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Considering the analogy between classical thermodynamic parameters and black hole parameters, the four laws of thermodynamics are reinterpreted for Kerr and Kerr-Newman black holes. A simple model for the dynamic relationships was obtained by considering the surface area of the outer horizon of a Kerr and Kerr-Newman black hole as the area of a per...
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... ultimate singularity at the centre of the black hole. The key to understanding black holes is to appreciate the meaning of the so-called event horizon [2]. Unlike steady black holes, rotating black holes have complex structure consisting with an outer horizon, inner horizon and a region between static limit and the horizon known as the ergosphere (Fig. 1). Classically black holes were nature's ultimate sponges, absorbing all matter and emitting nothing. Superficially they had neither temperature nor entropy and were characterized by only a few basic parameters: mass, angular momentum, and charge [3]. The advent of quantum field theory in curved space-time changed all of these, leading ...
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... expression for Kerr black hole entropy can be deduced from Eq. 11: The Hawking radiation with respect to mass with Kerr parameter fixed at 0.3m a and entropy with time for Schwarzschild [18], Kerr and Kerr-Newman black holes are presented in Fig. 12 and Fig. 13 respectively. For a given mass value the Kerr-Newman black hole emits more radiation than the Kerr and Schwarzschild [18] black holes. But, when these black holes reach extreme masses, all of them tend to radiate similar amounts. Schwarzschild and Kerr black holes emit almost the same amount of radiation at extreme ...
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... implies that, at extreme mass conditions 'mass' parameter dominates the other parameters. In the entropy simulations (Fig.13), the entropy of the black holes decrease throughout the time and one could think of this as a violation of the second law of thermodynamics. ...
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... generally the second law of thermodynamics can be presented as the summation of the entropies of the black hole ( 10 K was simulated using Stephan-Boltzmann equation at the outer event horizon. This is shown in Fig. 14. The red line denotes peak of the radiation jet of the black hole. This is exactly at the centre of the black hole. Hawking radiation distribution on the surface of the black hole from the top view is presented in Fig. 15. The peak of the radiation is at the centre of the black hole and decays gradually towards the event horizon. ...
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... of the black hole ( 10 K was simulated using Stephan-Boltzmann equation at the outer event horizon. This is shown in Fig. 14. The red line denotes peak of the radiation jet of the black hole. This is exactly at the centre of the black hole. Hawking radiation distribution on the surface of the black hole from the top view is presented in Fig. 15. The peak of the radiation is at the centre of the black hole and decays gradually towards the event horizon. ...
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