Thermodynamics phase transition and Hawking radiation of the Schwarzschild black hole with quintessence-like matter and a deficit solid angle

被引:17
作者
Rodrigue, Kamiko Kouemeni Jean [1 ]
Saleh, Mahamat [2 ]
Thomas, Bouetou Bouetou [3 ,4 ,5 ]
Kofane, Timoleon Crepin [4 ,5 ]
机构
[1] Univ Maroua, Fac Sci, Dept Phys, POB 814, Maroua, Cameroon
[2] Univ Maroua, Higher Teachers Training Coll, Dept Phys, POB 55, Maroua, Cameroon
[3] Univ Yaounde I, Ecole Natl Super Polytech, POB 8390, Yaounde, Cameroon
[4] Univ Yaounde I, Fac Sci, Dept Phys, POB 812, Yaounde, Cameroon
[5] Africain Ctr Excellence Informat & Commun Technol, Yaounde, Cameroon
关键词
Black hole; Quintessence-like matter; Deficit solid angle; Thermodynamics; Phase transition; GRAVITATIONAL-FIELD; CHARGED-PARTICLES; ENERGY COMPONENT; SECRET TUNNEL; EQUATION;
D O I
10.1007/s10714-018-2367-3
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
In this paper, we investigate the thermodynamics and Hawking radiation of Schwarzschild black hole with quintessence-like matter and deficit solid angle. From the metric of the black hole, we derive the expressions of temperature and specific heat using the laws of black hole thermodynamics. Using the null geodesics method and Parikh-Wilczeck tunneling method, we derive the expressions of Boltzmann factor and the change of Bekenstein-Hawking entropy for the black hole. The behaviors of the temperature, specific heat, Boltzmann factor and the change of Bekenstein entropy versus the deficit solid angle (epsilon(2)) and the density of static spherically symmetric quintessence-like matter (rho(0)) were explicitly plotted. The results show that, when the deficit solid angle (epsilon(2)) and the density of static spherically symmetric quintessence-like matter at r = 1 (rho(0)) vanish (rho(0) = epsilon = 0), these four thermodynamics quantities are reduced to those obtained for the simple case of Schwarzschild black hole. For low entropies, the presence of quintessence-like matter induces a first order phase transition of the black hole and for the higher values of the entropies, we observe the second order phase transition. When increasing rho(0), the transition points are shifted to lower entropies. The same thing is observed when increasing epsilon(2). In the absence of quintessence-like matter (rho(0) = 0), these transition phenomena disappear. Moreover the rate of radiation decreases when increasing rho(0) or (epsilon(2)).
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页数:15
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