Beyond lensing by the cosmological constant

Faraoni, Valerio; Lapierre-Léonard, Marianne

doi:10.1103/physrevd.95.023509

Cited by 39 publications

(57 citation statements)

References 60 publications

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“…First, before the critical time at which the black hole/cosmological AH pair is created, there is a naked singularity and this solution of the Einstein equations cannot be obtained as the development of regular Cauchy data. Second, AHs ultimately depend on the foliation [51], although all spherically symmetric foliations (the only ones of practical importance here) determine the same AHs [52]. Third, while the RN solution is the most general spherical and locally static electrovacuum solution of the Einstein equations with positive Λ, in the presence of a fluid there is no general solution and the charged Thahurta and McVittie geometries cannot claim such a degree of generality.…”

Section: Discussionmentioning

confidence: 95%

“…However, AHs are foliation-dependent, as exemplified dramatically by the fact that in the Schwarzschild spacetime there exist foliations without AHs [51]. This problem is somehow alleviated by the recent realization that, in spherical symmetry, all spherically symmetric foliations (to which we restrict here) possess the same AHs [52]. In any case, the recent detections of gravitational waves from black hole mergers by the LIGO interferometers [53] are based in an essential way on the use of marginally trapped surfaces and AHs.…”

Section: Cauchy Horizon Of Charged Black Holes and Determinism In Grmentioning

confidence: 95%

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Conformal cosmological black holes: Towards restoring determinism to Einstein theory

2019

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A widespread solution-generating technique of general relativity consists of conformally transforming known "seed" solutions. It is shown that these new solutions always solve the field equations of a pathological Brans-Dicke theory. Furthermore, when interpreted as effective Einstein equations, those field equations exhibit, in the case of a cosmological "background", an induced imperfect fluid as an additional effective source besides the original sources of the "seed" solutions. As an application, the charged non-rotating Thakurta black hole conformal to Reissner-Nordström is used to demonstrate the fragility of the inner Cauchy horizon when this black hole is embedded in the universe (even accounting for the separation of black hole and Hubble scales). Similarly, the charged McVittie spacetime representing a charged black hole embedded in a cosmological "background" with varying Hubble parameter does not exhibit a real Cauchy horizon. These arguments speak in favor of restoring determinism to Einstein theory, which was questioned in recent research. * fhammad@ubishops.ca † dkazici@ubishops.ca, dkazici@nku.edu.tr ‡ vfaraoni@ubishops.ca 1 We use the notations of Ref. [1].

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Section: Discussionmentioning

confidence: 95%

Section: Cauchy Horizon Of Charged Black Holes and Determinism In Grmentioning

confidence: 95%

Conformal cosmological black holes: Towards restoring determinism to Einstein theory

2019

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“…2pÃ Ω (20) in the tilded world. Not much should be construed from this complicated relation between tilded quantities: a conformal transformation with Ω = Ω (t, r) preserving the spherical symmetry has changed the situation in which Eq.…”

Section: Conformal Transformationsmentioning

confidence: 99%

Spacetime mappings of the Brown–York quasilocal energy

2019

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“…The chief objection raised is that, if one uses the cosmological McVittie description instead of the static geometry, there will be no light bending due to Λ at all, in the leading order. However, recently in [39], a non-vanishing contribution of Λ has been claimed for the McVittie spacetime, by using an effective local mass function. Thus it would be fair to admit that the debate is still far from being over.…”

Section: Introductionmentioning

confidence: 99%

Light bending, static dark energy, and related uniqueness of Schwarzschild–de Sitter spacetime

Ali

Bhattacharya

2018

Phys. Rev. D

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Since the Schwarzschild-de Sitter spacetime is static inside the cosmological event horizon, if the dark energy state parameter is sufficiently close to −1, apparently one could still expect an effectively static geometry, in the attraction dominated region inside the maximum turn around radius, RTA,max, of a cosmic structure. We take the first order metric derived recently assuming a static and ideal dark energy fluid with equation of state P (r) = αρ(r) as a source in Ref.[1], which reproduced the expression for RTA,max found earlier in the cosmological McVittie spacetime. Here we show that the equality originates from the equivalence of geodesic motion in these two backgrounds, in the nonrelativistic regime. We extend this metric up to the third order and compute the bending of light using the Rindler-Ishak method. For α = −1, a dark energy dependent term appears in the bending equation, unlike the case of the cosmological constant, α = −1. Due to this new term in particular, existing data for the light bending at galactic scales yields, (1 + α) O(10 −14 ), thereby practically ruling out any such static and inhomogeneous dark energy fluid we started with. Implication of this result pertaining the uniqueness of the Schwarzschild-de Sitter spacetime in such inhomogeneous dark energy background is discussed.

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Beyond lensing by the cosmological constant

Cited by 39 publications

References 60 publications

Conformal cosmological black holes: Towards restoring determinism to Einstein theory

Conformal cosmological black holes: Towards restoring determinism to Einstein theory

Spacetime mappings of the Brown–York quasilocal energy

Light bending, static dark energy, and related uniqueness of Schwarzschild–de Sitter spacetime

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