Efficient magnetic-field amplification due to the Kelvin-Helmholtz instability in binary neutron star mergers

被引：193

作者：

Kiuchi, Kenta ^{[1
]}

Cerda-Duran, Pablo ^{[2
]}

Kyutoku, Koutarou ^{[3
]}

Sekiguchi, Yuichiro ^{[4
]}

Shibata, Masaru ^{[1
]}

机构：

[1] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan

[2] Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Valencia, Spain

[3] RIKEN, Interdisciplinary Theoret Sci iTHES Res Grp, Wako, Saitama 3510198, Japan

[4] Toho Univ, Dept Phys, Funabashi, Chiba 2748510, Japan

来源：

PHYSICAL REVIEW D | 2015年 / 92卷 / 12期

基金：

欧洲研究理事会;

关键词：

TURBULENCE; SIMULATIONS; EQUATIONS; MODELS;

D O I：

10.1103/PhysRevD.92.124034

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 approximate to 10(3). We also explore the saturation of the magnetic-field energy and our result shows that it is likely to be greater than or similar to 4 x10(50) erg, which is greater than or similar to 0.1% of the bulk kinetic energy of the merging binary neutron stars.

引用

页数：11

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