Abstract
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.
Highlights
Einstein’s theory of general relativity (GR) is a gravity theory which was developed in1916
We see that the effective potential depends on Black holes (BHs)’s mass denoted by M, and the dimensionless tidal charge denoted by q and effective Planck mass on the brane denoted by M p and fundamental Planck scale in the 5D bulk denoted by M5 and radius r and R(r )
P where the impact parameters depend on the BHs mass denoted by M, the dimensionless tidal charge denoted by q, effective Planck mass on the brane denoted by M p, and fundamental Planck scale in the 5D bulk denoted by M5
Summary
Einstein’s theory of general relativity (GR) is a gravity theory which was developed in. Werner showed that it is possible to find the weak deflection angle of stationary black holes, such as the Kerr black hole, using GBT [34]. The shadow of a black hole is caused by gravitational light deflection.
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