Toroidal horizons in binary black hole inspirals

Cohen, Michael; Kaplan, Jeffrey D.; Scheel, Mark A.

doi:10.1103/physrevd.85.024031

Cited by 15 publications

(16 citation statements)

References 25 publications

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“…Speaking in a paradoxical manner purposely, rather wandering null geodesics might determine the definite mathematical concept for the topology of the event horizon, e.g. the binary of black holes [35,44,[49][50][51][52].…”

Section: Discussion: Binary Black Holementioning

confidence: 99%

Black hole shadow and Wandering null geodesics

Siino

2021

Preprint

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The role of the wandering null geodesic is studied in a black hole spacetime. Based on the continuity of the solution of the geodesic equation, the wandering null geodesics commonly exist and explain the typical phenomena of the optical observation of event horizons. Moreover, a new concept of 'black room' is investigated to relate the wandering null geodesic to the black hole shadow more closely.

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Section: Discussion: Binary Black Holementioning

confidence: 99%

Black hole shadow and Wandering null geodesics

Siino

2021

Preprint

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“…If we compactify the large black hole horizon by adding the points at infinity (so that at early and late times its topology is spherical), we can say that these sections of the merger horizon have the topology of a torus. The occurrence of toroidal topology in the spatial sections of a generic, non-axisymmetric event horizon during the instants close to merger has been observed and discussed in [2,3,5,9,15,16,17,18,19]. These toroidal spatial sections of the event horizon are actually a gauge-dependent feature, since one can always choose different spacelike slicings where the topology remains spherical.…”

Section: Constant-time Slices and Toroidal Topologymentioning

confidence: 99%

Black hole fusion in the extreme mass ratio limit

Montero

Zilhão

2018

Phys. Rev. D

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We present a simple, general, and accurate construction of the event horizons for the fusion of two neutral, rotating black holes with arbitrary orientation and values of their spins, in the extreme mass ratio limit where one black hole is much larger than the other. We compute several parameters that characterize the fusion and investigate their dependence on the black hole spin and orientation axis. We also exhibit and study the appearance of transient toroidal topology of the horizon. An earlier conjecture about universal critical exponents before and after an axisymmetric pinch is proven.

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“…Following this, we can explore spinning [24,58] and eccentric [59,60] binaries, where modified first laws hold. A second direction of study is to investigate the redshift factor on the actual EHs of BH spacetimes, although this requires intensive postprocessing [61,62]. One could also improve the extraction of the redshift by developing a method to compute the best approximate HKV at each time step, analogous to the method used in SpEC to compute BH spins [57,[63][64][65].…”

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confidence: 99%

Redshift Factor and the First Law of Binary Black Hole Mechanics in Numerical Simulations

2016

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The redshift factor z is an invariant quantity of fundamental interest in post-Newtonian and selfforce descriptions of compact binaries. It connects different approximation schemes, and plays a central role in the first law of binary black hole mechanics, which links local quantities to asymptotic measures of energy and angular momentum in these systems. Through this law, the redshift factor is conjectured to have a close relation to the surface gravity of the event horizons of black holes in circular orbits. We propose and implement a novel method for extracting the redshift factor on apparent horizons in numerical simulations of quasicircular binary inspirals. Our results confirm the conjectured relationship between z and the surface gravity of the holes and that the first law holds to a remarkable degree for binary inspirals. The redshift factor enables tests of analytic predictions for z in spacetimes where the binary is only approximately circular, giving a new connection between analytic approximations and numerical simulations.Introduction.-The relativistic two body problem is of fundamental importance in both general relativity and the astrophysics of compact objects. Compact binaries emit gravitational radiation and inspiral, eventually merging in a dynamic, nonlinear process. These mergers are the most promising sources of gravitational waves and provide a window into untested regimes of physics. The landmark detection of binary black hole (BH) mergers through gravitational waves [1-3] highlights both the sophistication of waveform models and the need for further improvements to search for and interpret gravitational wave signals. Current methods include post-Newtonian (PN) expansions in the slow velocity regime [4], selfforce (SF) approximations [5] for systems with high mass ratios, and direct numerical solutions [6][7][8] of inspirals beginning tens of orbits before merger. Each method has its limitations, and they are combined into effective one body (EOB) [9,10] and phenomenological waveform models [11]. In addition, connections and comparisons between the different approaches yield new insights into each of them [12,13]. Such insights deepen our understanding of relativity and maximize the scientific benefits of future gravitational wave observations. Invariant quantities play a crucial role in these comparisons, since each method uses different gauges and various approximation schemes. The invariant redshift factor z has proven essential in comparisons between analytic approximations, as first discussed for circular binaries [14]. Such systems remain stationary in the corotating frame, having a helical symmetry embodied in a helical Killing vector (HKV) K µ . In this context, the redshift factor allows for comparison of results obtained in distinct coordinate gauges [15,16], and has played a central role in the development of PN and EOB theory using SF, e.g. Refs. [17][18][19].For isolated BHs, the laws of black hole mechanics are relations between the area, angular momentum, and charge of the h...

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Toroidal horizons in binary black hole inspirals

Cited by 15 publications

References 25 publications

Black hole shadow and Wandering null geodesics

Black hole shadow and Wandering null geodesics

Black hole fusion in the extreme mass ratio limit

Redshift Factor and the First Law of Binary Black Hole Mechanics in Numerical Simulations

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