Self-Consistent Picture of the Mass Ejection from a One Second Long Binary Neutron Star Merger Leaving a Short-Lived Remnant in a General-Relativistic Neutrino-Radiation Magnetohydrodynamic Simulation

被引:47
作者
Kiuchi, Kenta [1 ,2 ]
Fujibayashi, Sho [1 ]
Hayashi, Kota [2 ]
Kyutoku, Koutarou [2 ,3 ,4 ]
Sekiguchi, Yuichiro [2 ,5 ]
Shibata, Masaru [1 ,2 ]
机构
[1] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Potsdam, Germany
[2] Kyoto Univ, Yukawa Inst Theoret Phys, Ctr Gravitat Phys & Quantum Informat, Kyoto 6068502, Japan
[3] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan
[4] RIKEN, Interdisciplinary Theoret & Math Sci Program iTHEM, Wako, Saitama 3510198, Japan
[5] Toho Univ, Dept Phys, Funabashi, Chiba 2748510, Japan
关键词
EQUATION-OF-STATE; MULTI-MESSENGER OBSERVATIONS; INFRARED LIGHT CURVES; GAMMA-RAY BURSTS; ELECTROMAGNETIC COUNTERPART; DYNAMICAL EJECTA; OPTICAL COUNTERPART; GRMHD SIMULATIONS; MAGNETIC-FIELD; JET-AFTERGLOW;
D O I
10.1103/PhysRevLett.131.011401
中图分类号
O4 [物理学];
学科分类号
0702 ;
摘要
We perform a general-relativistic neutrino-radiation magnetohydrodynamic simulation of a one secondlong binary neutron star merger on the Japanese supercomputer Fugaku using about 85 million CPU hours with 20 736 CPUs. We consider an asymmetric binary neutron star merger with masses of 1.2M0 and 1.5M0 anda "soft" equation of state SFHo. It results in a short-lived remnant with the lifetime of i:10.017 s, and subsequent massive torus formation with the mass of i:10.05M0 after the remnant collapses to a black hole. For the first time, we find that after the dynamical mass ejection, which drives the fast tail and mildly relativistic components, the postmerger mass ejection from the massive torus takes place due to the magnetorotational instability-driven turbulent viscosity in a single simulation and the two ejecta components are seen in the distributions of the electron fraction and velocity with distinct features.
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页数:8
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