Geodesic motion in Schwarzschild spacetime surrounded by quintessence

Abstract

We study the time-like geodesic congruences, in the space-time geometry of a Schwarzschild black hole surrounded by quintessence. The nature of effective potential along with the structure of the possible orbits for test particles in view of the different values of quintessence parameter are analysed in detail. An increase in quintessence parameter is seen to set the particles from further distance into motion around black hole. The effect of quintessence parameter is investigated analytically wherever possible otherwise we perform the numerical analysis to probe the structure of possible orbits. It is observed that there exist a number of different possible orbits for a test particle in case of non-radial geodesics, such as circular (stable as well as unstable) bound orbits, radially plunge and fly-by orbits, whereas no bound orbits exist in case of radial geodesics.

Studying gravitational deflection of light by Kiselev black hole via homotopy perturbation method

“…where m is the mass of the black hole and σ is the normalization factor satisfying 0 < σ < 1 [28]. the quintessence equation of state parameter, w q = p q /ρ q , that is related to the energy density as follows ρ q = −3σw q u 3(1+wq) /2.…”

“…The same applies to the astrophysical models with a quintessence field. For example, the evolving quintessence scalar field dark energy model and study the geodesics around a Schwarzschild black hole surrounded by such scalar field was considered in [28]. The spherically symmetric solutions describing a black hole surrounded by dark energy in the form of a quintessential field with equation of state in the form p = w q ρ, with the quintessential parameter −1 < w q < −1/3, has been found by Kiselev [29], and later has been investigated in several articles (e.g., in [30,31,32]).…”

Geodesic flows in a charged black hole spacetime with quintessence

“…The study of geodesics alongwith their deformations in the background of a given spacetime is an elegant way to describe the underlying geometry of that particular spacetime [1][2][3]5,6,13,30]. A number of studies related to the geodesic motion in the background of various BH spacetimes have been performed time and again mainly in view of their astrophysical importance [14][15][16][17][18][19][20][21][22][23][24][25][26][27][28][29].…”

Marginally stable circular orbits in the Schwarzschild black hole surrounded by quintessence matter

“…For the same black hole time-like geodesics have been studied by Rashmi et. al [25]. They have considered three different values of the equation of state parameter ω q = −1, −2/3, −1/3 and four different values of the normalization factor α = 0.1, 0.08, 0.05, 0.005.…”