2002

DOI: 10.1103/physrevd.65.103004

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Gravitational lensing by naked singularities

K. S. Virbhadra

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Jhep07(2015)1602

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Determination Of the Black Hole Spin From The Resonance Model1

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Cited by 636 publications

(598 citation statements)

References 13 publications

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“…We quantify the impact of these effects both in the thin lens approximation, where the trigonometric relations in the lens geometry are expanded to first order, and for a lens with deflection terms of higher order included. As an example, in this second case, we have chosen the Virbhadra-Ellis [12] lens equation. The observables that we discuss are limited to solutions of these equations and to their magnifications, although time delays, shears and the light curves of a typical microlensing event can be easily included in this framework.…”

Section: Jhep07(2015)160mentioning

confidence: 99%

“…In the case of a neutrino, the corresponding cross section is obtained by sending the fermion mass m of the related Dirac cross section to zero, giving dσ dΩ 12) JHEP07(2015)160 which is energy independent. Notice that the inclusion of the chiral projector P L in the expression of the neutrino amplitude, which carries a factor 1/2, makes the neutrino and Dirac cross sections coincide.…”

Section: Jhep07(2015)160mentioning

confidence: 99%

See 1 more Smart Citation

Neutrino and photon lensing by black holes: radiative lens equations and post-Newtonian contributions

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et al. 2015

J. High Energ. Phys.

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We extend a previous phenomenological analysis of photon lensing in an external gravitational background to the case of a massless neutrino, and propose a method to incorporate radiative effects in the classical lens equations of neutrinos and photons. The study is performed for a Schwarzschild metric, generated by a point-like source, and expanded in the Newtonian potential at first order. We use a semiclassical approach, where the perturbative corrections to neutrino scattering, evaluated at one-loop in the Standard Model, are compared with the Einstein formula for the deflection using an impact parameter formulation. For this purpose, we use the renormalized expression of the graviton/fermion/fermion vertex presented in previous studies. We show the agreement between the classical and the semiclassical formulations, for values of the impact parameter b h of the neutrinos of the order of b h ∼ 20, measured in units of the Schwarzschild radius. The analysis is then extended with the inclusion of the post Newtonian corrections in the external gravity field, showing that this extension finds application in the case of the scattering of a neutrino/photon off a primordial black hole. The energy dependence of the deflection, generated by the quantum corrections, is then combined with the standard formulation of the classical lens equations. We illustrate our approach by detailed numerical studies, using as a reference both the thin lens and the Virbhadra-Ellis lens.

“…We quantify the impact of these effects both in the thin lens approximation, where the trigonometric relations in the lens geometry are expanded to first order, and for a lens with deflection terms of higher order included. As an example, in this second case, we have chosen the Virbhadra-Ellis [12] lens equation. The observables that we discuss are limited to solutions of these equations and to their magnifications, although time delays, shears and the light curves of a typical microlensing event can be easily included in this framework.…”

Section: Jhep07(2015)160mentioning

confidence: 99%

“…In the case of a neutrino, the corresponding cross section is obtained by sending the fermion mass m of the related Dirac cross section to zero, giving dσ dΩ 12) JHEP07(2015)160 which is energy independent. Notice that the inclusion of the chiral projector P L in the expression of the neutrino amplitude, which carries a factor 1/2, makes the neutrino and Dirac cross sections coincide.…”

Section: Jhep07(2015)160mentioning

confidence: 99%

Neutrino and photon lensing by black holes: radiative lens equations and post-Newtonian contributions

¹

,

²

,

³

et al. 2015

J. High Energ. Phys.

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We extend a previous phenomenological analysis of photon lensing in an external gravitational background to the case of a massless neutrino, and propose a method to incorporate radiative effects in the classical lens equations of neutrinos and photons. The study is performed for a Schwarzschild metric, generated by a point-like source, and expanded in the Newtonian potential at first order. We use a semiclassical approach, where the perturbative corrections to neutrino scattering, evaluated at one-loop in the Standard Model, are compared with the Einstein formula for the deflection using an impact parameter formulation. For this purpose, we use the renormalized expression of the graviton/fermion/fermion vertex presented in previous studies. We show the agreement between the classical and the semiclassical formulations, for values of the impact parameter b h of the neutrinos of the order of b h ∼ 20, measured in units of the Schwarzschild radius. The analysis is then extended with the inclusion of the post Newtonian corrections in the external gravity field, showing that this extension finds application in the case of the scattering of a neutrino/photon off a primordial black hole. The energy dependence of the deflection, generated by the quantum corrections, is then combined with the standard formulation of the classical lens equations. We illustrate our approach by detailed numerical studies, using as a reference both the thin lens and the Virbhadra-Ellis lens.

“…They defined the relativistic images which are very demagnified unless the observer, the lens and the source are very highly aligned and would serve as a proof of the general relativity if they were ever observed. After this paper Virbhadra and Ellis [17] numerically investigated the lensing by naked singularities. On the other hand, Perlick [18] has considered lensing in a spherically symmetric and static spacetime, based on the lightlike geodesic equation without approximations.…”

Section: Introductionmentioning

confidence: 99%

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

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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

“…Eqs. (3), (4), (34)(35)(36) imply that, the horizon of the black hole does not only effect the Hawking radiation but also influence the strong gravitational lensing in the carved spacetime. Because the horizon H r is determined by the metric in the gravitational field, the gravitational lensing is related the metric of the black hole closely.…”

Section: Resultsmentioning

confidence: 99%

Strong Gravitational Lensing in the Einstein-Proca Theory

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et al. 2014

Int J Theor Phys

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Adopting the strong field limit approach, we investigate the strong gravitational lensing of a spherically symmetric spacetime in the Einstein-Proca theory. With the strong field limit coefficient, three observable quantities are obtained, which are the innermost relativistic image, the deflection angle and the ratio of the flux. Comparing the observable value and the theoretical value of the strong gravitational lensing, we can verify the effectiveness of the strong gravitational lensing model.

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