Note on trapped surfaces in the Vaidya solution

Bengtsson, Ingemar; Senovilla, José M. M.

doi:10.1103/physrevd.79.024027

Cited by 42 publications

(89 citation statements)

References 12 publications

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“…Closed trapped surface cannot be found entirely in a flat spacetime. However, parts of a closed marginally trapped surface can be found passing through a region of flat space where both null expansions are negative [21].…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…The Vaidya solutions have a number of nice properties that make them popular for investigations of this type [19][20][21]. The Vaidya spacetimes [28] are a class of spherically symmetric, non-vacuum spacetimes with line element in advanced null Eddington-Finkelstein coordinates (v, r, θ, φ):…”

Section: The Vaidya Metricmentioning

confidence: 99%

“…It was also shown that there are flat regions inside the event horizon (the region contained within the shell) where no trapped surface passes. Bengtsson and Senovilla [21] analytically constructed trapped surfaces that pass through the flat region. This is not a contradiction; while there are some flat regions where no trapped surface can be located, there are trapped surfaces in other parts of the flat region.…”

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confidence: 99%

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Slicing dependence of nonspherically symmetric quasilocal horizons in Vaidya spacetimes

et al. 2011

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It is well known that quasi-local black hole horizons depend on the choice of a time coordinate in a spacetime. This has implications for notions such as the surface of the black hole and also on quasi-local physical quantities such as horizon measures of mass and angular momentum. In this paper, we compare different horizons on non-spherically symmetric slicings of Vaidya spacetimes. The spacetimes we investigate include both accreting and evaporating black holes. For some simple choices of the Vaidya mass function function corresponding to collapse of a hollow shell, we compare the area for the numerically found axisymmetric trapping horizons with the area of the spherically symmetric trapping horizon and event horizon. We find that as expected, both the location and area are dependent on the choice of foliation. However, the area variation is not large, of order 0.017% for a slowly evolving horizon withṁ = 0.02. We also calculate analytically the difference in area between the spherically symmetric quasi-local horizon and event horizon for a slowly accreting black hole. We find that the difference can be many orders of magnitude larger than the Planck area for sufficiently large black holes.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Section: The Vaidya Metricmentioning

confidence: 99%

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confidence: 99%

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Slicing dependence of nonspherically symmetric quasilocal horizons in Vaidya spacetimes

et al. 2011

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“…VAIDYA'S SPACETIME The Vaidya's spacetime with an ingoing null dust usually written in the form [32],…”

Section: General Covariant Hořava-lifshitz Gravity With Minimum Cmentioning

confidence: 99%

Vaidya solution in general covariant Hořava–Lifshitz gravity with the minimum coupling and without projectability: Infrared limit

Goldoni

Silva

Chan

et al. 2015

Int. J. Mod. Phys. D

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In this paper, we have studied nonstationary radiative spherically symmetric spacetime, in general covariant theory (U (1) extension) of the Hořava-Lifshitz gravity with the minimum coupling, in the post-newtonian approximation (PPN), without the projectability condition and in the infrared limit. The Newtonian prepotential ϕ was assumed null. We have shown that there is not the analogue of the Vaidya's solution in the Hořava-Lifshitz Theory (HLT) with the minimum coupling, as we know in the General Relativity Theory (GRT).

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“…Using this Ansatz, we solve the problem of transforming the Vaidya metric to the diagonal coordinates fully analytically by calculating all metric coefficients. Vaidya metric (1) with a linear mass function has been considered previously in a large number of publications in various aspects [4,5,[32][33][34][35][36]. However, the form of the Vaidya metric in diagonal coordinates was not obtained in these publications.…”

Section: Introductionmentioning

confidence: 99%

Vaidya spacetime in the diagonal coordinates

Berezin

Dokuchaev

Eroshenko

2017

J. Exp. Theor. Phys.

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We have analyzed the transformation from initial coordinates (v, r) of the Vaidya metric with light coordinate v to the most physical diagonal coordinates (t, r). An exact solution has been obtained for the corresponding metric tensor in the case of a linear dependence of the mass function of the Vaidya metric on light coordinate v. In the diagonal coordinates, a narrow region (with a width proportional to the mass growth rate of a black hole) has been detected near the visibility horizon of the Vaidya accreting black hole, in which the metric differs qualitatively from the Schwarzschild metric and cannot be represented as a small perturbation. It has been shown that, in this case, a single set of diagonal coordinates (t, r) is insufficient to cover the entire range of initial coordinates (v, r) outside the visibility horizon; at least three sets of diagonal coordinates are required, the domains of which are separated by singular surfaces on which the metric components have singularities (either g00 = 0 or g00 = ∞.). The energy-momentum tensor diverges on these surfaces; however, the tidal forces turn out to be finite, which follows from an analysis of the deviation equations for geodesics. Therefore, these singular surfaces are exclusively coordinate singularities that can be referred to as false firewalls because there are no physical singularities on them. We have also considered the transformation from the initial coordinates to other diagonal coordinates (η, y), in which the solution is obtained in explicit form, and there is no energy-momentum tensor divergence.

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Note on trapped surfaces in the Vaidya solution

Cited by 42 publications

References 12 publications

Slicing dependence of nonspherically symmetric quasilocal horizons in Vaidya spacetimes

Slicing dependence of nonspherically symmetric quasilocal horizons in Vaidya spacetimes

Vaidya solution in general covariant Hořava–Lifshitz gravity with the minimum coupling and without projectability: Infrared limit

Vaidya spacetime in the diagonal coordinates

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