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| Paper: |
Physical Simulations for the Merger of Binary Neutron Stars in General Relativity |
| Volume: |
453, Advances in Computational Astrophysics: Methods, Tools, and Outcome |
| Page: |
161 |
| Authors: |
Shibata, M.; Kiuchi, K.; Kyutoku, K.; Sekiguchi, Y. |
| Abstract: |
We review the latest numerical simulations for the merger of binary
neutron stars performed in the framework of full general relativity
incorporating finite-temperature equations of state (EOS) and neutrino
cooling for the first time. We employ a purely nucleonic EOS and an
EOS incorporating a degree of freedom for hyperons, derived by Shen et
al. The numerical simulations show that for the purely nucleonic EOS,
a hypermassive neutron star (HMNS) with a long lifetime (≫ 10 ms)
is the outcome for the total mass M ≤ 3.0M☉. By contrast,
the formed HMNS collapse to a black hole in a shorter time scale in
the hyperonic EOS for M ≥ 2.7M☉. It is shown that the
typical total neutrino luminosity of the HMNS is ∼ 3–10×
1053 ergs/s and the effective amplitude of gravitational waves
from the HMNS is 2–6×10–22 at f≈ 2–2.5 kHz for a
source distance of 100 Mpc, depending on the mass and EOS. The
neutrino luminosity curves in the formation and evolution of black
holes are also presented, and we show that the total neutrino
luminosity of a torus surrounding the black holes is typically ∼
1053 ergs/s. If pair annihilation of neutrinos and anti-neutrinos
efficiently occurs, the HMNS and black hole-torus systems are
promising sources for the central engine of short gamma-ray bursts. |
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