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arXiv · 1105.2125

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

Yuichiro Sekiguchi·Kenta Kiuchi·Koutarou Kyutoku·Masaru Shibata
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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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Yuichiro Sekiguchi, Kenta Kiuchi, Koutarou Kyutoku, Masaru Shibata. 2011-06-24. Gravitational waves and neutrino emission from the merger of binary neutron stars. https://doi.org/10.1103/physrevlett.107.051102

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