Recoil Velocities from Equal-Mass Binary-Black-Hole Mergers

Koppitz, Michael; Pollney, Denis; Reisswig, Christian; Rezzolla, Luciano; Thornburg, Jonathan; Diener, Peter; Schnetter, Erik

doi:10.1103/physrevlett.99.041102

Cited by 232 publications

(297 citation statements)

References 34 publications

(40 reference statements)

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“…If the IMBH is rapidly spinning, recent numerical relativity results suggest that the kick can be a lot higher (Baker et al 2007;Campanelli et al 2007aCampanelli et al , 2007bGonzalez et al 2007a;Herrmann et al 2007b;Koppitz et al 2007). Baker et al (2007) and Campanelli et al (2007a) provide a fit to numerical relativity results that gives the kick as a function of the various orbital parameters.…”

Section: Number Density Of Globulars With a Suitable Imbhmentioning

confidence: 99%

Rates and Characteristics of Intermediate Mass Ratio Inspirals Detectable by Advanced LIGO

Mandel

Brown

Gair

et al. 2008

ApJ

128

179

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Gravitational waves (GWs) from the inspiral of a neutron star ( NS) or stellar-mass black hole ( BH ) into an intermediate-mass black hole ( IMBH ) with mass M $ 50 350 M may be detectable by the planned advanced generation of ground-based GW interferometers. Such intermediate mass ratio inspirals (IMRIs) are most likely to be found in globular clusters. We analyze four possible IMRI formation mechanisms: (1) hardening of an NS-IMBH or BH-IMBH binary via three-body interactions, (2) hardening via Kozai resonance in a hierarchical triple system, (3) direct capture, and (4) inspiral of a CO from a tidally captured main-sequence star; we also discuss tidal effects when the inspiraling object is an NS. For each mechanism we predict the typical eccentricities of the resulting IMRIs. We find that IMRIs will have largely circularized by the time they enter the sensitivity band of ground-based detectors. Hardening of a binary via three-body interactions, which is likely to be the dominant mechanism for IMRI formation, yields eccentricities under 10 À4 when the GW frequency reaches 10 Hz. Even among IMRIs formed via direct captures, which can have the highest eccentricities, around 90% will circularize to eccentricities under 0.1 before the GW frequency reaches 10 Hz. We estimate the rate of IMRI coalescences in globular clusters and the sensitivity of a network of three Advanced LIGO detectors to the resulting GWs. We show that this detector network may see up to tens of IMRIs per year, although rates of one to a few per year may be more plausible. We also estimate the loss in signal-to-noise ratio that will result from using circular IMRI templates for data analysis and find that, for the eccentricities we expect, this loss is negligible.

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Section: Number Density Of Globulars With a Suitable Imbhmentioning

confidence: 99%

Rates and Characteristics of Intermediate Mass Ratio Inspirals Detectable by Advanced LIGO

Mandel

Brown

Gair

et al. 2008

ApJ

128

179

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“…(4.18), we can rewrite the effective amplitude and phase of the waveforms in terms of M and η as: 19) where the constant C is given by Eq.(4.17). We use this family of parametrized waveforms to create a two- dimensional template bank of non-spinning waveforms.…”

Section: From Phenomenological To Physical Parametersmentioning

confidence: 99%

“…The field is now rapidly developing the capability to routinely evolve generic black-hole binary configurations in the comparable-mass regime, and to accurately extract the gravitational-wave signal. Important milestones include simulations of unequal-mass binaries and calculations of the gravitational recoil effect and the evolution of black-hole binaries with spin [14,15,16,17,18,19,20,21,22,23,24].…”

Section: Introductionmentioning

confidence: 99%

Erratum: Template bank for gravitational waveforms from coalescing binary black holes: Nonspinning binaries [Phys. Rev. DPRVDAQ1550-799877, 104017 (2008)]

Ajith¹,

Babak²,

Chen³

et al. 2009

Phys. Rev. D

183

209

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Gravitational waveforms from the inspiral and ring-down stages of the binary black hole coalescences can be modelled accurately by approximation/perturbation techniques in general relativity. Recent progress in numerical relativity has enabled us to model also the non-perturbative merger phase of the binary black-hole coalescence problem. This enables us to coherently search for all three stages of the coalescence of non-spinning binary black holes using a single template bank. Taking our motivation from these results, we propose a family of template waveforms which can model the inspiral, merger, and ring-down stages of the coalescence of non-spinning binary black holes that follow quasi-circular inspiral. This two-dimensional template family is explicitly parametrized by the physical parameters of the binary. We show that the template family is not only effectual in detecting the signals from black hole coalescences, but also faithful in estimating the parameters of the binary. We compare the sensitivity of a search (in the context of different ground-based interferometers) using all three stages of the black hole coalescence with other template-based searches which look for individual stages separately. We find that the proposed search is significantly more sensitive than other template-based searches for a substantial mass-range, potentially bringing about remarkable improvement in the event-rate of ground-based interferometers. As part of this work, we also prescribe a general procedure to construct interpolated template banks using non-spinning black hole waveforms produced by numerical relativity.

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“…We treat the imparted recoil velocity V k essentially as a free parameter ranging from V k = 100 km s −1 to V k = 3000 km s −1 , where the latter values are not realistic and serve here only to appreciate the disc dynamics under extreme conditions. We recall, in fact, that the recoil velocities in the orbital plane are expected to be < ∼ 450 km s −1 (Koppitz et al 2007;Herrmann et al 2007;Pollney et al 2007).…”

Section: Initial Modelsmentioning

confidence: 99%

Electromagnetic counterparts of recoiling black holes: general relativistic simulations of non-Keplerian discs

Zanotti

Rezzolla

Zanna

et al. 2010

A&A

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Aims. We investigate the dynamics of a circumbinary disc that responds to the loss of mass and to the recoil velocity of the black hole produced by the merger of a binary system of supermassive black holes. Methods. We perform the first two-dimensional general relativistic hydrodynamics simulations of extended non-Keplerian discs and employ a new technique to construct a "shock detector", thus determining the precise location of the shocks produced in the accreting disc by the recoiling black hole. In this way we can study how the properties of the system, such as the spin, mass and recoil velocity of the black hole, affect the mass accretion rate and are imprinted on the electromagnetic emission from these sources. Results. We argue that the estimates of the bremsstrahlung luminosity computed without properly taking into account the radiation transfer yield cooling times that are unrealistically short. At the same time we show, through an approximation based on the relativistic isothermal evolution, that the luminosity produced can reach a peak value above L 10 43 erg/s at about ∼30 d after the merger of a binary with total mass M 10 6 M and persist for several days at values which are a factor of a few smaller. If confirmed by more sophisticated calculations such a signal could indeed lead to an electromagnetic counterpart of the merger of binary black-hole system.

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Recoil Velocities from Equal-Mass Binary-Black-Hole Mergers

Cited by 232 publications

References 34 publications

Rates and Characteristics of Intermediate Mass Ratio Inspirals Detectable by Advanced LIGO

Rates and Characteristics of Intermediate Mass Ratio Inspirals Detectable by Advanced LIGO

Erratum: Template bank for gravitational waveforms from coalescing binary black holes: Nonspinning binaries [Phys. Rev. DPRVDAQ1550-799877, 104017 (2008)]

Electromagnetic counterparts of recoiling black holes: general relativistic simulations of non-Keplerian discs

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