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Gravitational-wave luminosity of binary neutron stars mergers

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arxiv 1712.04267 v1 pith:XWXKSZEY submitted 2017-12-12 gr-qc astro-ph.HE

Gravitational-wave luminosity of binary neutron stars mergers

Francesco Zappa , Sebastiano Bernuzzi , David Radice , Albino Perego , Tim Dietrich This is my paper
classification gr-qc astro-ph.HE
keywords neutronremnantstarluminositymergersangularbinaryenergy
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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 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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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Short GRB 090510: a magnetized neutron star binary merger leading to a black hole

    astro-ph.HE 2025-09 conditional novelty 6.0

    GRB 090510 is modeled as a merger of two ~1.2 solar mass neutron stars that forms a spinning 2.36 solar mass black hole, with each emission phase traced to a different energy source.

  2. Prospect for Detection of Strongly Lensed Multi-messenger Signals of Binary Neutron Star Mergers

    astro-ph.HE 2026-07 conditional novelty 5.0

    Future CE+ET detectors may detect lensed BNS kilonovae at ~0.5/yr via pointed follow-up of known galaxy lenses, while lensed sGRBs and afterglows remain rare or undetectable with current-generation facilities.