Gravitational lensing in the Simpson-Visser black-bounce spacetime in a strong deflection limit

Tsukamoto, Naoki

doi:10.1103/physrevd.103.024033

Cited by 78 publications

(25 citation statements)

References 144 publications

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“…Further research analysing SV spacetime has been performed in a plethora of other papers; please see reference 35 for details. These analyses include discussion of the quasi-normal modes and associated ringdown 36,37 , calculations pertaining to shadows and gravitational lensing effects [38][39][40][41][42][43] , as well as discourse surrounding precession phenomena 44 .…”

Section: Simpson-vissermentioning

confidence: 99%

Black-bounce to traversable wormhole

Simpson

Visser

2019

J. Cosmol. Astropart. Phys.

278

296

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So-called "regular black holes" are a topic currently of considerable interest in the general relativity and astrophysics communities. Herein we investigate a particularly interesting regular black hole spacetime described by the line elementThis spacetime neatly interpolates between the standard Schwarzschild black hole and the Morris-Thorne traversable wormhole; at intermediate stages passing through a black-bounce (into a future incarnation of the universe), an extremal null-bounce (into a future incarnation of the universe), and a traversable wormhole. As long as the parameter a is non-zero the geometry is everywhere regular, so one has a somewhat unusual form of "regular black hole", where the "origin" r = 0 can be either spacelike, null, or timelike. Thus this spacetime generalizes and broadens the class of "regular black holes" beyond those usually considered.

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Section: Simpson-vissermentioning

confidence: 99%

Black-bounce to traversable wormhole

Simpson

Visser

2019

J. Cosmol. Astropart. Phys.

278

296

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“…In the case a = 0 and m = 0, which corresponds to the Schwarzschild metric, the energy in the Møller prescription is equal to the ADM mass M. The obtained results for the Einstein energy E E and the Møller energy E M come to support the use of the Einstein and Møller prescriptions for the evaluation of the energy of a gravitational background, specifying that the positive energy regions can serve as a convergent gravitational lens, while the negative one can serve as a divergent gravitational lens [56]. In fact, the Simpson-Visser metric and its generalizations appear to be extremely advantageous for a deeper understanding of strong-field gravitational lensing of light reflected by a photon sphere of black holes and wormholes [55,[57][58][59]. Further, the small region of negativity in the expressions of the Einstein energy E E in the case a < 2m indicates some difficulty in the physically meaningful interpretation of the energy in certain regions of a specific space-time.…”

Section: Discussion and Concluding Remarksmentioning

confidence: 99%

Einstein and Møller Energy-Momentum Distributions for the Static Regular Simpson–Visser Space-Time

et al. 2021

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Energy-momentum localization for the four-dimensional static and spherically symmetric, regular Simpson–Visser black hole solution is studied by use of the Einstein and Møller energy-momentum complexes. According to the particular values of the parameter of the metric, the static Simpson–Visser solution can possibly describe the Schwarzschild black hole solution, a regular black hole solution with a one-way spacelike throat, a one-way wormhole solution with an extremal null throat, or a traversable wormhole solution of the Morris–Thorne type. In both prescriptions it is found that all the momenta vanish, and the energy distribution depends on the mass m, the radial coordinate r, and the parameter a of the Simpson–Visser metric. Several limiting cases of the results obtained are discussed, while the possibility of astrophysically relevant applications to gravitational lensing issues is pointed out.

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“…The most obvious, again, black hole thermodynamic since now they represent solutions with a sensible action principle with a clear field content 8 . On the other hand, it is possible to study several astrophysically relevant aspects of these black holes, as for example black hole shadows [75,76], gravitational lensing [77,78], black hole mimickers [79,80], quasinormal modes and echoes [81][82][83][84], to mention a few examples. We expect to report along these lines in our upcoming contributions.…”

Section: Conclusion and Further Developmentsmentioning

confidence: 99%

(A)dS Taub-NUT and exact black bounces with scalar hair

Barrientos¹,

Cisterna²,

Mora³

et al. 2022

Preprint

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We present a new family of exact four-dimensional Taub-NUT spacetimes in Einstein-Λ theory supplemented with a conformally coupled scalar field exhibiting a power-counting superrenormalizable potential. Our configurations are constructed in the following manner: A solution of a conformally coupled theory with a conformal potential, henceforth the seed (gµν , φ), is transformed by the action of a specific change of frame in addition with a simultaneous shift of the seed scalar field. The conformal factor of the transformation and the shift are both affine functions of the original scalar φ. The new configuration, (ḡµν , φ), solves the field equations of a conformally coupled theory with the extended aforementioned super-renormalizable potential, this under the presence of an effective cosmological constant. The new spectrum of solutions is notoriously enhanced with respect to the original seed containing regular black holes, wormholes, and bouncing cosmologies. We highlight the existence of two types of exact black bounces given by de Sitter and anti-de Sitter geometries that transit across three different configurations each. The de Sitter geometries transit from a regular black hole with event and cosmological horizons to a bouncing cosmology that connects two de Sitter Universes with different values of the asymptotic cosmological constant. An intermediate phase, which might be represented by two different configurations, takes place. These configurations are given by a de Sitter wormhole or by a bouncing cosmology that connects two de Sitter Universes, both under the presence of a cosmological horizon. On the other hand, the anti-de Sitter geometries transit from a regular black hole with inner and event horizons to a wormhole that connects two asymptotic boundaries with different constant curvatures. The intermediate phase is given in this case by an anti-de Sitter regular black hole with a single event horizon. This regular black hole might appear in two different configurations. As a regular anti-de Sitter black hole inside of an anti-de Sitter wormhole or as an anti-de Sitter regular black hole with a cosmological bounce in its interior. All these geometries are shown to be smoothly connected by the mass parameter only. Other standard stationary black holes, bouncing cosmologies and wormholes are also identified.

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Gravitational lensing in the Simpson-Visser black-bounce spacetime in a strong deflection limit

Abstract: We investigate gravitational lensing by a primary photon sphere which is formed by unstable circular light orbits, and by a secondary photon sphere on a wormhole throat in a black-bounce spacetime which is suggested in [F.

Cited by 78 publications

References 144 publications

Black-bounce to traversable wormhole

Black-bounce to traversable wormhole

Einstein and Møller Energy-Momentum Distributions for the Static Regular Simpson–Visser Space-Time

(A)dS Taub-NUT and exact black bounces with scalar hair

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