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• W2605924385 abstract "Employing a simplified version of the Israel-Stewart formalism for general-relativistic shear-viscous hydrodynamics, we perform axisymmetric general-relativistic simulations for a rotating neutron star surrounded by a massive torus, which can be formed from differentially rotating stars. We show that with our choice of a shear-viscous hydrodynamics formalism, the simulations can be stably performed for a long time scale. We also demonstrate that with a possibly high shear-viscous coefficient, not only viscous angular momentum transport works but also an outflow could be driven from a hot envelope around the neutron star for a time scale $ensuremath{gtrsim}100text{ }text{ }mathrm{ms}$ with the ejecta mass $ensuremath{gtrsim}{10}^{ensuremath{-}2}text{ }text{ }{M}_{ensuremath{bigodot}}$, which is comparable to the typical mass for dynamical ejecta of binary neutron-star mergers. This suggests that massive neutron stars surrounded by a massive torus, which are typical outcomes formed after the merger of binary neutron stars, could be the dominant source for providing neutron-rich ejecta, if the effective shear viscosity is sufficiently high, i.e., if the viscous $ensuremath{alpha}$ parameter is $ensuremath{gtrsim}{10}^{ensuremath{-}2}$. The present numerical result indicates the importance of a future high-resolution magnetohydrodynamics simulation that is the unique approach to clarify the viscous effect in the merger remnants of binary neutron stars by the first-principle manner." @default.
• W2605924385 created "2017-04-28" @default.
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• W2605924385 date "2017-04-11" @default.
• W2605924385 modified "2023-10-14" @default.
• W2605924385 title "General relativistic viscous hydrodynamics of differentially rotating neutron stars" @default.
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• W2605924385 doi "https://doi.org/10.1103/physrevd.95.083005" @default.
• W2605924385 hasPublicationYear "2017" @default.
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