Deflection angle of light for an observer and source at finite distance from a rotating wormhole

Ono, Toshiaki; Ishihara, Asahi; Asada, Hideki

doi:10.1103/physrevd.98.044047

Cited by 99 publications

(76 citation statements)

References 44 publications

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“…Later, Ono et al developed a different approach using the Gauss-Bonnet theorem that enables the calculation of the deflection angle for the finite distance case in the Kerr spacetime [42]. By using Equations (42) and (43), the generalized optical metric γ ij and the gravitomagnetic term β i for the Kerr metric are obtained as:…”

Section: Kerr Spacetime and γ Ijmentioning

confidence: 99%

“…For the rotating Teo wormhole of Equation (128), the components of the generalized optical metric are [43]:…”

Section: Rotating Teo Wormhole and Optical Metricmentioning

confidence: 99%

“…In particular, we hope that the detailed calculations in this paper will be helpful for readers to compute the gravitational deflection of light by the new powerful method. For instance, this new technique has been used to study the gravitational lensing in rotating Teo wormholes [43] and also in Damour-Solodukhin wormholes [44]. This formulation has been successfully used to clarify the deflection of light in a rotating global monopole spacetime with a deficit angle [45].…”

Section: Introductionmentioning

confidence: 99%

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The Effects of Finite Distance on the Gravitational Deflection Angle of Light

Ono

Asada

2019

Universe

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In order to clarify the effects of the finite distance from a lens object to a light source and a receiver, the gravitational deflection of light has been recently reexamined by using the Gauss–Bonnet (GB) theorem in differential geometry (Ishihara et al. 2016). The purpose of the present paper is to give a short review of a series of works initiated by the above paper. First, we provide the definition of the gravitational deflection angle of light for the finite-distance source and receiver in a static, spherically symmetric and asymptotically flat spacetime. We discuss the geometrical invariance of the definition by using the GB theorem. The present definition is used to discuss finite-distance effects on the light deflection in Schwarzschild spacetime for both the cases of weak deflection and strong deflection. Next, we extend the definition to stationary and axisymmetric spacetimes. We compute finite-distance effects on the deflection angle of light for Kerr black holes and rotating Teo wormholes. Our results are consistent with the previous works if we take the infinite-distance limit. We briefly mention also the finite-distance effects on the light deflection by Sagittarius A * .

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Section: Kerr Spacetime and γ Ijmentioning

confidence: 99%

“…For the rotating Teo wormhole of Equation (128), the components of the generalized optical metric are [43]:…”

Section: Rotating Teo Wormhole and Optical Metricmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Effects of Finite Distance on the Gravitational Deflection Angle of Light

Ono

Asada

2019

Universe

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“…Then, Werner has enlarged this formalism and derive the angle of deflection by a Kerr-Newman BH by using the Nazim's method with Rander-Finsler metric [26]. Recently, Ishihara et al [27][28][29][30] computed the deflection angle in a static, spherically symmetric and asymptotically flat space by using the finite distance from an observer to a light source. Moreover, the GBT has been stretched out to the wormhole geometries and non-asymptotically flat spacetime with topological effects [31][32][33].…”

Section: Introductionmentioning

confidence: 99%

Effect of the Quintessential Dark Energy on Weak Deflection Angle by Kerr-Newmann Black Hole

Javed¹,

Abbas²,

Овгун³

2019

Preprint

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In this work, we study the weak gravitational lensing in the background of Kerr-Newman black hole with quintessential dark energy. Initially, we compute the deflection angle of light by charged black hole with quintessential dark energy by utilizing the Gauss-Bonnet theorem. Firstly, we suppose the light rays on the equatorial plane in the axisymmetric spacetime. In doing so, we first find the corresponding optical metrics and then calculate the Gaussian optical curvature to utilize in Gauss-Bonnet theorem. Consequently, we calculate the deflection angle of light for rotating charged black hole with quintessence. Additionally, we also find the deflection angle of light for Kerr-Newman black hole with quintessential dark energy. In order to verify our results, we derive deflection angle by using null geodesic equations which reduces to the deflection angle of Kerr solution with the reduction of specific parameters. Furthermore, we analyze the graphical behavior of deflection angle $\Theta$ w.r.t to quintessence parameter $\alpha$, impact parameter $b$, BH charge $Q$ and rotation parameter $a$. Our graphical analysis retrieve various results regarding to the deflection angle by the Kerr-Newman black hole with quintessential dark energy.

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“…Moreover, using the GBT on the Rindler-modified Schwarzschild black hole, Sakalli andÖvgün recently showed the deflection angle at the infrared region [37]. The method of calculating the bending angle of light using the GBT has been extensively studied in [38][39][40].…”

Section: Introductionmentioning

confidence: 99%

Light deflection by charged wormholes in Einstein-Maxwell-dilaton theory

2017

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In this paper, we study the deflection of light by a class of charged wormholes within the context of the Einstein-Maxwell-dilaton theory. The primordial wormholes are predicted to exist in the early universe, where inflation driven by the dilaton field. We perform our analysis through optical geometry using the Gibbons-Werner method (GW), by adopting the Gauss-Bonnet theorem and the standard geodesics approach. We report an interesting result for the deflection angle in leadingorder terms-namely, the deflection angle increases due to the electric charge Q and the magnetic charge P , whereas it decreases due to the dilaton charge Σ. Finally, we confirm our findings by means of geodesics equations. Our computations show that the GW method gives an exact result in leading order terms.PACS numbers: 95.30.Sf, 98.62.Sb

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Deflection angle of light for an observer and source at finite distance from a rotating wormhole

Cited by 99 publications

References 44 publications

The Effects of Finite Distance on the Gravitational Deflection Angle of Light

The Effects of Finite Distance on the Gravitational Deflection Angle of Light

Effect of the Quintessential Dark Energy on Weak Deflection Angle by Kerr-Newmann Black Hole

Light deflection by charged wormholes in Einstein-Maxwell-dilaton theory

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