Post-innermost stable circular orbit ringdown amplitudes in extreme mass ratio inspiral

Hadar, Shahar; Kol, Barak

doi:10.1103/physrevd.84.044019

Cited by 23 publications

(31 citation statements)

References 30 publications

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“…In this paper we use the conformal map to compute the gravitational radiation produced during this post-ISCO plunge into a near-extreme Kerr black hole. This complements the computation in [9] of radiation produced during the post-ISCO plunge into a nonrotating Schwarzschild black hole.…”

Section: Introductionmentioning

confidence: 57%

Gravity waves from extreme-mass-ratio plunges into Kerr black holes

2014

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Massive objects orbiting a near-extreme Kerr black hole quickly plunge into the horizon after passing the innermost stable circular orbit. The plunge trajectory is shown to be related by a conformal map to a circular orbit. Conformal symmetry of the near-horizon region is then used to compute the gravitational radiation produced during the plunge phase.the near-NHEK geometry [10] is obtained by scaling r ∼ κ to zero: PHYSICAL REVIEW D 90, 064045 (2014) 1550-7998=2014=90(6)=064045 (11) 064045-1

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Section: Introductionmentioning

confidence: 57%

Gravity waves from extreme-mass-ratio plunges into Kerr black holes

2014

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“…In particular, the curves for mass ratios ¼ 10 À4;À5;À6 are almost superposed, which points out that radiation reaction has little effect during the plunge phase for these binaries. This fact suggests that, when & 10 À4 , the motion is ''quasigeodesic'' around and below LSO crossing [10], i.e., it is a good approximation to the geodesic plunge from the LSO [17,23,119,121].…”

Section: Angular Momentum Lossmentioning

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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“…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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Post-innermost stable circular orbit ringdown amplitudes in extreme mass ratio inspiral

Cited by 23 publications

References 30 publications

Gravity waves from extreme-mass-ratio plunges into Kerr black holes

Gravity waves from extreme-mass-ratio plunges into Kerr black holes

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

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

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