Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 682, Issue 1, Pages L29-L32Publisher
IOP PUBLISHING LTD
DOI: 10.1086/590927
Keywords
black hole physics; galaxies : nuclei; gravitational waves; relativity
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Recent numerical relativistic results demonstrate that the merger of comparable-mass spinning black holes has a maximum recoil kick of up to similar to 4000 km s(-1). 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 similar to eta(2) (where eta is the symmetric mass ratio), as previously proposed, but is more consistent with similar to 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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