Total Quantum Statistical Entropy of Reissner-Nordstrom Black Holes: in Dirac Field Case

The total quantum statistical entropy of Reissner-Nordstrom black holes in Dirac field case is evaluated in this article. The space-time of the black holes is divided into three regions: region 1 (r>r_o), region 2 ( r_o > r > r_i), and region 3 (r_i >r>0), where r_o is the radius of the outer event horizon, and r_i is the radius of the inner event horizon. The total quantum statistical entropy of Reissner-Nordstrom black holes is S=S₁+S₂+S₃, where S_i (i=1,2,3) is the entropy, contributed by regions 1,2,3. The detailed calculation shows that S₂ is neglectfully small. S₁=w_t(π²/45)k_b(A_o/ε²β³), S₃=-w_t(π²/45)k_b(A_i/ε²β³), where A_o and A_i are, respectively, the areas of the outer and inner event horizons, w_t=2^s[1- 2^-(s+1)], s=d/2, d is the space-time dimension, here d=4, s=2. As r_i approaches r_o in the extreme case the total quantum statistical entropy of Reissner-Nordstrom black holes approaches zero.     

Noncommutative Inspired Reissner-Nordstrom Black Holes in Large Extra Dimensions

Recently, a new noncommutative geometry inspired solution of the coupled Einstein Maxwell field equations including black holes in 4-dimension is found. In this paper, we generalize some aspects of this model to the Reissner Nordstrom （RN） like geometries with large extra dimensions. We discuss Hawking radiation process based on noncommutative inspired solutions. In this framework, existence of black hole remnant and possibility of its detection in LHC are investigated.     

Area Spectrum of Black Holes with Quantum Corrections via Periodicity

Using the Heisenberg uncertainty principle, Bekenstein once claimed that the horizon area of a black hole is quantized with uniform spacing $8\pi l_{p}^{2}$ . This spacing is shown to be corrected with inverse area terms from the perspective of periodicity, which indicates that the area spectrum in this case is no longer evenly spaced. Concretely we study the corrected area spectrum by equaling the motion period of an outgoing wave to the period of gravitational system in Kruskal coordinate with respect to the Euclidean time with consideration of quantum corrections to the semiclassical action. To check our result, we also study the corrected area spectrum in the framework of Generalized Uncertainty Principle. We find the area spectrum produced from the perspective of periodicity takes the same form as the one obtained by the Generalized Uncertainty Principle. As examples, area spectrum with quantum corrections of a Schwarzschild black hole and a Kerr black hole are studied. Our result shows that the formula for area spectrum with quantum corrections is universal though it is not independent of the black hole parameters. In addition, we also discuss the motion period of fermions and find that the area spectrum of a black hole is independent of particle statistics when the black hole is perturbed by an outgoing fermion.     

Remarks on the Equipartition Rule and Thermodynamics of Reissner-Nordstrom Black Holes

In Verlinde’s work, gravity is explained as an entropic force caused by changes in the information associated with the positions of material bodies. In this paper, we investigate the thermodynamic property of Reissner-Nordstrom black holes from the equipartition rule and holographic scenario. As a result, the first law of thermodynamics of the black holes is recovered.     

On Quantum Life of Black Holes

We review some ideas about the quantum physics of black hole information storage and processing in terms of a general phenomenon of quantum criticality.     

Tunneling from a Quantum Black Hole

A quantum black hole has been presented by Kenmoku et al. (1998), and its surface gravity is divergent. We find that its tunneling probability is essentially different from Boltzmann distribution. It is interesting that two peaks appears in the spectrum when the black hole mass decreases close to Planck mass, which is different from black body radiation. PACS: 04.70.Dy     

Quantum Tunneling Radiation of Kerr-NUT Black Hole

Based on particles in a dynamical geometry, extending the Parikh ＇s method of quantum tunneling, radiation, we deeply investigate the quantum tunneling radiation of Kerr-NUT bhck hole. When self-gravitating action, energy conservation, and angular momentum conservation are taken into account, the emission rate of the particle on the event horizon is related to the change of Bekenstein-Hawking entropy and the emission spectrum is not precisely thermal, but is consistent with an underlying unitary theory.     

Quantum Tunneling Radiation of Kerr-NUT Black Hole

Based on particles in a dynamical geometry, extending the Parikh‘s method of quantum tunneling radiation,we deeply investigate the quantum tunneling radiation of Kerr-NUT black hole. When self-gravitating action, energyconservation, and angular momentum conservation are taken into account, the emission rate of the particle on the event horizon is related to the change of Bekenstein-Hawking entropy and the emission spectrum is not precisely thermal, but is consistent with an underlying unitary theory.     

Tunneling Radiation of Massive Vector Bosons from Dilaton Black Holes

It is well known that Hawking radiation can be treated as a quantum tunneling process of particles from the event horizon of black hole. In this paper, we attempt to apply the massive vector bosons tunneling method to study the Hawking radiation from the non-rotating and rotating dilaton black holes. Starting with the Proca field equation that govern the dynamics of massive vector bosons, we derive the tunneling probabilities and radiation spectrums of the emitted vector bosons from the static spherical symmetric dilatonic black hole, the rotating Kaluza-Klein black hole, and the rotating Kerr-Sen black hole. Comparing the results with the blackbody spectrum, we satisfactorily reproduce the Hawking temperatures of these dilaton black holes, which are consistent with the previous results in the literature.     

The Quantum Formulation of Black Hole Area Spectrum and Entropy Spectrum

In this paper, the area spectrum of this static BTZ black hole in different cases (rotating, non-rotating, and extreme) is investigated. The final results show that the spectral formulation is 2πnℏ when this black hole is non-rotating. For the black hole in other two different cases, its spectrum is angular momentum-dependent. Unexpectedly, their area spectra are both equally spaced. What is more, the entropy spectrum is also calculated via the method put forward by Chen et al. However, it is demonstrated that the well known area-entropy law is greatly changed. Above all, the entropy spectrum of this non-rotating BTZ black hole is also equally spaced.     

The Quantum Field Theory Boundaries Applicability and Black Holes Thermodynamics

International Journal of Theoretical Physics - This paper presents a study of the applicability boundary of the well-known quantum field theory. Based on the results of black hole thermodynamics,...     

New Quantum Effect for Vaidya-Bonner-de Sitter Black Holes

The field equations of spin s = 0, 1/2, 1, and2 in the Vaidya–Bonner–de Sitter space-timeare investigated. The results show that the radiativemechanism of massive spin fields depends on the spinstate. We have sufficient reasons to conjecture thatthe effect originates from the quantumergosphere.     

A Planck-Like Problem for Quantum Charged Black Holes

Motivated by the parallelism existing between the puzzles of classical physics at the beginning of the XXth century and the current paradoxes in the search of a quantum theory of gravity, we give, in analogy with Planck's black body radiation problem, a solution for the exact Hawking flux of evaporating Reissner-Nordström black holes. Our results show that when back-reaction effects are fully taken into account the standard picture of black hole evaporation is significantly altered, thus implying a possible resolution of the information loss problem.     

Quantum Statistical Entropy of Six Dimensional Horowitz-Strominger Black Holes

Using the membrane model which is developed from the brick-wall model, we calculated the bosonic and fermionic entropy of 6-d Horowitz-Strominger black holes. The result shows the quantum entropy of such black holes is still proportional to the area of the event horizon only if the cut-off is properly chosen. As for the extreme black holes,the entropy approaches zero.     

The Quantum Corrections to the Entropy of Stationary Axisymmetric Einstein-Maxwell-Dilaton-Axion Black Holes

By using 't Hooft's brick wall model, thecorrections for a massless quantum scalar field to theblack hole entropy are studied in a stationaryaxisymmetric Einstein-Maxwell-dilaton-axion black holespace-time. The free energy and entropy for this case arecalculated; in Hartle-Hawking states, the derivedquantum entropy is composed of the part that has ageometric feature and the part that is logarithmically divergent, and it turns out that thelogarithmic part is related to the characteristicquantities of a black hole.     

Canonical Entropy of Reissner-Nordstrom Black Hole

Recently, Hawking radiation of the black hole has been studied using the tunnel effect method. It is found the radiation spectrum of the black hole is not a strictly pure thermal spectrum. How the departure from pure thermal spectrum affects the entropy? This is a very interesting problem. In this paper, we calculate the partition function by energy spectrum obtained by tunnel effect. Using the relation between the partition function and entropy, we derive the expression of entropy the general charged black hole. In our calculation, we not only consider the correction to the black hole entropy due to fluctuation of energy but also consider the effect of the change of the black hole charges on entropy. We discuss Reissner-Nordstrom black hole and obtain that Reissner-Nordstrom black hole cannot approach the extreme black hole by changing its charges.     

Black Holes: Interfacing the Classical and the Quantum

The central idea of this paper is that forming the black hole horizon is attended with the transition from the classical regime of evolution to the quantum one. We offer and justify the following criterion for discriminating between the classical and the quantum: creations and annihilations of particle-antiparticle pairs are impossible in the classical reality but possible in the quantum reality. In flat spacetime, we can switch from the classical picture of field propagation to the quantum picture by changing the overall sign of the spacetime signature. To describe a self-gravitating object at the final stage of its classical evolution, we propose to use the Foldy–Wouthuysen representation of the Dirac equation in curved spacetimes, and the Gozzi classical path integral. In both approaches, maintaining the dynamics in the classical regime is controlled by supersymmetry.     

Quantum Non-thermal Effect from Black Holes Surrounded by Quintessence

We present a short and direct derivation of Hawking radiation as atunneling process across the horizon and compute the tunneling probability. Considering the self-gravitation and energy conservation, we use the Keski-Vakkuri, Kraus, and Wilczek (KKW) analysis to compute the temperature and entropy of the black holes surrounded by quintessence and obtain the temperature and entropy are different from the Hawking temperature and theBekenstein-Hawking entropy. The result we get can offer a possiblemechanism to deal with the information loss paradox because thespectrum is not purely thermal.