Strong Field Limit of Black Hole Gravitational Lensing

Bozza, V.; Capozziello, Salvatore; Iovane, Gerardo; Scarpetta, G.

doi:10.1023/a:1012292927358

Cited by 348 publications

(459 citation statements)

References 10 publications

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“…In the Schwarzschild spacetime, images of light rays passing by the light sphere are much fainter than the images under the weak-field approximation and the former images do not affect the microlensing light curves [62,63].…”

Section: Introductionmentioning

confidence: 99%

Strong deflection limit analysis and gravitational lensing of an Ellis wormhole

Tsukamoto

2016

Phys. Rev. D

137

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Observations of gravitational lenses in strong gravitational fields give us a clue to understanding dark compact objects. In this paper, we extend a method to obtain a deflection angle in a strong deflection limit provided by Bozza [Phys. Rev. D 66, 103001 (2002)] to apply to ultrastatic spacetimes. We also discuss on the order of an error term in the deflection angle. Using the improved method, we consider gravitational lensing by an Ellis wormhole, which is an ultrastatic wormhole of the Morris-Thorne class.

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Section: Introductionmentioning

confidence: 99%

Strong deflection limit analysis and gravitational lensing of an Ellis wormhole

Tsukamoto

2016

Phys. Rev. D

137

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“…In the last two papers, the authors concentrate on the methods developed by Bozza. Bozza et al [22] developed an analytical technique for obtaining the deflection angle in the strong-field situation and showed that the deflection angle diverges logarithmically as light rays approach the photon sphere of a Schwarzschild black hole. In [23] Bozza extended the analytical theory of strong lensing for a general class of static spherically symmetric metrics and showed that the logarithmic divergence of the deflection angle at the photon sphere is a common feature of such spacetimes.…”

Section: Introductionmentioning

confidence: 99%

Kerr-Sen dilaton-axion black hole lensing in the strong deflection limit

Gyulchev

Yazadjiev

2007

Phys. Rev. D

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In the present work we study numerically quasi-equatorial lensing by the charged, stationary, axially-symmetric Kerr-Sen dilaton-axion black hole in the strong deflection limit. In this approximation we compute the magnification and the positions of the relativistic images. The most outstanding effect is that the Kerr-Sen black hole caustics drift away from the optical axis and shift in clockwise direction with respect to the Kerr caustics. The intersections of the critical curves on the equatorial plane as a function of the black hole angular momentum are found, and it is shown that they decrease with the increase of the parameter Q 2 /M . All of the lensing quantities are compared to particular cases as Schwarzschild, Kerr and Gibbons-Maeda black holes. I. INTRODUCTIONOne of the consequences of Einstein's General Theory of Relativity is that light rays are deflected by gravity. Although this discovery was made in the last century, the possibility that there could be such a deflection had been suspected much earlier, by Newton and Laplace, for the first time. The phenomena resulting from the deflection of electromagnetic radiation in a gravitational field are referred to as gravitational lensing (GL) and an object causing a detectable deflection is known as a gravitational lens. Nowadays, gravitational lensing is a rapidly developing area of research, and it has found applications ranging from the search of extrasolar planets and compact dark matter to the estimation of the values of the cosmological parameters [10]. In most of these cases it is possible to assume that the gravitational field is weak, hence the angle of deflection of the light in the field of a spherically symmetric body with mass M can be approximated by: that the present lens model could be able to distinguish observationally a black hole from naked singularity.The study of the gravitational lensing when light passes very close to a massive body, such as a black hole (a process also known as gravitational lensing in the strong deflection

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“…[2,3,4]. The logarithmic divergence of the deflection angle in the impact parameter was showed to be universal and valid for all spherically symmetric black holes [5], as every class of such black holes leads to the same expansion for the deflection angle, with coefficients depending on the specific form of the black hole metric.…”

Section: Introductionmentioning

confidence: 99%

Kerr black hole lensing for generic observers in the strong deflection limit

2006

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We generalize our previous work on gravitational lensing by a Kerr black hole in the strong deflection limit, removing the restriction to observers on the equatorial plane. Starting from the Schwarzschild solution and adding corrections up to the second order in the black hole spin, we perform a complete analytical study of the lens equation for relativistic images created by photons passing very close to a Kerr black hole. We find out that, to the lowest order, all observables (including shape and shift of the black hole shadow, caustic drift and size, images position and magnification) depend on the projection of the spin on a plane orthogonal to the line of sight. In order to break the degeneracy between the black hole spin and its inclination relative to the observer, it is necessary to push the expansion to higher orders. In terms of future VLBI observations, this implies that very accurate measures are needed to determine these two parameters separately.

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Strong Field Limit of Black Hole Gravitational Lensing

Cited by 348 publications

References 10 publications

Strong deflection limit analysis and gravitational lensing of an Ellis wormhole

Strong deflection limit analysis and gravitational lensing of an Ellis wormhole

Kerr-Sen dilaton-axion black hole lensing in the strong deflection limit

Kerr black hole lensing for generic observers in the strong deflection limit

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