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008			220928b ||||| |||| 00| 0 eng d
020			_ahbk
082			_a512.7 _bQ259
100			_aRimsha Babar, _bMS Mathematics, _c2016-2018, _dSupervised by Dr. Wajiha Jawed
245			_aQuantum tunneling and corrections for Kerr-Newman-ADS black hole with quintessence _c/ Rimsha Babar
260			_aLahore : _bDivision of Science and Technology, University of Education, _c2018
300			_a79 p.
520			_aThe 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.
650			_aMathematics--Quantum Tunneling--Quintessence
942			_cTH