The goal of this thesis is to determine the Hawking radiation spectrum via quantum
tunneling strategy for charged massive spin-1 and spin-0 particles in the background
of Kerr-Newman-AdS black hole with quintessence. Utilizing, Hamilton-Jacobi technique and after applying the Wentzel, Kramers and Brillouin (WKB) method to
the field equations, we calculate the tunneling probability and recover the expected
Hawking temperature. We consider the Proca equation to study the motion of vector
particles and Klein-Gordan equation for the investigation of scalar particles motion.
The Hawking temperature for vector and and scalar particles seems to be identical.
Moreover, we analyze the corrected Hawking temperature by taking into account the
quantum gravity effects. For this purpose, we assume the generalized Proca and
Klein-Gordan equations involving the effects of generalized uncertainty principle and
investigate the corrected Hawking temperature for corresponding black hole.
We examine that the expressions of corrected temperatures for spin-1 and spin-0
particles seems to be similar, while the angular momentum and mass are not similar
in their expressions. The inclusion of quantum effects causes deceleration in Hawking
temperature and due to these effects sometimes we obtain black hole remnant under
some specific conditions.
Furthermore, we discuss the behavior of Hawking temperature graphically by
taking into account the quantum gravity effects. We analyze the behavior of corrected temperature for fixed black hole mass Mˇ = 1 and state parameter ˇ ω = −2/3. We
check the stability and instability of black hole by considering the effects of various
parameters on Hawking temperature by visualizing 2-dimensional and 3-dimensional
plots.
Moreover, we analyze the effects of correction parameter βˇ on corrected Hawking
temperature, for β < ˇ 100 the temperature shows positive value and for β > ˇ 100, the
temperature indicates the negative value and for βˇ = 100, the temperature express
zero value and flat behavior. For a very small value of Λ and ˇ β < ˇ 100, the temperature
decreases as ˇ r+ increases, this physical behavior reflects the stability of black hole and
for β > ˇ 100, the temperature always shows negative value which identify black hole
instability.
It is also worth to note that in the graphs of temperature with respect to quintessence
the behavior of Tˇ
eˇ−Hˇ shows only in the specific range of quintessence parameter, i.e.,
0 ≤ αˇ ≤ 0.16. From besides of this range, we cannot observe any behavior of temperature and for this specific range of ˇ α, the maximum values of charge Qˇ = 1 and
rotation parameters ˇ a = 1 and for greater than these values the temperature reflects
no behavior.