Computing the merger of black-hole binaries: The IBBH problem

被引：70

作者：

Brady, PR ^{[1
]}

Creighton, JDE ^{[1
]}

Thorne, KS ^{[1
]}

机构：

[1] CALTECH, Pasadena, CA 91125 USA

来源：

PHYSICAL REVIEW D | 1998年 / 58卷 / 06期

基金：

美国国家科学基金会;

关键词：

D O I：

10.1103/PhysRevD.58.061501

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Gravitational radiation arising from the inspiral and merger of binary black holes (BBH's) is a promising candidate for detection by kilometer-scale interferometric gravitational wave observatories. This Rapid Communication discusses a serious obstacle to searches for such radiation and to the interpretation of any observed waves: the inability of current computational techniques to evolve a BBH through its last similar to 10 orbits of inspiral (similar to 100 radians of gravitational-wave phase). A new set of numerical-relativity techniques is proposed for solving this "intermediate binary black hole" (IBBH) problem: (i) numerical evolutions performed in coordinates co-rotating with the BBH, in which the metric coefficients evolve on the long timescale of inspiral, and (ii) techniques for mathematically freezing out gravitational degrees of freedom that are not excited by the waves. [S0556-2821(98)50218-4].

引用

页数：5

共 23 条

[21] Post-Newtonian expansion of gravitational waves from a particle in circular orbit around a rotating black hole: Up to O(v(8)) beyond the quadrupole formula [J].