High-resolution numerical-relativity simulations for the merger of binary magnetized neutron stars
High-resolution numerical-relativity simulations for the merger of binary magnetized neutron stars
复制标题
双磁化中子星合并的高分辨率数值相对论模拟
DOI：
10.1103/physrevd.90.041502
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发表时间：
2014
影响因子：
5
通讯作者：
and T. Wada
中科院分区：
文献类型：
--
作者：
K. Kiuchi;K. Kyutoku;Y. Sekiguchi;M. Shibata;and T. Wada
我们在日本超级计算机K。中子星和合并残留物被70米的网格间距所覆盖，这是迄今为止得出的结果中分辨率最高的。通过深入的分辨率研究，首次阐明了中子星星并合过程中磁场的几种放大机制。首先，在合并开始时剪切层中发展的开尔文-亥姆霍兹不稳定性显著地放大了磁场。合并后形成的超大质量中子星星（HMNS）会受到非轴对称的磁旋转不稳定性的影响，这会放大HMNS中的磁场。这两种放大机制不能用非相干分辨率运行找到。我们还表明，HMNS最终崩溃的黑洞所包围的吸积环面，这是强磁化在出生。
We perform high-resolution magnetohydrodynamics simulations of binary neutron star mergers in numerical relativity on the Japanese supercomputer K. The neutron stars and merger remnants are covered by a grid spacing of 70 m, which yields the highest-resolution results among those derived so far. By an in-depth resolution study, we clarify several amplification mechanisms of magnetic fields during the binary neutron star merger for the first time. First, the Kelvin-Helmholtz instability developed in the shear layer at the onset of the merger significantly amplifies the magnetic fields. A hypermassive neutron star (HMNS) formed after the merger is then subject to the nonaxisymmetric magnetorotational instability, which amplifies the magnetic field in the HMNS. These two amplification mechanisms cannot be found with insufficient-resolution runs. We also show that the HMNS eventually collapses to a black hole surrounded by an accretion torus which is strongly magnetized at birth.