Gravitational radiation from plunging orbits: Perturbative study

Mino, Yasushi; Brink, Jeandrew

doi:10.1103/physrevd.78.124015

Cited by 29 publications

(53 citation statements)

References 43 publications

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“…In this analysis, we have demonstrated that perturbation theoretical techniques based on the Teukolsky equation are an excellent tool for extending the reach of our computations, allowing us to model large mass ratios that are challenging for 3+1 numerical simulations, but may be of astrophysical significance. Our analysis joins previous work by Damour and colleagues [46,47], Mino and Brink [57], and by Lousto and colleagues [56] which likewise used perturbation theory to model large mass ratio binaries. By using the Teukolsky equation, we can explore how the larger black hole's spin impacts the analysis, exemplified by our demonstration of how the previously identified "antikick" [82] strongly depends on this spin.…”

Section: Discussionsupporting

confidence: 75%

“…III B, this behavior arises by virtue of how the Teukolsky equation's source term goes to zero, so that its solutions transition to their homogeneous form, as the infalling body approaches the large black hole's event horizon. Mino and Brink [57] first appear to have exploited this behavior, which was also seen in recent work by Lousto, Nakano, Zlochower, and Campanelli [56]. This demonstrates the power of perturbative methods at modeling physically important aspects of the merger waves.…”

Section: This Papersupporting

confidence: 52%

“…Finally, Mino and Brink [57] used perturbative techniques to model the waves from the plunge, quantifying the manner in which the geometry of the final infall impacts the kick imparted to the binary. As already mentioned, their analysis also took advantage of the manner in which the source redshifts away as the infalling body approaches the larger black hole's event horizon.…”

Section: B Gravitational-wave Recoilmentioning

confidence: 99%

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Binary black hole merger gravitational waves and recoil in the large mass ratio limit

Sundararajan¹,

Khanna

Hughes³

2010

Phys. Rev. D

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Spectacular breakthroughs in numerical relativity now make it possible to compute spacetime dynamics in almost complete generality, allowing us to model the coalescence and merger of binary black holes with essentially no approximations. The primary limitation of these calculations is now computational. In particular, it is difficult to model systems with large mass ratio and large spins, since one must accurately resolve the multiple lengthscales which play a role in such systems. Perturbation theory can play an important role in extending the reach of computational modeling for binary systems. In this paper, we present first results of a code which allows us to model the gravitational waves generated by the inspiral, merger, and ringdown of a binary system in which one member of the binary is much more massive than the other. This allows us to accurately calibrate binary dynamics in the large mass ratio regime. We focus in this analysis on the recoil imparted to the merged remnant by these waves. We closely examine the "antikick," an anti-phase cancellation of the recoil arising from the plunge and ringdown waves, described in detail by Schnittman et al. We find that, for orbits aligned with the black hole spin, the antikick grows as a function of spin. The total recoil is smallest for prograde coalescence into a rapidly rotating black hole, and largest for retrograde coalescence. Amusingly, this completely reverses the predicted trend for kick versus spin from analyses that only include inspiral information.

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Section: Discussionsupporting

confidence: 75%

Section: This Papersupporting

confidence: 52%

Section: B Gravitational-wave Recoilmentioning

confidence: 99%

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Binary black hole merger gravitational waves and recoil in the large mass ratio limit

Sundararajan¹,

Khanna

Hughes³

2010

Phys. Rev. D

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“…An important issue in all attempts to model binary coalescence with perturbation theory is the computation of the so-called excitation coefficients, or more generally the question of which fundamental frequencies contribute to the radiation. In this context, perturbation-theory calculations are offering new insights [49][50][51][52].…”

Section: Introductionmentioning

confidence: 99%

Modeling multipolar gravitational-wave emission from small mass-ratio mergers

Barausse

Buonanno

Hughes³

et al. 2012

Phys. Rev. D

163

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Using the effective-one-body (EOB) formalism and a time-domain Teukolsky code, we generate inspiral, merger, and ringdown waveforms in the small mass-ratio limit. We use EOB inspiral and plunge trajectories to build the Teukolsky equation source term, and compute full coalescence waveforms for a range of black hole spins. By comparing EOB waveforms that were recently developed for comparable mass binary black holes to these Teukolsky waveforms, we improve the EOB model for the (2, 2), (2, 1), (3, 3), and (4, 4) modes. Our results can be used to quickly and accurately extract useful information about merger waves for binaries with spin, and should be useful for improving analytic models of such binaries.

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“…Black-hole perturbation theory is, instead, the natural tool to model large-mass-ratio binaries [9][10][11][12][13][14][15][16][17][18][19]. The relative dynamics of the binary is described by the motion of a particle (representing the small black hole) in a fixed background, black-hole spacetime (representing the central, supermassive black hole).…”

Section: Introductionmentioning

confidence: 99%

Binary black hole coalescence in the large-mass-ratio limit: The hyperboloidal layer method and waveforms at null infinity

Bernuzzi¹,

2011

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We compute and analyze the gravitational waveform emitted to future null infinity by a system of two black holes in the large-mass-ratio limit. We consider the transition from the quasiadiabatic inspiral to plunge, merger, and ringdown. The relative dynamics is driven by a leading order in the mass ratio, 5PN-resummed, effective-one-body (EOB), analytic-radiation reaction. To compute the waveforms, we solve the Regge-Wheeler-Zerilli equations in the time-domain on a spacelike foliation, which coincides with the standard Schwarzschild foliation in the region including the motion of the small black hole, and is globally hyperboloidal, allowing us to include future null infinity in the computational domain by compactification. This method is called the hyperboloidal layer method, and is discussed here for the first time in a study of the gravitational radiation emitted by black hole binaries. We consider binaries characterized by five mass ratios, ¼ 10 À2;À3;À4;À5;À6 , that are primary targets of space-based or thirdgeneration gravitational wave detectors. We show significative phase differences between finite-radius and null-infinity waveforms. We test, in our context, the reliability of the extrapolation procedure routinely applied to numerical relativity waveforms. We present an updated calculation of the final and maximum gravitational recoil imparted to the merger remnant by the gravitational wave emission, v end kick =ðc 2 Þ ¼ 0:04474 AE 0:00007 and v max kick =ðc 2 Þ ¼ 0:05248 AE 0:00008. As a self-consistency test of the method, we show an excellent fractional agreement (even during the plunge) between the 5PN EOB-resummed mechanical angular momentum loss and the gravitational wave angular momentum flux computed at null infinity. New results concerning the radiation emitted from unstable circular orbits are also presented. The high accuracy waveforms computed here could be considered for the construction of template banks or for calibrating analytic models such as the effective-one-body model.

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Gravitational radiation from plunging orbits: Perturbative study

Cited by 29 publications

References 43 publications

Binary black hole merger gravitational waves and recoil in the large mass ratio limit

Binary black hole merger gravitational waves and recoil in the large mass ratio limit

Modeling multipolar gravitational-wave emission from small mass-ratio mergers

Binary black hole coalescence in the large-mass-ratio limit: The hyperboloidal layer method and waveforms at null infinity

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