Modeling kicks from the merger of nonprecessing black hole binaries

被引:93
作者
Baker, John G. [1 ]
Boggs, William D.
Centrella, Joan
Kelly, Bernard J.
McWilliams, Sean T.
Miller, M. Coleman
van Meter, James R.
机构
[1] Univ Maryland, Dept Phys, College Pk, MD 20742 USA
[2] Univ Maryland, Dept Astron, College Pk, MD 20742 USA
[3] NASA, Goddard Space Flight Ctr, Lab Gravitat Astrophys, Greenbelt, MD 20771 USA
关键词
black hole physics; galaxies : nuclei; gravitational waves; relativity;
D O I
10.1086/521330
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Several groups have recently computed the gravitational radiation recoil produced by the merger of two spinning black holes. The results suggest that spin can be the dominant contributor to the kick, with reported recoil speeds of hundreds to even thousands of kilometers per second. The parameter space of spin kicks is large, however, and it is ultimately desirable to have a simple formula that gives the approximate magnitude of the kick given a mass ratio, spin magnitudes, and spin orientations. As a step toward this goal, we perform a systematic study of the recoil speeds from mergers of black holes with mass ratio q = m(1)/m(2) = 2/ 3 and dimensionless spin parameters of a(1)/m(1) and a(2)/m(2) equal to 0 or 0.2, with directions aligned or antialigned with the orbital angular momentum. We also run an equal-mass a(1)/m(1) = -a(2)/m(2) = 0.2 case, and find good agreement with previous results. We find that, for currently reported kicks from aligned or antialigned spins, a simple kick formula inspired by post-Newtonian analyses can reproduce the numerical results to better than similar to 10%.
引用
收藏
页码:1140 / 1144
页数:5
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