2008
DOI: 10.1086/590927
|View full text |Cite
|
Sign up to set email alerts
|

Modeling Kicks from the Merger of Generic Black Hole Binaries

Abstract: Recent numerical relativistic results demonstrate that the merger of comparable-mass spinning black holes has a maximum "recoil kick" of up 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 ∼ η 2 (where η is the symmetric mass ratio), as previously proposed, but is more consistent with ∼ η 3 , at least for systems with low orbital precession. We … Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
2
2
1

Citation Types

7
233
2

Year Published

2008
2008
2015
2015

Publication Types

Select...
5
4

Relationship

0
9

Authors

Journals

citations
Cited by 188 publications
(242 citation statements)
references
References 80 publications
7
233
2
Order By: Relevance
“…This would lead to a recoil velocity in the resulting black hole that might be as high as 4000 km s −1 (Gonzalez et al 2007;Campanelli et al 2007b,a;Healy et al 2009;Herrmann et al 2007), depending on the mass ratio of the initial black holes and the directions of their spins, but this velocity might be significantly suppressed by the relativistic alignment of the spins (Kesden et al 2010). It is not easy, of course to include numerical relativity in an N-body code, but semi-analytical formulae, coming from fitting between numerical relativity results and post-Newtonian theory (Lousto & Zlochower 2008;Baker et al 2008;Lousto et al 2010) to determine the direction and magnitude of the recoil velocity. These semi-analytical formulas could be easily included in the binary module of Myriad, making the code a tool capable of reproducing collisions of black holes realistically.…”
Section: Discussionmentioning
confidence: 99%
“…This would lead to a recoil velocity in the resulting black hole that might be as high as 4000 km s −1 (Gonzalez et al 2007;Campanelli et al 2007b,a;Healy et al 2009;Herrmann et al 2007), depending on the mass ratio of the initial black holes and the directions of their spins, but this velocity might be significantly suppressed by the relativistic alignment of the spins (Kesden et al 2010). It is not easy, of course to include numerical relativity in an N-body code, but semi-analytical formulae, coming from fitting between numerical relativity results and post-Newtonian theory (Lousto & Zlochower 2008;Baker et al 2008;Lousto et al 2010) to determine the direction and magnitude of the recoil velocity. These semi-analytical formulas could be easily included in the binary module of Myriad, making the code a tool capable of reproducing collisions of black holes realistically.…”
Section: Discussionmentioning
confidence: 99%
“…As two black holes inspiral and coalesce, asymmetric emission of gravitational waves imparts a kick to the merged black hole (e.g., Fitchett 1983;Baker et al 2008;van Meter et al 2010). If this kick is larger than the escape velocity at the galaxy center, as can happen for high black hole spins and particular orientations, then the merged black hole will be ejected.…”
Section: Discussionmentioning
confidence: 99%
“…In case of random spin distributions (dry mergers), the kick formula (Campanelli et al 2007;Baker et al 2008;) predicts the kick fraction independent of recoil velocity (Campanelli et al 2007;Schnittman & Buonanno 2007;Baker et al 2008;Komossa & Merritt 2008b). Under these assumptions, kicks with velocities larger than 500 km s −1 are relatively common (Figure 1 of 454 S. Komossa Komossa & Merritt 2008b).…”
Section: The Frequency Of Recoiling Smbhsmentioning
confidence: 99%
“…As a result, when two SMBHs coalesce the newly formed single SMBH recoils. Configurations of coalescing black holes can lead to recoil velocities up to 3800 km s −1 (e.g., Campanelli et al 2007Campanelli et al , 2009González et al 2007González et al , 2009Herrmann et al 2007;Baker et al 2008;Brügmann et al 2008;Dain et al 2008;Miller & Matzner 2009;Le Tiec et al 2009;), for maximally spinning equal-mass black hole binaries with anti-aligned spins in the orbital plane. The kick velocity can be as large as ∼ 10 4 km s −1 in hyperbolic encounters (Healy et al 2009).…”
Section: Introductionmentioning
confidence: 99%