Practical formula for the radiated angular momentum

Lousto, Carlos O.; Zlochower, Yosef

doi:10.1103/physrevd.76.041502

Cited by 65 publications

(87 citation statements)

References 21 publications

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“…The formulae in Refs. [81,82] are valid at r = ∞. We obtain highly accurate values for these quantities by solving for them on spheres of finite radius (typically r/M = 25, 30, 35, 40), fitting the results to a polynomial dependence in l = 1/r, and extrapolating to l = 0.…”

Section: Numerical Techniquesmentioning

confidence: 99%

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Extra-large remnant recoil velocities and spins from near-extremal-Bowen-York-spin black-hole binaries

2008

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We evolve equal-mass, equal-spin black-hole binaries with specific spins of a/mH ∼ 0.925, the highest spins simulated thus far and nearly the largest possible for Bowen-York black holes, in a set of configurations with the spins counter-aligned and pointing in the orbital plane, which maximizes the recoil velocities of the merger remnant, as well as a configuration where the two spins point in the same direction as the orbital angular momentum, which maximizes the orbital hang-up effect and remnant spin. The coordinate radii of the individual apparent horizons in these cases are very small and the simulations require very high central resolutions (h ∼ M/320). We find that these highly spinning holes reach a maximum recoil velocity of ∼ 3300 km s −1 (the largest simulated so far) and, for the hangup configuration, a remnant spin of a/mH ∼ 0.922. These results are consistent with our previous predictions for the maximum recoil velocity of ∼ 4000 km s −1 and remnant spin; the latter reinforcing the prediction that cosmic censorship is not violated by merging highlyspinning black-hole binaries. We also numerically solve the initial data for, and evolve, a single maximal-Bowen-York-spin black hole, and confirm that the 3-metric has an O(r −2 ) singularity at the puncture, rather than the usual O(r −4 ) singularity seen for non-maximal spins.

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Section: Numerical Techniquesmentioning

confidence: 99%

“…[81,82]. However, rather than using the full ψ 4 we decompose it into ℓ and m modes and solve for the radiated linear momentum, dropping terms with ℓ ≥ 5.…”

Section: Numerical Techniquesmentioning

confidence: 99%

Extra-large remnant recoil velocities and spins from near-extremal-Bowen-York-spin black-hole binaries

2008

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“…This is of particular interest because it is most closely related to the rates of emission of gravitational-wave energy and linear momentum [60,61]. As with the strain and ψ 4 , the strain-rate can be decomposed into spherical harmonics:…”

Section: Simulationsmentioning

confidence: 99%

Mergers of black-hole binaries with aligned spins: Waveform characteristics

et al. 2011

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We conduct a descriptive analysis of the multipolar structure of gravitational-radiation waveforms from equal-mass aligned-spin mergers, following an approach first presented in the complementary context of nonspinning black holes of varying mass ratio [1]. We find that, as with the nonspinning mergers, the dominant waveform mode phases evolve together in lock-step through inspiral and merger, supporting the previous waveform description in terms of an adiabatically rigid rotator driving gravitational-wave emission -an implicit rotating source (IRS). We further apply the latetime merger-ringdown model for the rotational frequency introduced in [1], along with an improved amplitude model appropriate for the dominant (2, ±2) modes. This provides a quantitative description of the merger-ringdown waveforms, and suggests that the major features of these waveforms can be described with reference only to the intrinsic parameters associated with the state of the final black hole formed in the merger. We provide an explicit model for the merger-ringdown radiation, and demonstrate that this model agrees to fitting factors better than 95% with the original numerical waveforms for system masses above ∼ 150M⊙. This model may be directly applicable to gravitational-wave detection of intermediate-mass black hole mergers.

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“…[25,26,27,28,29,30,31,32]), and first results for certain configurations with spin have also become available [33,34]. In order to overcome phase inaccuracies in long evolutions, significant progress has been made by the Caltech-Cornell group using spectral codes [35,36], and by the Jena group using higher (sixth) order finite differencing [37].…”

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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Practical formula for the radiated angular momentum

Cited by 65 publications

References 21 publications

Extra-large remnant recoil velocities and spins from near-extremal-Bowen-York-spin black-hole binaries

Extra-large remnant recoil velocities and spins from near-extremal-Bowen-York-spin black-hole binaries

Mergers of black-hole binaries with aligned spins: Waveform characteristics

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

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