Modeling GW170817 based on numerical relativity and its implications

Abstract

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.

21 pages, 6 figures, accepted for publication in Phys. Rev. D

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• Towards Understanding Astrophysical Effects of Nuclear Symmetry Energy
• Full Transport Model of GW170817-Like Disk Produces a Blue Kilonova
• A General-relativistic Determination of the Threshold Mass to Prompt Collapse in Binary Neutron Star Mergers
• Revisiting the lower bound on tidal deformability derived by AT 2017gfo
• First 100 ms of a long-lived magnetized neutron star formed in a binary neutron star merger
• When Did the Remnant of GW170817 Collapse to a Black Hole?
• Capture of Leptophilic Dark Matter in Neutron Stars
• Confronting gravitational-wave observations with modern nuclear physics constraints
• Implications of the mass $M=2.17_{-0.10}^{+0.11}$M${}_{\odot }$ of PSR~J0740+6620 on the Equation of State of Super-Dense Neutron-Rich Nuclear Matter
• Extended calculations of energy levels and transition rates of Nd II-IV ions for application to neutron star mergers
• Effects of spin on magnetized binary neutron star mergers and jet launching
• Comparing treatments of weak reactions with nuclei in simulations of core-collapse supernovae
• Propagation of a Short GRB Jet in the Ejecta: Jet Launching Delay Time, Jet Structure, and GW170817/GRB 170817A
• Revisiting the maximum mass of differentially rotating neutron stars in general relativity: Übermassive stars with realistic equations of state
• Hyperonic Neutron Star Matter in Light of GW170817
• Diagnosing the remnants of binary neutron star merger from GW170817/GRB170817A event
• Maximum Mass Of Differentially Rotating Strange Quark Stars
• Suitable resolution for EOS tables in neutron star investigation
• High-energy emissions from neutron star mergers
• Constraints from the GW170817 merger event on the nuclear matter equation of state
• Constraints on the Neutron Star Equation of State from GW170817