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Recently, the Hawking radiation of a black hole has been studied using the tunnel effect method. The radiation spectrum of a black hole is derived. By discussing the correction to spectrum of the rotating black hole, we obtain the canonical entropy. The derived canonical entropy is equal to the sum of Bekenstein-Hawking entropy and correction term. The correction term near the critical point is different from the one near others. This difference plays an important role in studying the phase transition of the black hole. The black hole thermal capacity diverges at the critical point. However, the canonical entropy is not a complex number at this point. Thus we think that the phase transition created by this critical point is the second order phase transition. The discussed black hole is a five-dimensional Kerr-AdS black hole. We provide a basis for discussing thermodynamic properties of a higher-dimensional rotating black hole. [ABSTRACT FROM AUTHOR]

Recently, there has been much attention devoted to resolving the quantum corrections to the Bekenstein–Hawking entropy of a black hole. In this paper, we calculate the correction value of thermodynamic quantities of the Achucarro–Oritz black hole motivated by utilizing the generalized uncertainty principle. We obtain the Cardy–Verlinde formula after considering the correction. [ABSTRACT FROM AUTHOR]

Recently, there has been a lot of attention devoted to resolving the quantum corrections to the Bekenstein–Hawking entropy of the black hole. In particular, the coefficient of the logarithmic term in the black hole entropy correction has been of great interest. In this paper, the black hole is corresponded to a canonical ensemble in statistics by radiant spectrum, resulted from the black hole tunnelling effect studies and the partition function of ensemble is derived. Then the entropy of the black hole is calculated. When the first-order approximation is taken into account, the logarithmic term of entropy correction is consistent with the result of the generalized uncertainty principle. In our calculation, there are no uncertainty factors. The prefactor of the logarithmic correction and the one if fluctuation is considered are the same. Our result shows that if the thermal capacity is negative, there is no divergent term. We provide a general method for further discussion on quantum correction to Bekenstein–Hawking entropy. We also offer a theoretical basis for comparing string theory and loop quantum gravity and deciding which one is more reliable. [ABSTRACT FROM AUTHOR]

Abstract: Recently, Hawking radiation of the black hole has been studied using the tunnel effect method. It is found that the radiation spectrum of the black hole is not a strictly pure thermal spectrum. How does the departure from pure thermal spectrum affect the entropy? This is a very interesting problem. In this Letter, we calculate the partition function by energy spectrum obtained from tunnel effect. Using the partition function, we compute the black hole entropy and derive the expression of the black hole entropy after considering the radiation. And we derive the entropy of charged black hole. In our calculation, we consider not only the correction to the black hole entropy due to fluctuation of energy but also the effect of the change of the black hole charges on entropy. There is no other hypothesis. Our result is more reasonable. According to the fact that the black hole entropy is not divergent, we obtain the lower limit of Banados–Teitelboim–Zanelli black hole energy. That is, the least energy of Banados–Teitelboim–Zanelli black hole, which satisfies the stationary condition in thermodynamics. [Copyright &y& Elsevier]

In this paper we discuss thermodynamics parameters of black hole horizon and cosmological horizon in general high-dimensional space-time. We obtain that the entropy of a cosmological horizon can be described by the Cardy-Verlinde formula. However, the entropy of black hole horizon will be expressed in a form of the Cardy-Verlinde formula, if one adopts the methods given by Abbott and Deser to compute the mass of a black hole in general high-dimensional space-time. Through discussion, relation among various thermodynamics parameters of the black hole in general high-dimensional space-time is given. That is, differential formula of the first law of thermodynamics is obtained. Because we discuss the general high-dimensional space-time, our result has universality. [ABSTRACT FROM AUTHOR]

In this paper, by using quantum statistical methods, we directly obtain the partition function of Bose field and Fermi field on the background of the axisymmetrical Sen black hole. The difficult-to-solve wave equation is avoided. Then via the improved brick-wall method and membrane model, we calculate the entropy of Bose field and Fermi field of the black hole. We find that the entropy of the black hole is proportional to the area of the horizon. In our results, we do not encounter the left out term nor the divergent logarithmic term that appears in the original brick-wall method. The question that arose in the brick-wall method of whether the entropy of the scalar or Dirac fields outside the event horizon is the entropy of the black hole does not arise in the present method. The influence of spinning degeneracy of particles on entropy of the black hole is also given. We provide a way to study various complicated black holes. [ABSTRACT FROM AUTHOR]

By using the method of quantum statistics, we directly derive the partition functions of bosonic and fermionic field in Kaluza–Klein black hole with axial symmetry. Then via the improved brick-wall method, membrane model, we obtain that the entropy of bosonic and fermionic field in black hole is proportional to the area of horizon. In our result, the stripped term and the divergent logarithmic term no longer exist. The problem that the state density is divergent around the horizon doesn't exist either. We also give the influence of the spining degeneracy of particles on the entropy of black hole. We offer a new, simple, and direct way of calculating the entropy of different complicated black holes. [ABSTRACT FROM AUTHOR]

Using the method of quantum statistics, we directly derive the partition functions of bosonic and fermionic field in Kerr black hole with axial symmetry. Then via the improved brick-wall method for membrane model, we show that the entropy of the bosonic and fermionic field in the black hole is proportional to the area of the horizon. In our result, the stripped term and the divergent logarithmic term no longer exist. Hence the problem that the state density is divergent around the horizon doesn't exist. We also give the influence of the spining degeneracy of particles on the entropy of black hole. We offer a new simple and direct way of calculating the entropy of different complicated black holes. [ABSTRACT FROM AUTHOR]

Starting from the Klein-Gordon equation, we calculate the entropy of Schwarzschild-de Sitter black hole in non-thermal-equilibrium by using the improved brick-wall methodmembrane model. When taking the proper cutoff in the obtained result, we obtain that both black hole's entropy and cosmic entropy are proportional to the areas of event horizon. We avoid the logarithmic term and stripped term in the original brick-wall method. It offers a new way of studying the entropy of the black hole in non-thermal-equilibrium. [ABSTRACT FROM AUTHOR]

Abstract: Using the new global embedding approach and analytical continuation method of wave function we discuss Hawking radiation of acoustic black holes. Unruh–Hawking temperature of the acoustic black hole is derived. The corresponding relation between these methods calculating Hawking radiation of acoustic black hole is established. The calculation result shows that the contributions of chemical potential to the ingoing wave and the outgoing wave are the same. [Copyright &y& Elsevier]

Recently, there has been much attention devoted to resolving the quantum corrections to the Bekenstein-Hawking black hole entropy. In particular, many researchers have expressed a vested interest in the coefficient of the logarithmic term of the black hole entropy correction term. In this paper, we calculate the correction value of the black hole entropy by utilizing the generalized uncertainty principle and obtain the correction term caused by the generalized uncertainty principle. Because in our calculation we think that the Bekenstein-Hawking area theorem is still valid after considering the generalized uncertainty principle, we derive that the coefficient of the logarithmic term of the black hole entropy correction term is positive. This result is different from the known result at present. Our method is valid not only for single horizon spacetime but also for spin axial symmetric spacetimes with double horizons. In the whole process, the physics idea is clear and calculation is simple. It offers a new way for studying the entropy correction of the complicated spacetime. [ABSTRACT FROM AUTHOR]