Quasi-local Black Hole Horizons

Krishnan, B.

doi:10.1007/978-3-662-46035-1_25

Cited by 7 publications

(11 citation statements)

References 66 publications

(106 reference statements)

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“…Quantum effects [1,4,[6][7][8][9][10][11][12] add additional complexity. Event horizons may become optional [4,10,13], and the notion of a black hole (BH) is then tied with one of the locally or quasilocally defined surfaces, such as an apparent horizon [14,15]. Hawking radiation accompanies the formation and evolution of black holes [16].…”

Section: Introductionmentioning

confidence: 99%

Energy-momentum tensor and metric near the Schwarzschild sphere

et al. 2019

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Regularity of the horizon radius rg of a collapsing body constrains a limiting form of a spherically symmetric energy-momentum tensor near it. Its nonzero limit belongs to one of four classes that are distinguished only by two signs. As a result, close to rg the geometry can always be described by either an ingoing or outgoing Vaidya metric with increasing or decreasing mass. If according to a distant outside observer the trapped regions form in finite time, then the Einstein equations imply violation of the null energy condition. In this case the horizon radius and its rate of change determine the metric in its vicinity, and the hypersurface r = rg(t) is timelike during both the expansion and contraction of the trapped region. We present the implications of these results for the firewall paradox and discuss arguments that the required violation of the null energy condition is incompatible with the standard analysis of black hole evaporation.

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Section: Introductionmentioning

confidence: 99%

Energy-momentum tensor and metric near the Schwarzschild sphere

et al. 2019

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“…A trapped region -a spacetime domain where both radial null geodesics have negative expansion -forms inside the collapsing matter. Its suitably defined outer boundary (i.e., the apparent horizon or another related surface) asymptotically approaches the event horizon [1][2][3][4][5][6].…”

Section: Introductionmentioning

confidence: 99%

Black hole evaporation and semiclassical thin shell collapse

2019

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In case of spherical symmetry, the assumptions of finite-time formation of a trapped region and regularity of its boundary -the apparent horizon -are sufficient to identify the form of the metric and energy-momentum tensor in its vicinity. By comparison with the known results for quasistatic evaporation of black holes, we complete the identification of their parameters. Consistency of the Einstein equations allows only two possible types of higher-order terms in the energy-momentum tensor. By using its local conservation, we provide a method of calculation of the higher-order terms, explicitly determining the leading-order regular corrections. Contraction of a spherically symmetric thin dust shell is the simplest model of gravitational collapse. Nevertheless, the inclusion of a collapse-triggered radiation in different extensions of this model leads to apparent contradictions. Using our results, we resolve these contradictions and show how gravitational collapse may be completed in finite time according to a distant observer.

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“…The world tube traced out by a MOTS during time evolution can be used to study energy fluxes, the evolution of mass, angular momentum and higher multipole mo-ments [4,18,22,28,41]. The world tube can be used as an inner boundary for Hamiltonian calculations, and the laws of BH mechanics hold [8,10,12,21,25,27,29]. In general the world tubes can be null, spacelike, timelike, or of mixed signature [5-8, 11, 12].…”

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confidence: 99%

Interior of a Binary Black Hole Merger

et al. 2019

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We find strong numerical evidence for a new phenomenon in a binary black hole spacetime, namely the merger of marginally outer trapped surfaces (MOTSs). By simulating the head-on collision of two nonspinning unequal mass black holes, we observe that the MOTS associated with the final black hole merges with the two initially disjoint surfaces corresponding to the two initial black holes. This yields a connected sequence of MOTSs interpolating between the initial and final state all the way through the non-linear binary black hole merger process. In addition, we show the existence of a MOTS with self-intersections formed immediately after the merger. This scenario now allows us to track physical quantities (such as mass, angular momentum, higher multipoles, and fluxes) across the merger, which can be potentially compared with the gravitational wave signal in the wave-zone, and with observations by gravitational wave detectors. This also suggests a possibility of proving the Penrose inequality mathematically for generic astrophysical binary back hole configurations.

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Quasi-local Black Hole Horizons

Cited by 7 publications

References 66 publications

Energy-momentum tensor and metric near the Schwarzschild sphere

Energy-momentum tensor and metric near the Schwarzschild sphere

Black hole evaporation and semiclassical thin shell collapse

Interior of a Binary Black Hole Merger

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