Gravitational Waves and Neutrino Emission from the Merger of Binary Neutron Stars

被引：219

作者：

Sekiguchi, Yuichiro ^{[1
]}

Kiuchi, Kenta ^{[1
]}

Kyutoku, Koutarou ^{[1
]}

Shibata, Masaru ^{[1
]}

机构：

[1] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan

来源：

PHYSICAL REVIEW LETTERS | 2011年 / 107卷 / 05期

关键词：

EQUATION-OF-STATE; PHYSICAL MODELS; NUCLEAR-MATTER; CORE-COLLAPSE; EVOLUTION; SIMULATIONS; SUPERNOVA; STEP;

D O I：

10.1103/PhysRevLett.107.051102

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

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 (>> 10 ms) is the outcome for the total mass less than or similar to 3.0M(circle dot). It is shown that the typical total neutrino luminosity of the HMNS is similar to 3-8 x 10(53) erg/s and the effective amplitude of gravitational waves from the HMNS is 4-6 x 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.

引用

页数：5

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