Beyond the Bowen–York extrinsic curvature for spinning black holes

Hannam, M. D.; Husa, S.; Bruegmann, Bernd; González, José Antonio García-Cruces; Sperhake, Ulrich

doi:10.1088/0264-9381/24/12/s02

Cited by 44 publications

(66 citation statements)

References 50 publications

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“…In practice, the amount of "junk radiation" associated with these initial data sets increases with the magnitude of the spin of the hole. The amount of this extra radiation has been studied perturbatively by Gleiser et al [30] and numerically by Hannam et al [31] and Dain et al [32]. The last shows that, for the case s/m 2 = 0.90, a single BY black hole would relax into a Kerr black hole after emitting about 0.1% of the initial gravitational mass.…”

Section: Resultsmentioning

confidence: 97%

High-spin binary black hole mergers

Marronetti

Tichy

Brügmann³

et al. 2008

Phys. Rev. D

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We study identical mass black hole binaries with spins perpendicular to the binary's orbital plane. These binaries have individual spins ranging from s/m 2 = −0.90 to 0.90, (s1 = s2 in all cases) which is near the limit possible with standard Bowen-York puncture initial data. The extreme cases correspond to the largest initial spin simulations to date. Our results expand the parameter space covered by Rezzolla et al. and, when combining both data sets, we obtain estimations for the minimum and maximum values for the intrinsic angular momenta of the remnant of binary black hole mergers of J/M 2 = 0.341 ± 0.004 and 0.951 ± 0.004 respectively. Note, however, that these values are reached through extrapolation to the singular cases |s1| = |s2| = 1 and thus remain as estimates until full-fledged numerical simulations provide confirmation.

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Section: Resultsmentioning

confidence: 97%

High-spin binary black hole mergers

Marronetti

Tichy

Brügmann³

et al. 2008

Phys. Rev. D

Self Cite

181

219

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“…Most codes in the field (including BAM and SpEC) primarily use conformally flat initial data, which limits the BH spins to a/m ∼ 0.92 [43][44][45]. There has been some work in constructing high-spin data for puncture codes like BAM [46,47], but to date no waveforms for long-term quasi-circular inspirals have been published. For the SpEC code, however, high-spin data have been produced and used in production simulations, based on a superposition of Kerr-Schild data [36,44,48].…”

Section: B Numerical Relativity Waveformsmentioning

confidence: 99%

Frequency-domain gravitational waves from nonprecessing black-hole binaries. I. New numerical waveforms and anatomy of the signal

et al. 2016

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In this paper we discuss the anatomy of frequency-domain gravitational-wave signals from non-precessing black-hole coalescences with the goal of constructing accurate phenomenological waveform models. We first present new numerical-relativity simulations for mass ratios up to 18, including spins. From a comparison of different post-Newtonian approximants with numerical-relativity data we select the uncalibrated SEOBNRv2 model as the most appropriate for the purpose of constructing hybrid post-Newtonian/numerical-relativity waveforms, and we discuss how we prepare time-domain and frequency-domain hybrid data sets. We then use our data together with results in the literature to calibrate simple explicit expressions for the final spin and radiated energy. Equipped with our prediction for the final state we then develop a simple and accurate mergerringdown-model based on modified Lorentzians in the gravitational wave amplitude and phase, and we discuss a simple method to represent the low frequency signal augmenting the TaylorF2 post-Newtonian approximant with terms corresponding to higher orders in the post-Newtonian expansion. We finally discuss different options for modelling the small intermediate frequency regime between inspiral and merger-ringdown. A complete phenomenological model based on the present work is presented in a companion paper [1].

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“…Conformally-curved initial data has been found to reduce the amount of spurious radiation in Refs. [39,66].…”

Section: Suitability For Evolutionsmentioning

confidence: 99%

Binary-black-hole initial data with nearly extremal spins

et al. 2008

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There is a significant possibility that astrophysical black holes with nearly-extremal spins exist. Numerical simulations of such systems require suitable initial data. In this paper, we examine three methods of constructing binary-black-hole initial data, focusing on their ability to generate black holes with nearly-extremal spins: (i) Bowen-York initial data, including standard puncture data (based on conformal flatness and Bowen-York extrinsic curvature), (ii) standard quasi-equilibrium initial data (based on the extended-conformal-thin-sandwich equations, conformal flatness, and maximal slicing), and (iii) quasi-equilibrium data based on the superposition of Kerr-Schild metrics. We find that the two conformally-flat methods (i) and (ii) perform similarly, with spins up to about 0.99 obtainable at the initial time. However, in an evolution, we expect the spin to quickly relax to a significantly smaller value around 0.93 as the initial geometry relaxes. For quasi-equilibrium superposed Kerr-Schild (SKS) data [method (iii)], we construct initial data with initial spins as large as 0.9997. We evolve SKS data sets with spins of 0.93 and 0.97 and find that the spin drops by only a few parts in 10 4 during the initial relaxation; therefore, we expect that SKS initial data will allow evolutions of binary black holes with relaxed spins above 0.99. Along the way to these conclusions, we also present several secondary results: the power-law coefficients with which the spin of puncture initial data approaches its maximal possible value; approximate analytic solutions for large spin puncture data; embedding diagrams for single spinning black holes in methods (i) and (ii); non-unique solutions for method (ii). All of the initial data sets that we construct contain sub-extremal black holes, and when we are able to push the spin of the excision boundary surface into the super-extremal regime, the excision surface is always enclosed by a second, sub-extremal apparent horizon. The quasilocal spin is measured by using approximate rotational Killing vectors, and the spin is also inferred from the extrema of the intrinsic scalar curvature of the apparent horizon. Both approaches are found to give consistent results, with the approximate-Killing-vector spin showing least variation during the initial relaxation.

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Beyond the Bowen–York extrinsic curvature for spinning black holes

Cited by 44 publications

References 50 publications

High-spin binary black hole mergers

High-spin binary black hole mergers

Frequency-domain gravitational waves from nonprecessing black-hole binaries. I. New numerical waveforms and anatomy of the signal

Binary-black-hole initial data with nearly extremal spins

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