2018
DOI: 10.3847/1538-4357/aabafd
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Mass Ejection from the Remnant of a Binary Neutron Star Merger: Viscous-radiation Hydrodynamics Study

Abstract: We perform long-term general relativistic neutrino-radiation hydrodynamics simulations (in axisymmetry) for a massive neutron star (MNS) surrounded by a torus, which is a canonical remnant formed after the binary neutron star merger. We take into account effects of viscosity which is likely to arise in the merger remnant due to magnetohydrodynamical turbulence. The viscous effect plays key roles for the mass ejection from the remnant in two phases of the evolution. In the first t 10 ms, a differential rotation… Show more

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Cited by 279 publications
(376 citation statements)
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“…For our shear viscous hydrodynamics simulations [65,66], we have to give the shear viscous coefficient ν. Using the α-viscous prescription [67,68], we set it as…”
Section: Evolution Of Massive Neutron Star-torus Systemmentioning
confidence: 99%
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“…For our shear viscous hydrodynamics simulations [65,66], we have to give the shear viscous coefficient ν. Using the α-viscous prescription [67,68], we set it as…”
Section: Evolution Of Massive Neutron Star-torus Systemmentioning
confidence: 99%
“…For the viscous evolution of a remnant massive neutron star surrounded by a torus, there are two mechanisms for the mass ejection [65]. In the short-term evolution with the duration in a few tens of ms, the differential rotation of the remnant massive neutron star becomes the engine for the mass ejection.…”
Section: Evolution Of Massive Neutron Star-torus Systemmentioning
confidence: 99%
See 3 more Smart Citations