Effect of the Brane-Dicke coupling parameter on weak gravitational lensing by wormholes and naked singularities

Abstract

In this paper, we analyze the deflection angle of light by Brane-Dicke wormhole in the weak field limit approximation to find the effect of the Brane-Dicke coupling parameter on the weak gravitation lensing. For this purpose, we consider new geometric techniques, i.e., Gauss-Bonnet theorem and optical geometry in order to calculate the deflection angle. Furthermore, we verify our results by considering the most familiar geodesic technique. Moreover, we establish the quantum corrected metric of Brane-Dicke wormhole by replacing the classical geodesic with Bohmian trajectories, whose matter source and anisotropic pressure are influenced by Bohmian quantum effects and calculate its quantum corrected deflection angle. Then, we calculate the deflection angle by naked singularities and compare with the result of wormhole's. Such a novel lensing feature might serve as a way to detect wormholes, naked singularities and also the evidence of Brane-Dicke theory. 95.30.Sf, 98.62.Sb

Finite-distance gravitational deflection of massive particles by a Kerr-like black hole in the bumblebee gravity model

“…(48) and the finite-distance deflection angle of a massive particle by a Schwarzschild-like black hole in the bumblebee gravity theory in Eq. (49). In particular, when considering the limit of deflection of light in Schwarzschild-like spacetime, in Eq.…”

“…(48) and Eq. (49) are also obtained for the first time. Further more, considering the infinite-distance deflection of light in Schwarzschild-like spacetime, we correct a mistake in Ref.…”

Black hole mimicker hiding in the shadow: Optical properties of the γ metric

“…* aaskar17@fudan.edu.cn † ahmadjon@astrin.uz ‡ dimitry@fudan.edu.cn § daniele.malafarina@nu.edu.kz ¶ bambi@fudan.edu.cn * * ahmedov@astrin.uz To this aim it is important to consider physically viable solutions that exhibit small deviations from black hole solutions. For example, investigations of the observational features of a space-time metric which slightly deviates from the Kerr solution have been mostly considered in the context of modified theories of gravity (see for example, [15][16][17][18][19][20][21][22][23][24][25][26][27][28][29][30][31]) or perturbations of the Kerr metric [32][33][34]. The observables of the compact objects, particularly the shadow of the compact objects in modified or alternative theories of gravity have been studied in Refs.…”

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

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