Gravitational Waves from the Papaloizou-Pringle Instability in Black-Hole-Torus Systems

被引：72

作者：

Kiuchi, Kenta ^{[1
]}

Shibata, Masaru ^{[1
]}

Montero, Pedro J. ^{[2
]}

Font, Jose A. ^{[3
]}

机构：

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

[2] Max Planck Inst Astrophys, D-81748 Garching, Germany

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

来源：

PHYSICAL REVIEW LETTERS | 2011年 / 106卷 / 25期

关键词：

ROTATING SUPERMASSIVE STAR; ACCRETION DISKS; SIMULATIONS; COLLAPSE; MASS;

D O I：

10.1103/PhysRevLett.106.251102

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

Black hole (BH)-torus systems are promising candidates for the central engine of gamma-ray bursts (GRBs), and also possible outcomes of the collapse of supermassive stars to supermassive black holes (SMBHs). By three-dimensional general relativistic numerical simulations, we show that an m = 1 nonaxisymmetric instability grows for a wide range of self-gravitating tori orbiting BHs. The resulting nonaxisymmetric structure persists for a time scale much longer than the dynamical one, becoming a strong emitter of large amplitude, quasiperiodic gravitational waves. Our results indicate that both, the central engine of GRBs and newly formed SMBHs, can be strong gravitational wave sources observable by forthcoming ground-based and spacecraft detectors.

引用

页数：4

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