Light paths of normal and phantom Einstein-Maxwell-dilaton black holes

Azreg‐Aïnou, Mustapha

doi:10.1103/physrevd.87.024012

Cited by 37 publications

(29 citation statements)

References 59 publications

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“…The series expansions of the arcsin terms in (46) in powers of (σ, u o , u s , u n ) is straightforward; the series expansion of the first line in (46) has been done in Appendix A of Ref. [35]. In this work we show how to derive the series expansion of the first term in the second line of (46); the series expansion of the second term is obtained by mere substitution u o ↔ u s .…”

Section: Case W Q = −2/3mentioning

confidence: 99%

“…(2.8) of Ref. [35] insert r + + r − = 2M, r + r − = Q 2 , and r 2 + + r 2 − = 4M 2 − 2Q 2 , where r − < r + are the two horizons). The second line in (48) is a correction to the deflection angle for the Reissner-Nordström black hole when the observer and the source are at large, but finite, distances from the lens.…”

Section: Case W Q = −2/3mentioning

confidence: 99%

“…(2.8) of Ref. [35], γ = 1 corresponds to Reissner-Nordström black hole and to obtain the first line in (48) from Eq. (2.8) of Ref.…”

Section: Case W Q = −2/3mentioning

confidence: 99%

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Strong gravitational lensing by a charged Kiselev black hole

2017

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We study the gravitational lensing scenario where the lens is a spherically symmetric charged black hole (BH) surrounded by quintessence matter. The null geodesic equations in the curved background of the black hole are derived. The resulting trajectory equation is solved analytically via perturbation and series methods for a special choice of parameters, and the distance of the closest approach to black hole is calculated. We also derive the lens equation giving the bending angle of light in the curved background. In the strong field approximation, the solution of the lens equation is also obtained for all values of the quintessence parameter w q . For all w q , we show that there are no stable closed null orbits and that corrections to the deflection angle for the Reissner-Nordström black hole when the observer and the source are at large, but finite, distances from the lens do not depend on the charge up to the inverse of the distances squared. A part of the present work, analyzed, however, with a different approach, is the extension of Younas et al. (Phys Rev D 92:084042, 2015) where the uncharged case has been treated.

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Section: Case W Q = −2/3mentioning

confidence: 99%

Section: Case W Q = −2/3mentioning

confidence: 99%

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Strong gravitational lensing by a charged Kiselev black hole

2017

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“…Some other black hole solutions describing gravity coupled to phantom scalar fields or phantom Maxwell fields have been found and the corresponding geometric structure and thermodynamic properties are also studied in [65][66][67][68][69][70][71][72][73]. The strong gravitational lensing of such a kind of black holes with phantom hair has been investigated in [74][75][76][77][78]. In this paper, we are going to study shadow of a regular phantom black hole [64] as photons couple to the Weyl tensor and then probe what effects of the phantom charge of the black hole, the photon polarization directions and the coupling between photon and Weyl tensor on the properties of the shadow.…”

Section: Introductionmentioning

confidence: 99%

Double shadow of a regular phantom black hole as photons couple to the Weyl tensor

2016

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We have studied the shadow of a regular phantom black hole as photons couple to the Weyl tensor. We find that due to the coupling photons with different polarization directions propagate along different paths in the spacetime so that there exists a double shadow for a black hole, which is quite different from that in the non-coupling case where only a single shadow emerges. The overlap region of the double shadow, the umbra, of the black hole increases with the phantom charge and decreases with the coupling strength. The dependence of the penumbra on the phantom charge and the coupling strength is converse to that of the umbra. Combining with the supermassive central object in our Galaxy, we estimated the shadow of the black hole as the photons couple to the Weyl tensor. Our results show that the coupling brings about richer behaviors of the propagation of coupled photon and the shadow of the black hole in the regular phantom black hole spacetime.

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“…A countably infinite number of relativistic images are formed in a spherically symmetric static spacetime, if the radius of the lens object is smaller than a photon sphere (= 3r g /2, where r g is the radius of the event horizon in the Schwarzschild spacetime) [41,49,50]. The gravitational lensing in the strong gravitational field by various black holes and wormholes has been investigated intensively in the recent decade (see [51][52][53][54][55][56] and references therein). In a series of the papers on the relativistic images, the observables for the suppermassive object at the center of our Galaxy with instruments which can measure the relativistic images are discussed intensively.…”

Section: Introductionmentioning

confidence: 99%

Gravitational lensing in Tangherlini spacetime in the weak gravitational field and the strong gravitational field

et al. 2014

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The gravitational lensing effects in the weak gravitational field by exotic lenses have been investigated intensively to find nonluminous exotic objects. Gravitational lensing based on 1/r n fall-off metric, as a one-parameter model that can treat by hand both the Schwarzschild lens (n=1) and the Ellis wormhole (n=2) in the weak field, has been recently studied. Only for n = 1 case, however, it has been explicitly shown that effects of relativistic lens images by the strong field on the light curve can be neglected. We discuss whether relativistic images by the strong field can be neglected for n > 1 in the Tangherlini spacetime which is one of the simplest models for our purpose. We calculate the divergent part of the deflection angle for arbitrary n and the regular part for n = 1, 2 and 4 in the strong field limit, the deflection angle for arbitrary n under the weak gravitational approximation. We also compare the radius of the Einstein ring with the radii of the relativistic Einstein rings for arbitrary n. We conclude that the images in the strong gravitational field have little effect on the total light curve and that the time-symmetric demagnification parts in the light curve will appear even after taking account of the images in the strong gravitational field for n > 1.

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Light paths of normal and phantom Einstein-Maxwell-dilaton black holes

Cited by 37 publications

References 59 publications

Strong gravitational lensing by a charged Kiselev black hole

Strong gravitational lensing by a charged Kiselev black hole

Double shadow of a regular phantom black hole as photons couple to the Weyl tensor

Gravitational lensing in Tangherlini spacetime in the weak gravitational field and the strong gravitational field

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