Collision of two black holes

Anninos, Peter; Hobill, David; Seidel, Edward; Smarr, Larry; Suen, Wai-Mo

doi:10.1103/physrevlett.71.2851

Cited by 213 publications

(288 citation statements)

References 12 publications

(10 reference statements)

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“…on a 3-dimensional spacelike hypersurface) and are then stepped to the next instant using an "ADM" [2] form of the Einstein evolution equations [3]. The evolution is unconstrained, and maintenance of the constraint functions with small error is verified throughout the run.This work extends previous work on headon encounters [4][5][6][7]. It is comparable to recent results of Brügmann [8]: non-headon black hole evolution through to significant interaction and merger.…”

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confidence: 80%

Grazing Collisions of Black Holes via the Excision of Singularities

et al. 2000

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We present the first simulations of non-headon (grazing) collisions of binary black holes in which the black hole singularities have been excised from the computational domain. Initially two equal mass black holes m are separated a distance ≈ 10m and with impact parameter ≈ 2m. Initial data are based on superposed, boosted (velocity ≈ 0.5c) solutions of single black holes in Kerr-Schild coordinates. Both rotating and non-rotating black holes are considered. The excised regions containing the singularities are specified by following the dynamics of apparent horizons. Evolutions of up to t ≈ 35m are obtained in which two initially separate apparent horizons are present for t ≈ 3.8m. At that time a single enveloping apparent horizon forms, indicating that the holes have merged. Apparent horizon area estimates suggest gravitational radiation of about 2.6% of the total mass. The evolutions end after a moderate amount of time because of instabilities.Introduction: Gravitational wave detectors [1] will soon begin searching for gravitational radiation from astrophysical binary compact objects. To understand these observations, and to predict parameter regimes in which to search for their radiation, efforts are underway to model the interaction of compact sources. We report here a direct numerical simulation of interacting spinning black hole binaries, in genuinely hyperbolic (nonheadon) trajectories. The initial spin angular momenta evolved here are either zero, or parallel to each other and perpendicular to the orbital plane. The interior of the equal mass holes and their interior singularities are excised from the computation. (Our method is neither restricted to equal masses nor to parallel spins). Evolution is carried out in a Cauchy scheme, in which the state of the gravitational system (the 3-spatial metric g ab ) and its rate of change (the 3-spatial extrinsic curvature K ab ) are specified at one instant (i.e. on a 3-dimensional spacelike hypersurface) and are then stepped to the next instant using an "ADM" [2] form of the Einstein evolution equations [3]. The evolution is unconstrained, and maintenance of the constraint functions with small error is verified throughout the run.This work extends previous work on headon encounters [4][5][6][7]. It is comparable to recent results of Brügmann [8]: non-headon black hole evolution through to significant interaction and merger. But our approach has a novel feature: the singularity-excising character of the computation of generic encounters which allows "natural" motion of the black holes through the computational

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confidence: 80%

Grazing Collisions of Black Holes via the Excision of Singularities

et al. 2000

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“…For instance, consider the good agreement between numerical relativity simulations of equal-mass BH collisions and the point-particle extrapolations to equal-mass systems. In D = 4, early work [42] and more recent simulations (see e.g. [21]) found that the TABLE I.…”

Section: Resultsmentioning

confidence: 99%

Radiation from particles with arbitrary energy falling into higher-dimensional black holes

2011

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We consider point particles with arbitrary energy per unit mass E that fall radially into a higherdimensional, nonrotating, asymptotically flat black hole. We compute the energy and linear momentum radiated in this process as functions of E and of the spacetime dimensionality D = n + 2 for n = 2, . . . , 9 (in some cases we go up to 11). We find that the total energy radiated increases with n for particles falling from rest (E = 1). For fixed particle energies 1 < E ≤ 2 we show explicitly that the radiation has a local minimum at some critical value of n, and then it increases with n. We conjecture that such a minimum exists also for higher particle energies. The present point-particle calculation breaks down when n = 11, because then the radiated energy becomes larger than the particle mass. Quite interestingly, for n = 11 the radiated energy predicted by our calculation would also violate Hawking's area bound. This hints at a qualitative change in gravitational radiation emission for n 11. Our results are in very good agreement with numerical simulations of low-energy, unequal-mass black hole collisions in D = 5 (that will be reported elsewhere) and they are a useful benchmark for future nonlinear evolutions of the higher-dimensional Einstein equations.

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“…For example, if the black hole is small, we expect to find in the gravitational radiation spectra a strong peak located at ω 2 = 4n 2 + l(l + 1) , n = 1, 2, ... [5]. Moreover, some major results in perturbation theory and numerical relativity [27,28], studying the collision of two black holes, with masses of the same order of magnitude, allow us to infer that evolving the collision of two black holes in AdS spacetime, should not bring major differences in relation to our results (though it is of course a much more difficult task, even in perturbation theory). In particular, in the small black hole regime, the spectra and waveforms should be dominated by quasinormal ringing.…”

Section: Discussionmentioning

confidence: 99%

Black hole collision with a scalar particle in four-, five-, and seven-dimensional anti–de Sitter spacetimes: Ringing and radiation

Cardoso¹,

Lemos²

2002

Phys. Rev. D

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In this work we compute the spectra, waveforms and total scalar energy radiated during the radial infall of a small test particle coupled to a scalar field into a d-dimensional Schwarzschild-anti-de Sitter black hole. We focus on d = 4, 5 and 7, extending the analysis we have done for d = 3. For small black holes, the spectra peaks strongly at a frequency ω ∼ d−1, which is the lowest pure antide Sitter (AdS) mode. The waveform vanishes exponentially as t → ∞, and this exponential decay is governed entirely by the lowest quasinormal frequency. This collision process is interesting from the point of view of the dynamics itself in relation to the possibility of manufacturing black holes at LHC within the brane world scenario, and from the point of view of the AdS/CFT conjecture, since the scalar field can represent the string theory dilaton, and 4, 5, 7 are dimensions of interest for the AdS/CFT correspondence.

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Collision of two black holes

Cited by 213 publications

References 12 publications

Grazing Collisions of Black Holes via the Excision of Singularities

Grazing Collisions of Black Holes via the Excision of Singularities

Radiation from particles with arbitrary energy falling into higher-dimensional black holes

Black hole collision with a scalar particle in four-, five-, and seven-dimensional anti–de Sitter spacetimes: Ringing and radiation

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