Modeling kicks from the merger of generic black-hole binaries

Details Modeling kicks from the merger of generic black-hole binaries Modeling kicks from the merger of generic black-hole binaries

2008-02-04

arxiv.org/abs/0802.0416v2

Astrophys.J.682:L29-L32,2008

Astronomy and Astrophysics

Astrophysics

5 pages, 1 figure, 3 tables. Version published in Astrophys. J. Lett

Scientific paper

10.1086/590927

Recent numerical relativistic results demonstrate that the merger of comparable-mass spinning black holes has a maximum ``recoil kick'' of up to $\sim 4000 \kms$. However the scaling of these recoil velocities with mass ratio is poorly understood. We present new runs showing that the maximum possible kick perpendicular to the orbital plane does not scale as $\sim\eta^2$ (where $\eta$ is the symmetric mass ratio), as previously proposed, but is more consistent with $\sim\eta^3$, at least for systems with low orbital precession. We discuss the effect of this dependence on galactic ejection scenarios and retention of intermediate-mass black holes in globular clusters.

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