Gravitational deflection angle of light: Definition by an observer and its application to an asymptotically nonflat spacetime

Takizawa, Keita; Ono, Toshiaki; Asada, Hideki

doi:10.1103/physrevd.101.104032

Cited by 54 publications

(49 citation statements)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The weak deflection angle, using the GBT for various spacetimes, was studied by many physicists. For example, the deflection angle of light was studied for BHs and wormholes by the following authors [35][36][37][38][39][40][41][42][43][44][45][46][47][48][49][50][51][52][53]: Ovgun et al studied for different spacetimes, such as Schwarzschild-like spacetime, the bumblebee gravity model [54][55][56][57][58][59][60], and Javed et al studied the impact of various matter fields [61][62][63][64][65]. Next, Ishihara et al [66] showed that it is conceivable to calculate the weak deflection angle using the finite-distances method.…”

Section: Kdsmentioning

confidence: 99%

Weak Deflection Angle and Shadow by Tidal Charged Black Hole

2021

View full text Add to dashboard Cite

In this article, we calculate the deflection angle of a tidal charged black hole (TCBH) in weak field limits. First, we obtain the Gaussian optical curvature and then apply the Gauss–Bonnet theorem on it. With the help of Gibbons–Werner method, we are able to calculate the light’s deflection angle by TCBH in weak field limits. After calculating the deflection angle of light, we check the graphical behavior of TCBH. Moreover, we further find the light’s deflection angle in the presence of the plasma medium and also check the graphical behavior in the presence of the plasma medium. Moreover, we investigate the shadow of TCBH. For calculating the shadow, we first find the null geodesics around the TCBH and then find its shadow radius. We also obtain TCBH’s shadow in the plasma medium. Hence, we discuss the shadow of the TCBH, using the M87* parameters announced by the event horizon telescope.

show abstract

Section: Kdsmentioning

confidence: 99%

Weak Deflection Angle and Shadow by Tidal Charged Black Hole

2021

View full text Add to dashboard Cite

show abstract

“…Up to this point, we have not mentioned details of α. Takizawa et al have shown Eq. ( 23) for the deflection angle of light can be justified even in a nonasymptotically flat spacetime [22]. They have calculated α in the Schwarzschild de-Sitter spacetime.…”

Section: Deflection Angle Of Light On Ds/ads Backgroundsmentioning

confidence: 99%

“…As an example, we assume the Schwarzschild de-Sitter spacetime, for which α is calculated in References [9,22]. Their α is invariant under transformations of spatial coordinates, because it can be expressed as the areal integral of the Gaussian curvature of the plane.…”

Section: Deflection Angle Of Light On Ds/ads Backgroundsmentioning

confidence: 99%

“…( 86) and (89), the deflection angle of light for a given lens mass is larger (smaller) in dS (AdS) than in the flat case, where d L = D L is used. This means that, through a coupling of Λ with m, the separation angle of multiple images is It is worthwhile to mention also that α in References [9,22] apparently diverges as b → ∞, while Eq. ( 79) is not divergent because the present formulation takes full account of the curvature of dS backgrounds.…”

Section: Deflection Angle Of Light On Ds/ads Backgroundsmentioning

confidence: 99%

“…Until recently, the definition for the deflection angle of light has required the asymptotic flat-ness of a spacetime [5][6][7][8]. However, recent works [9,22] based on the Gauss-Bonnet theorem [23] have enabled us to well define the deflection angle without assuming the asymptotic flatness. This new method has been applied by several groups to various spacetime models [24][25][26][27][28][29][30][31][32][33][34].…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Gravitational lens on de-Sitter background

Takizawa,

Asada

2021

Preprint

Self Cite

View full text Add to dashboard Cite

Gravitational lenses are examined in de-Sitter (dS) background, for which the existence of the dS horizon is taken into account and hyperbolic trigonometry is used together with the hyperbolic angular diameter distance. Spherical trigonometry is used to discuss a gravitational lens in antide Sitter (AdS) background. The difference in the form among the dS/AdS lens equations and the exact lens equation in Minkowski background begins at the third order, when a small angle approximation is used in terms of lens and source planes. The angular separation of lensed images is decreased by the third-order deviation in the dS lens equation, while it is increased in AdS. In the present framework on the dS/AdS backgrounds, we discuss also the deflection angle of light, which does not include any term of purely the cosmological constant. Despite the different geometry, the deflection angle of light rays in hyperbolic and spherical geometry can take the same form. Through a coupling of the cosmological constant with lens mass, the separation angle of multiple images is larger (smaller) in dS (AdS) than in the flat case, for a given mass, source direction and angular diameter distances among the lens, receiver and source.

show abstract

Schwarzschild-like black hole with a topological defect in bumblebee gravity

Güllü

Овгун

2022

Annals of Physics

View full text Add to dashboard Cite

Gravitational deflection angle of light: Definition by an observer and its application to an asymptotically nonflat spacetime

Cited by 54 publications

References 35 publications

Weak Deflection Angle and Shadow by Tidal Charged Black Hole

Weak Deflection Angle and Shadow by Tidal Charged Black Hole

Gravitational lens on de-Sitter background

Schwarzschild-like black hole with a topological defect in bumblebee gravity

Contact Info

Product

Resources

About