Gravitational bending angle of light for finite distance and the Gauss-Bonnet theorem

Ishihara, Asahi; Suzuki, Yusuke; Ono, Toshiaki; Kitamura, Takao; Asada, Hideki

doi:10.1103/physrevd.94.084015

Cited by 238 publications

(309 citation statements)

References 34 publications

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“…Therefore, the main purpose of the present paper is to extend the earlier work [28], especially in order to examine finite-distance corrections in the strong deflection limit. We shall discuss their implications for possible observations.…”

Section: Introductionmentioning

confidence: 99%

“…Following Ishihara et al [28], the present paper considers a static and spherically symmetric (SSS) spacetime. The SSS spacetime can be described as (cf.…”

Section: A Notationmentioning

confidence: 99%

“…Let φ RS ≡ φ R − φ S denote the coordinate separation angle between the receiver and source. From the three angles Ψ R , Ψ S and φ RS , let us define [28] …”

Section: A Notationmentioning

confidence: 99%

“…They used the Gauss-Bonnet theorem to a spatial domain described by the optical metric, where they assumed that the source and receiver are located at an asymptotic region. By extending Gibbons and Werner's idea, Ishihara et al have recently investigated finite-distance corrections [28]. However, such works [27,28] are limited within the small deflection limit.…”

Section: Introductionmentioning

confidence: 99%

“…By extending Gibbons and Werner's idea, Ishihara et al have recently investigated finite-distance corrections [28]. However, such works [27,28] are limited within the small deflection limit.…”

Section: Introductionmentioning

confidence: 99%

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Finite-distance corrections to the gravitational bending angle of light in the strong deflection limit

et al. 2017

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Continuing work initiated in an earlier publication [Ishihara, Suzuki, Ono, Kitamura, Asada, Phys. Rev. D 94, 084015 (2016) ], we discuss a method of calculating the bending angle of light in a static, spherically symmetric and asymptotically flat spacetime, especially by taking account of the finite distance from a lens object to a light source and a receiver. For this purpose, we use the Gauss-Bonnet theorem to define the bending angle of light, such that the definition can be valid also in the strong deflection limit. Finally, this method is applied to Schwarzschild spacetime in order to discuss also possible observational implications. The proposed corrections for Sgr A * for instance are able to amount to ∼ 10 −5 arcseconds for some parameter range, which may be within the capability of near-future astronomy, while also the correction for the Sun in the weak field limit is ∼ 10 −5 arcseconds. 95.30.Sf, 98.62.Sb

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Section: Introductionmentioning

confidence: 99%

“…Following Ishihara et al [28], the present paper considers a static and spherically symmetric (SSS) spacetime. The SSS spacetime can be described as (cf.…”

Section: A Notationmentioning

confidence: 99%

“…Let φ RS ≡ φ R − φ S denote the coordinate separation angle between the receiver and source. From the three angles Ψ R , Ψ S and φ RS , let us define [28] …”

Section: A Notationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Finite-distance corrections to the gravitational bending angle of light in the strong deflection limit

et al. 2017

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Study of the Deflection Angle and Shadow of Black Hole Solutions in Non‐Plasma and Plasma Mediums Under the Effect of Einstein–Gauss–Bonnet Gravity

2023

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In this paper, the Gibbons and Werner technique is used to calculate the weak deflection angle for the black hole solution under the effects of Einstein–Gauss–Bonnet gravity. The Gauss–Bonnet theorem in the limits of weak field is used to evaluate the Gaussian optical curvature in order to obtain the results. The visual effects of the deflection angle on the impact parameter is also looked at and the smallest radius in the non‐plasma/plasma medium. Moreover, in order to check the consistency of the results concerning the weak deflection angle, the Keeton and Petters approach is applied to study the deflection angle, which is the expansion of series with a single mass variable, which can be directly addressed by using the post–post Newtonian framework. Furthermore, the deflection angle and shadow under the influence of the plasma is examined by using the motion of particle in a non‐magnetized plasma and pressure‐free plasma medium as described by the new ray‐tracing algorithm. It is shown that plasma as well as Einstein–Gauss‐Bonnet gravity corrections are affected by shadows.

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Black Hole in Quantum Wave Dark Matter

Pantig

Овгун

2022

Fortschritte der Physik

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In this work, we explored the effect of the fuzzy dark matter (FDM) (or wave dark matter) halo on a supermassive black hole (SMBH). Such a dark matter introduces a soliton core density profile, and we treat it ideally as a spherical distribution that surrounds the SMBH located at its center. In this direction, we obtained a new metric due to the union of the black hole and dark matter spacetime geometries. We applied the solution to the two known SMBH ‐ Sgr. A* and M87* and used the empirical data for the shadow diameter by EHT to constrain the soliton core radius rnormalc$r_\text{c}$ given some values of the boson mass mnormalb$m_\text{b}$. Then, we examine the behavior of the shadow radius based on such constraints and relative to a static observer. We found that different shadow sizes are perceived at regions robsrc$r_\text{obs}>r_\text{c}$, and the deviation is greater for values mb<10−22$m_\text{b}<10^{-22}$ eV. Concerning the shadow behavior, we have also analyzed the effect of the soliton profile on the thin‐accretion disk. Soliton dark matter effects manifest through the varying luminosity near the event horizon. We also analyzed the weak deflection angle and the produced Einstein rings due to soliton effects. We found considerable deviation, better than the shadow size deviation, for the light source near the SMBH with impact parameters comparable to the soliton core. Our results suggest the possible experimental detection of soliton dark matter effects using an SMBH at the galactic centers.

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Gravitational bending angle of light for finite distance and the Gauss-Bonnet theorem

Cited by 238 publications

References 34 publications

Finite-distance corrections to the gravitational bending angle of light in the strong deflection limit

Finite-distance corrections to the gravitational bending angle of light in the strong deflection limit

Study of the Deflection Angle and Shadow of Black Hole Solutions in Non‐Plasma and Plasma Mediums Under the Effect of Einstein–Gauss–Bonnet Gravity

Black Hole in Quantum Wave Dark Matter

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