TY - JOUR
T1 - Gravitational-wave luminosity of binary neutron stars mergers
AU - Zappa, Francesco
AU - Bernuzzi, Sebastiano
AU - Radice, David
AU - Perego, Albino
AU - Dietrich, Tim
N1 - Funding Information:
We thank A. Nagar for comments. S. B. acknowledges support by the EU H2020 under ERC Starting Grant No. BinGraSp-714626. T. D. acknowledges support by the European Unions Horizon 2020 research and innovation program under grant agreement No. 749145, BNSmergers. D. R. acknowledges support from a Frank and Peggy Taplin Membership at the Institute for Advanced Study and the Max-Planck/Princeton Center (MPPC) for Plasma Physics (NSF PHY-1523261). A. P. acknowledges support from the INFN initiative “High Performance data Network” funded by CIPE. Computations were performed on the supercomputer SuperMUC at the LRZ (Munich) under the project No. pr48pu, on the supercomputers Bridges, Comet, and Stampede (NSF XSEDE allocation TG-PHY160025), on NSF/NCSA Blue Waters (NSF PRAC ACI-1440083), and on Marconi at CINECA (PRACE proposal 2016153522 and ISCRA-B Project No. HP10B2PL6K).
Publisher Copyright:
© 2018 American Physical Society.
PY - 2018
Y1 - 2018
N2 - We study the gravitational-wave peak luminosity and radiated energy of quasicircular neutron star mergers using a large sample of numerical relativity simulations with different binary parameters and input physics. The peak luminosity for all the binaries can be described in terms of the mass ratio and of the leading-order post-Newtonian tidal parameter solely. The mergers resulting in a prompt collapse to black hole have the largest peak luminosities. However, the largest amount of energy per unit mass is radiated by mergers that produce a hypermassive neutron star or a massive neutron star remnant. We quantify the gravitational-wave luminosity of binary neutron star merger events, and set upper limits on the radiated energy and the remnant angular momentum from these events. We find that there is an empirical universal relation connecting the total gravitational radiation and the angular momentum of the remnant. Our results constrain the final spin of the remnant black hole and also indicate that stable neutron star remnant forms with super-Keplerian angular momentum.
AB - We study the gravitational-wave peak luminosity and radiated energy of quasicircular neutron star mergers using a large sample of numerical relativity simulations with different binary parameters and input physics. The peak luminosity for all the binaries can be described in terms of the mass ratio and of the leading-order post-Newtonian tidal parameter solely. The mergers resulting in a prompt collapse to black hole have the largest peak luminosities. However, the largest amount of energy per unit mass is radiated by mergers that produce a hypermassive neutron star or a massive neutron star remnant. We quantify the gravitational-wave luminosity of binary neutron star merger events, and set upper limits on the radiated energy and the remnant angular momentum from these events. We find that there is an empirical universal relation connecting the total gravitational radiation and the angular momentum of the remnant. Our results constrain the final spin of the remnant black hole and also indicate that stable neutron star remnant forms with super-Keplerian angular momentum.
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U2 - 10.1103/PhysRevLett.120.111101
DO - 10.1103/PhysRevLett.120.111101
M3 - Article
C2 - 29601774
AN - SCOPUS:85044124595
VL - 120
JO - Physical Review Letters
JF - Physical Review Letters
SN - 0031-9007
IS - 11
M1 - 111101
ER -