Back to Volume
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.
Back to Volume