Analytic Kerr black hole lensing for equatorial observers in the strong deflection limit

Bozza, V.; Luca, F. De; Scarpetta, G.; Sereno, Mauro

doi:10.1103/physrevd.72.083003

Cited by 159 publications

(162 citation statements)

References 51 publications

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“…The finite size of the caustic should show up at the next order due to terms ∝ a 2 r 2 Sch as suggested by numerical results [8]. It could be of interest to draw some comparison with the case of the strong deflection limit [9,10,11]. Such a limit has been treated considering small values of the angular momentum and including corrections proportional to a 2 .…”

Section: Discussionmentioning

confidence: 99%

“…For a source emitting isotropically, the unlensed source as seen by the observer is (r s /r os ) 2 smaller than as seen by an observer in the black hole position [10]. Then,…”

Section: Magnificationmentioning

confidence: 99%

“…Rauch and Blandford [8] provided a detailed analysis of the optical structure of the primary caustic surface. The analytical extension of the strong deflection limit methodology to the Kerr black hole has been performed as well in the limit of small values of the angular momentum and for sources in the asymptotically flat region of the space-time [9,10,11]. A full description of caustics and the inversion of lens mapping for sources near them has been performed up to the second order in a.…”

Section: Introductionmentioning

confidence: 99%

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Analytical Kerr black hole lensing in the weak deflection limit

2006

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We present an analytical treatment of gravitational lensing by a Kerr black hole in the weak deflection limit. Lightlike geodesics are expanded as a Taylor series up to and including third-order terms in m/b and a/b, where m is the black hole mass, a the angular momentum and b the impact parameter of the light ray. Positions and magnifications of individual images are computed with a perturbative analysis. At this order, the degeneracy with the translated Schwarzschild lens is broken. The critical curve is still a circle displaced from the black hole position in the equatorial direction and the corresponding caustic is point-like. The degeneracy between the black hole spin and its inclination relative to the observer is broken through the angular coordinates of the perturbed images.

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Section: Discussionmentioning

confidence: 99%

“…For a source emitting isotropically, the unlensed source as seen by the observer is (r s /r os ) 2 smaller than as seen by an observer in the black hole position [10]. Then,…”

Section: Magnificationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Analytical Kerr black hole lensing in the weak deflection limit

2006

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“…Bozza et. all [49] generelized this work by removing the restriction to observers on the equatorial plane. Amore at.…”

Section: Introductionmentioning

confidence: 99%

“…In their next work Bozza et. all [48] made a considerable step towards the analytical treatment of Kerr lensing, by restricting the observer in the equatorial plane and solving the general lens equation using perturbative methods for small values of the black hole spin. The limitation to the equatorial observer is motivated by the fact that the most important candidate for a black hole, Sgr A*, is likely to have a spin axis perpendicular to the galactic plane, where the solar system lies, in first approximation.…”

Section: Introductionmentioning

confidence: 99%

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

2007

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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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Strong gravitational lensing in a rotating Kaluza-Klein black hole with squashed horizons

Chen

Jing

2014

J. High Energ. Phys.

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Abstract:We have investigated the strong gravitational lensing in a rotating squashed Kaluza-Klein (KK) black hole spacetime. Our result show that the strong gravitational lensings in the rotating squashed KK black hole spacetime have some distinct behaviors from those in the backgrounds of the four-dimensional Kerr black hole and of the squashed KK Gödel black hole. In the rotating squashed KK black hole spacetime, the marginally circular photon radius ρ ps , the coefficientā,b, the deflection angle α(θ) in the φ direction and the corresponding observational variables are independent of whether the photon goes with or against the rotation of the background, which is different with those in the usual four-dimensional Kerr black hole spacetime. Moreover, we also find that with the increase of the scale of extra dimension ρ 0 , the marginally circular photon radius ρ ps and the angular position of the relativistic images θ ∞ first decreases and then increases in the rotating squashed KK black hole for fixed rotation parameter b, but in the squashed KK Gödel black hole they increase for the smaller global rotation parameter j and decrease for the larger one. In the extremely squashed case ρ 0 = 0, the coefficientā in the rotating squashed KK black hole increases monotonously with the rotation parameter, but in the squashed KK Gödel black hole it is a constant and independent of the global rotation of the Gödel Universe. These information could help us to understand further the effects of the rotation parameter and the scale of extra dimension on the strong gravitational lensing in the black hole spacetimes.

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Analytic Kerr black hole lensing for equatorial observers in the strong deflection limit

Cited by 159 publications

References 51 publications

Analytical Kerr black hole lensing in the weak deflection limit

Analytical Kerr black hole lensing in the weak deflection limit

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

Strong gravitational lensing in a rotating Kaluza-Klein black hole with squashed horizons

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