Modeling GW170817 based on numerical relativity and its implications

By M. Shibata, S. Fujibayashi, K. Hotokezaka, Kentaro Kiuchi, K. Kyutoku, Y. Sekiguchi, Masaomi Tanaka. 2017

287 citations recorded by the source corpus.

Gravitational-wave observation together with a large number of electromagnetic observations shows that the source of the latest gravitational-wave event, GW170817, detected primarily by advanced LIGO, is the merger of a binary neutron star. We attempt to interpret this observational event based on our results of numerical-relativity simulations performed so far paying particular attention to the optical and infra-red observations. We finally reach a conclusion that this event is described consistently by the presence of a long-lived hypermassive or supramassive neutron star as the merger remnant, because (i) significant contamination by lanthanide elements along our line of sight to this source can be avoided by the strong neutrino irradiation from it and (ii) it could play a crucial role to produce an ejecta component of appreciable mass with fast motion in the post-merger phase. We also point out that (I) the neutron-star equation of state has to be sufficiently stiff (i.e., the maximum mass of cold spherical neutron stars, M_max, has to be appreciably higher than 2M_sun in order that a long-lived massive neutron star can be formed as the merger remnant for the binary systems of GW170817, for which the initial total mass is >~ 2.73M_sun and (II) no detection of relativistic optical counterpart suggests a not-extremely high value of M_max approximately as 2.15-2.25M_sun.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/a82e67e7d65a7c8753cdd2f06f4e5864f629dadc

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Citations in the corpus

Origin of the heaviest elements: The rapid neutron-capture process (2019, background): “17 M (Margalit and Metzger, 2017; Shibata et al., 2017; Rezzolla et al., 2018; Ruiz et al., 2018) following the observation of GW170817.”
Long-term GRMHD simulations of neutron star merger accretion discs: implications for electromagnetic counterparts (2018, background): “Since most of the ejecta has Ye 0.25 with a mass-weighted velocity vr = 0.11c (Table 1), the disk outflow can easily generate a red kilonova component similar to that from GW170817.”
Mass Ejection from the Remnant of a Binary Neutron Star Merger: Viscous-radiation Hydrodynamics Study (2017, methodology): “We solve these equations in cylindrical coordinates as in Shibata et al. (2017b).”
Three-dimensional GRMHD Simulations of Neutrino-cooled Accretion Disks from Neutron Star Mergers (2017, background): “…ejecta mass ≈ 5 × 10−2M inferred for GW170817 exceeds the dynamical ejecta obtained by any general-relativistic (GR) NS–NS merger simulation to date (e.g. Shibata et al. 2017); the velocity v ≈ 0.1 c of the red KN is, furthermore, several times lower than that found by the numerical simulations.”
Using Gravitational-wave Observations and Quasi-universal Relations to Constrain the Maximum Mass of Neutron Stars (2017, methodology): “Second, our predictions are compatible with those recently presented by Shibata et al. (2017); Margalit & Metzger (2017), sharing a number of similar considerations with the latter.”
GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations (2017, methodology): “1~ (Shibata et al. 2017).”
A Magnetar Origin for the Kilonova Ejecta in GW170817 (2018, methodology): “While this process has been modeled as local “effective viscosity” (e.g., Radice et al. 2018; Shibata et al. 2017), angular momentum redistribution could in principle be dominated by torques from large-scale magnetic fields, even if they are weaker in magnitude than the smallerscale turbulent ones.”
Critical examination of constraints on the equation of state of dense matter obtained from GW170817 (2018, unknown): “5 1.8 2.0 2.2 2.4 2.6 2.8 3.0 Mmax [Msol] 100 200 300 400 500 600 700 Λ̃ ntr = 0.32fm −3 q = 1 q = 0.7 Margalit et al. (2017) Rezzolla et al. (2018) Shibata et al. (2017) Radice et al. (2018) FIG.”
Constraining the Dense Matter Equation of State with Joint Analysis of NICER and LIGO/Virgo Measurements (2019, result): “We find that the maximum mass distribution presented here is broadly consistent with values found in other works (see, e.g., Margalit & Metzger 2017; Shibata et al. 2017; Alsing et al. 2018; Rezzolla et al. 2018; Ruiz et al. 2018; Tews & Schwenk 2020).”