Gravitational Recoil Velocities from Eccentric Binary Black Hole Mergers

Sopuerta, Carlos F.; Yunes, Nicolás; Laguna, Pablo

doi:10.1086/512067

Cited by 63 publications

(78 citation statements)

References 35 publications

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“…The merger of two BHs forms a single BH that receives a recoil kick due to anisotropic emission of gravitational radiation during the merger. We use the results of Sopuerta et al (2007;their best estimate model) to estimate the magnitude of this kick.…”

Section: Standard Cluster Modelmentioning

confidence: 99%

The Total Merger Rate of Compact Object Binaries in the Local Universe

Sądowski

Belczyński

Bulik

et al. 2008

ApJ

130

157

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Using a population synthesis approach, we compute the total merger rate in the local universe for double neutron stars, double black holes, and black hole-neutron star binaries. These compact binaries are the prime source candidates for gravitational wave detection by LIGO and VIRGO. We account for mergers originating both from field populations and from dense stellar clusters, where dynamical interactions can significantly enhance the production of double compact objects. For both populations we use the same treatment of stellar evolution. Our results indicate that the merger rates of double neutron stars and black hole-neutron star binaries are strongly dominated by field populations, while merging black hole binaries are formed much more effectively in dense stellar clusters. The overall merger rate of double compact objects depends sensitively on the (largely unknown) initial mass fraction contained in dense clusters ( f cl ). For f cl P 0:0001, the Advanced LIGO detection rate will be dominated by field populations of double neutron star mergers, with a small but significant number of detections, $20 yr À1 . However, for a higher mass fraction in clusters, f cl k 0:001, the detection rate will be dominated by numerous mergers of double black holes originating from dense clusters, and it will be considerably higher, $25-300 yr À1 . In addition, we show that, once mergers of double black holes are detected, it is easy to differentiate between systems formed in the field and in dense clusters, since the chirp mass distributions are strikingly different. If significant field populations of double black hole mergers are detected, this will also place very strong constraints on common-envelope evolution in massive binaries. Finally, we point out that there may exist a population of merging black hole binaries in intergalactic space.

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Section: Standard Cluster Modelmentioning

confidence: 99%

The Total Merger Rate of Compact Object Binaries in the Local Universe

Sądowski

Belczyński

Bulik

et al. 2008

ApJ

130

157

View full text Add to dashboard Cite

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“…454 ‫ע‬ 25 km s than double the maximum recoil velocity found for nonspinning holes (González et al 2006), even including small eccentricity effects (Sopuerta et al 2007). Furthermore, the spin-induced recoil in the x-y plane might be offset by the mass-differenceinduced recoil, potentially implying that a rotation of the spin about the z-axis may lead to a significantly larger in-plane component of the recoil velocity.…”

mentioning

confidence: 91%

“…This will be the subject of an upcoming paper dV p Ϫp/2 by the authors. The total recoil velocity also acquires a correction (Sopuerta et al 2007) for small eccentricities, e, of the form .…”

mentioning

confidence: 99%

Large Merger Recoils and Spin Flips from Generic Black Hole Binaries

Campanelli

Lousto

Zlochower

et al. 2007

ApJ

517

648

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We report the first results from the evolution of generic black hole binaries, i.e., binaries containing unequalmass black holes with misaligned spins. Our configuration, which has a mass ratio of , consists of an initially 2 : 1 nonspinning hole orbiting a larger, rapidly spinning hole (specific spin ), with the spin direction a/m p 0.885 oriented Ϫ45Њ with respect to the orbital plane. We track the inspiral and merger for ∼2 orbits and find that the remnant receives a substantial kick of 454 km s Ϫ1 , more than twice as large as the maximum kick from nonspinning binaries. The remnant spin direction is flipped by 103Њ with respect to the initial spin direction of the larger hole. We performed a second run with antialigned spins, lying in the orbital plane that produces a kick a/m p ‫5.0ע‬ of ∼1830 km s Ϫ1 off the orbital plane. This value scales to nearly 4000 km s Ϫ1 for maximally spinning holes. Such a large recoil velocity opens up the possibility that a merged binary can be ejected even from the nucleus of a massive host galaxy.

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“…I, Ref. [18] suggests that maximum recoil velocity estimate for a binary with ν = 0.2 in quasicircular orbit lie in a range between (79-216) km s −1 . As mentioned above, our estimate for such system is ∼179.5 km s −1 and thus is consistent with their estimates.…”

Section: Resultsmentioning

confidence: 99%

“…It is evident from the above that the dependence of the relevant quantities on the integration variable τ is only through δφ which under the assumption of adiabatic inspiral takes the form 18) where second and higher derivatives of φ have been neglected. Finally, one just needs the following standard integral to compute the hereditary terms in (2.5)…”

Section: A Instantaneous Termsmentioning

confidence: 99%

2.5PN linear momentum flux from inspiralling compact binaries in quasicircular orbits and associated recoil: Nonspinning case

2012

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Anisotropic emission of gravitational waves (GWs) from inspiralling compact binaries leads to the loss of linear momentum and hence gravitational recoil of the system. The loss rate of linear momentum in the far-zone of the source (a nonspinning binary system of black holes in quasicircular orbit) is investigated at the 2.5 post-Newtonian (PN) order and used to provide an analytical expression in harmonic coordinates for the 2.5PN accurate recoil velocity of the binary accumulated in the inspiral phase. We find that the recoil velocity at the end of the inspiral phase (i.e at the innermost stable circular orbit (ISCO)) is maximum for a binary with symmetric mass ratio of ν ∼ 0.2 and is roughly about ∼4.58 km s −1 . Going beyond inspiral, we also provide an estimate of the more important contribution to the recoil velocity from the plunge phase. Again the recoil velocity at the end of the plunge, involving contributions both from inspiral and plunge phase, is maximum for a binary with ν ∼ 0.2 and is of the order of ∼180 km s −1 .

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Gravitational Recoil Velocities from Eccentric Binary Black Hole Mergers

Cited by 63 publications

References 35 publications

The Total Merger Rate of Compact Object Binaries in the Local Universe

The Total Merger Rate of Compact Object Binaries in the Local Universe

Large Merger Recoils and Spin Flips from Generic Black Hole Binaries

2.5PN linear momentum flux from inspiralling compact binaries in quasicircular orbits and associated recoil: Nonspinning case

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