Efficient magnetic-field amplification due to the Kelvin-Helmholtz instability in binary neutron star mergers
Efficient magnetic-field amplification due to the Kelvin-Helmholtz instability in binary neutron star mergers
复制标题
DOI：
10.1103/physrevd.92.124034
复制
发表时间：
2015-09
影响因子：
5
通讯作者：
K. Kiuchi;P. Cerd'a-Dur'an;K. Kyutoku;Y. Sekiguchi;M. Shibata
中科院分区：
文献类型：
--
作者：
K. Kiuchi;P. Cerd'a-Dur'an;K. Kyutoku;Y. Sekiguchi;M. Shibata
我们研究了双中子星合并过程中由于开尔文-亥姆霍兹不稳定性引起的磁场放大问题。通过在日本超级计算机“K”上进行高分辨率的广义相对论磁流体力学模拟，在合并开始后，对$4$-$5$ms的分辨率为$17.5$m，我们发现，中等最大强度$10^{13}$G的初始磁场至少放大了约10^3$。我们还讨论了磁场能量的饱和，结果表明它可能是合并的双中子星的体积动能的0.1倍，即10^{50}的4倍。
We explore magnetic-field amplification due to the Kelvin-Helmholtz instability during binary neutron star mergers. By performing high-resolution general relativistic magnetohydrodynamics simulations with a resolution of $17.5$ m for $4$--$5$ ms after the onset of the merger on the Japanese supercomputer "K", we find that an initial magnetic field of moderate maximum strength $10^{13}$ G is amplified at least by a factor of $\approx 10^3$. We also explore the saturation of the magnetic-field energy and our result shows that it is likely to be $\gtrsim 4 \times 10^{50}$ erg, which is $\gtrsim 0.1\%$ of the bulk kinetic energy of the merging binary neutron stars.