High resolution numerical relativity simulations for the merger of binary magnetized neutron stars

被引：189

作者：

Kiuchi, Kenta ^{[1
]}

Kyutoku, Koutarou ^{[2
]}

Sekiguchi, Yuichiro ^{[1
]}

Shibata, Masaru ^{[1
]}

Wada, Tomohide ^{[3
]}

机构：

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

[2] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA

[3] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

来源：

PHYSICAL REVIEW D | 2014年 / 90卷 / 04期

关键词：

LOCAL SHEAR INSTABILITY; DISKS;

D O I：

10.1103/PhysRevD.90.041502

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：5

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