars. We explore the evolution process of the remnant massive neutron stars and gravitational waves emitted by them, based on numerical-relativity simulations for binary neutron star mergers employing a variety of equations of state and choosing a plausible range of the neutron-star mass of binaries. We show that the lifetime of remnant hypermassive neutron stars depends strongly on the total binary mass and also on the equations of state. Gravitational waves emitted by the remnant massive neutron stars universally have a quasiperiodic nature of an approximately constant frequency although the frequency varies with time. We also show that the frequency and time-variation feature of gravitational waves depend strongly on the equations of state. We derive a fitting formula for the quasiperiodic gravitational waveforms, which may be used for the data analysis of a gravitational-wave signal.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/40cc4adc9ed69ebe6b5ae552d806a4a5d1ba858b

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Citations in the corpus

Europium production: neutron star mergers versus core-collapse supernovae (2013, background): “A number of recent studies (Oechslin, Janka & Marek 2007; Rosswog 2013, Bauswein et al. 2013; Hotokezaka et al. 2013; Kyutoku et al. 2013) find a spread of ejecta masses in this range with the exact numbers, around the value of10−2, depending on the binary mass ratio, and to some extent on the…”
NEUTRINO-DRIVEN WINDS IN THE AFTERMATH OF A NEUTRON STAR MERGER: NUCLEOSYNTHESIS AND ELECTROMAGNETIC TRANSIENTS (2015, background): “…to as dynamic ejecta, has long been recognized as the likely source of the heaviest r-process nuclei (Freiburghaus et al. 1999b; Rosswog et al. 1999; Roberts et al. 2011; Goriely et al. 2011; Korobkin et al. 2012; Bauswein et al. 2013; Hotokezaka et al. 2013; Rosswog 2013; Rosswog et al. 2014).”
Neutrino-driven winds from neutron star merger remnants (2014, background): “Because of the geometry of the emission, it is also supposed to be important in optically thin conditions (see e.g. Janka 1991; Burrows, Reddy & Thompson 2006).”
Three-dimensional GRMHD Simulations of Neutrino-cooled Accretion Disks from Neutron Star Mergers (2017, background): “The torus mass found from numerical simulations can be as high as ≈ 0.1− 0.2M in an NS–NS merger if the merger remnant goes through a hypermassive neutron star (HMNS) phase1 prior to forming a BH (e.g. Shibata & Taniguchi 2006; Hotokezaka et al. 2013a).”
The birth of black holes: neutron star collapse times, gamma-ray bursts and fast radio bursts (2014, background): “…where N(μBNS, σ BNS) specifies a normal distribution with mean μBNS and standard deviation σ BNS. Binary NS mergers are believed to approximately conserve rest mass (Mrest), with 0.01 M of material ejected during the merger (Rezzolla et al. 2011; Giacomazzo & Perna 2013; Hotokezaka et al. 2013).”
Mass Ejection from the Remnant of a Binary Neutron Star Merger: Viscous-radiation Hydrodynamics Study (2017, background): “First, during the merger, the dynamical mass ejection occurs(e.g., Hotokezaka et al. 2013b; Sekiguchi et al. 2015, 2016).”
Red or blue? A potential kilonova imprint of the delay until black hole formation following a neutron star merger (2014, background): “For particularly nearby mergers, oscillations excited in the HMNS may be detectable in the GW strain data (Shibata 2005; Bauswein et al. 2012; Hotokezaka et al. 2013b).”
Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis (2018, methodology): “In comparison to previous studies (Oechslin et al. 2007; Hotokezaka et al. 2013b, as reported in Wu et al. 2016) we find that disk winds and viscous outflows should contribute a significantly larger fraction of the overall ejecta.”