Relativistic diskoseismology

被引：164

作者：

Wagoner, RV ^{[1
]}

机构：

[1] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

[2] Stanford Univ, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA

来源：

PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS | 1999年 / 311卷 / 3-5期

基金：

美国国家航空航天局;

关键词：

black holes; accretion disks;

D O I：

10.1016/S0370-1573(98)00104-5

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

We will summarize results of calculations of the modes of oscillation trapped within the inner region of accretion disks by the strong-field gravitational properties of a black hole (or a compact, weakly magnetized neutron star). Their driving and damping will also be addressed. The focus will be on the most observable class: the analogue of internal gravity modes in stars. Their frequencies which correspond to the lowest mode numbers depend almost entirely upon only the mass and angular momentum of the black hole. Such a feature may have been detected in the X-Ray power spectra of two galactic "microquasars", allowing the angular momentum of the black hole to be determined in one case. (C) 1999 Elsevier Science B.V. All rights reserved.

引用

页码：259 / 269

页数：11

共 34 条

[1] RAPIDLY ROTATING NEUTRON-STARS IN GENERAL-RELATIVITY - REALISTIC EQUATIONS OF STATE [J].