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

Abstract

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.

Evolution of light deflection and shadow from a gauge-potential-like AdS black hole under the influence of a non-magnetic plasma medium

“…The Keeton and Petters method is used to compute the DA for an accelerating charged AdS BH solution. Keeton and Petters developed that technique to calculate the expression [75][76][77] and to make it more feasible with their approach. The limit of weak deflection is defined as an expansion of series with a single mass m variable in the post-post Newtonian (PPN) framework, which is an easy way to deal with gravity theories in weak field limits.…”

Study of bending angle and shadow in a new Schwarzschild-like black hole affected by plasma and non-plasma mediums*

“…[36], and the quasinormal modes in the eikonal limit and the radius of the BH shadow were found to be related in [37,38]. Additional important examinations of the BH shadow and DA were performed in [39][40][41]. The shadow cast by a dyon BH, also known as Kerr-Newman-Kasuya spacetime, was studied in [42], where it was concluded that the shadow image is affected by both its rotational momentum and dyon charge.…”