Global simulations of strongly magnetized remnant massive neutron stars formed in binary neutron star mergers
Global simulations of strongly magnetized remnant massive neutron stars formed in binary neutron star mergers
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DOI：
10.1103/physrevd.97.124039
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发表时间：
2017-10
影响因子：
5
通讯作者：
K. Kiuchi;K. Kyutoku;Y. Sekiguchi;M. Shibata
中科院分区：
文献类型：
--
作者：
K. Kiuchi;K. Kyutoku;Y. Sekiguchi;M. Shibata
我们进行了广义相对论磁流体动力学模拟约30$ ms合并后的一个二元中子星星的残余大质量中子星星（RMNS）的最好的网格分辨率为12.5 $ m的高空间分辨率。首先，我们估计，在合并的开尔文-亥姆霍兹不稳定性可以放大的磁场能量高达$\sim 1\%$的热能。第二，我们发现在$rho < 10^{13}~{\rmg ~cm^{-3}}$的RMNS包络和环面中，磁旋转不稳定性维持磁湍流状态，并且在这些区域中的有效粘性参数可能收敛到$\approximately 0.01$-0.02 $。第三，目前的网格分辨率还不足以维持RMNS中的磁湍流态（$\rho \ge 10^{13}~{\rm g~cm^{-3}}$）。
We perform a general-relativistic magnetohydrodynamics simulation for $\approx 30$ ms after merger of a binary neutron star to a remnant massive neutron star (RMNS) with a high spatial resolution of the finest grid resolution $12.5$ m. First, we estimate that the Kelvin-Helmholtz instability at merger could amplify the magnetic-field energy up to $\sim 1\%$ of the thermal energy. Second, we find that the magnetorotational instability in the RMNS envelope and torus with $\rho < 10^{13}~{\rm g~cm^{-3}}$ sustains magneto-turbulent state and the effective viscous parameter in these regions is likely to converge to $\approx 0.01$--$0.02$ with respect to the grid resolution. Third, the current grid resolution is not still fine enough to sustain magneto-turbulent state in the RMNS with $\rho \ge 10^{13}~{\rm g~cm^{-3}}$.