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Gravitational waves and neutrino emission from the merger of binary neutron stars

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arxiv 1105.2125 v2 pith:YCBEURZT submitted 2011-05-11 gr-qc astro-ph.HE

Yuichiro Sekiguchi , Kenta Kiuchi , Koutarou Kyutoku , Masaru Shibata This is my paper · ORCID
classification gr-qcastro-ph.HE
keywords neutrinohmnsneutronbinaryfirstgravitationalluminositymerger
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abstract

Numerical simulations for the merger of binary neutron stars are performed in full general relativity incorporating a finite-temperature (Shen's) equation of state (EOS) and neutrino cooling for the first time. It is found that for this stiff EOS, a hypermassive neutron star (HMNS) with a long lifetime ($\gg 10$ ms) is the outcome for the total mass $\alt 3.0M_{\odot}$. It is shown that the typical total neutrino luminosity of the HMNS is $\sim 3$--$8\times 10^{53}$ ergs/s and the effective amplitude of gravitational waves from the HMNS is 4--$6 \times 10^{-22}$ at $f=2.1$--2.5 kHz for a source distance of 100 Mpc. We also present the neutrino luminosity curve when a black hole is formed for the first time.

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Forward citations

Cited by 6 Pith papers

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