Energy and angular momentum radiated for non-head-on binary black hole collisions

Moreschi, Osvaldo M.; Pérez, Alejandro; Lehner, Luis

doi:10.1103/physrevd.66.104017

Cited by 6 publications

(3 citation statements)

References 40 publications

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“…In order to validate this suggestion, we analyzed a family of Robinson-Trautman (RT) spacetimes [33,34], representing an (eternal) BH together with purely outgoing gravitational radiation. The mathematical properties of this class of exact solutions is already well understood [37][38][39][40], therefore this spacetime is a good test for numerical schemes [41,42] and it is an excellent toy model for problems dealing with radiation in BH environments [43][44][45][46][47][48][49][50][51][52][53][54]. Although the associated BH horizon is stationary, these RT spacetimes also contain a white-hole horizon H − [40,[55][56][57], or, more precisely, a past outer-trapping horizon [58], whose dynamics offers a particularly well-suited scenario to test our geometric approach.…”

Section: The Cross-correlation Approach: An Executive Summarymentioning

confidence: 99%

Black-hole horizons as probes of black-hole dynamics. I. Post-merger recoil in head-on collisions

et al. 2012

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The understanding of strong-field dynamics near black-hole horizons is a long-standing and challenging problem in general relativity. Recent advances in numerical relativity and in the geometric characterization of blackhole horizons open new avenues into the problem. In this first paper in a series of two, we focus on the analysis of the recoil occurring in the merger of binary black holes, extending the analysis initiated in [1] with RobinsonTrautman spacetimes. More specifically, we probe spacetime dynamics through the correlation of quantities defined at the black-hole horizon and at null infinity. The geometry of these hypersurfaces responds to bulk gravitational fields acting as test screens in a scattering perspective of spacetime dynamics. Within a 3 + 1 approach we build an effective-curvature vector from the intrinsic geometry of dynamical-horizon sections and correlate its evolution with the flux of Bondi linear momentum at large distances. We employ this setup to study numerically the head-on collision of nonspinning black holes and demonstrate its validity to track the qualitative aspects of recoil dynamics at infinity. We also make contact with the suggestion that the antikick can be described in terms of a "slowness parameter" and how this can be computed from the local properties of the horizon. In a companion paper [2] we will further elaborate on the geometric aspects of this approach and on its relation with other approaches to characterize dynamical properties of black-hole horizons.

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Section: The Cross-correlation Approach: An Executive Summarymentioning

confidence: 99%

Black-hole horizons as probes of black-hole dynamics. I. Post-merger recoil in head-on collisions

et al. 2012

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“…Recent numerical results suggest that the Robinson-Trautman metrics can be used to estimate the mass loss during the final phase of the collision of two black holes. 2 There are also suggestions that the subclass of the so called C-metrics 3 (and their twisting generalizations 4 ) can describe spacetimes containing accelerating black holes. [5][6][7][8] In terms of standard coordinates u, r, ξ, ξ, where u and r are real and ξ is complex, the Robinson-Trautman metrics are given by 9 g = 2du(Hdu + dr) − 2r 2 P −2 dξd ξ .…”

Section: Introductionmentioning

confidence: 99%

Symmetries of the Robinson-Trautman equation

Natorf¹,

Tafel²

2006

Journal of Mathematical Physics

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“…If one wants to generalize these estimates to the case of the black hole collision with orbital angular momentum it is necessary to consider spacetimes with total angular momentum. This is the main physical motivation for this work; the application of these calculations to specific physical models will be presented elsewhere [15].…”

Section: Introductionmentioning

confidence: 99%