A New Method to Study Hawking Radiation of Charged Particle from Stationary Axisymmetric Sen Black Hole

Taking the self-gravitation interaction and energy conservation,charge conservation and angular momentum conservation into accpunt, we discuss the tunnelling characteristics of the charged particle from Sen black hole by the Hamilton-Jacobi method. The result shows that the tunnelling probability is related to the change of Bekenstein-Hawking entropy, and the actual radiation spectrum deviates from the pure thermal one, which is consistent with the result of Parikh and Wilczek and gives a new method to correct the Hawking pure thermal spectrum of Sen black hole.     

Hawking Radiation from the Horowitz-Strominger Black Hole

When a black hole radiates particles, it losses energy and shrinks, the horizon contracts from its original radius to a new smaller radius. This leads to the separation between the initial and final radii, which sets the barrier for the particles to tunnel We develop the work of Parikh [Phys. Rev. Lett. 85 (2000) 5042; Gen. Rel. Grav. 36 (2004) 2419] to a Horowitz-Strominger black hole, i.e. applying the Wentzel-Kramers-Brillouin approximation and semi-classical method to calculate the rate of the Hawking radiation. The result agrees with Г～e^-21mf=e^△SBH. It is also proven that the energy spectrum deviates from exact thermality.     

Hawking Radiation from the Cylindrical Symmetric Black Hole via Covariant Anomaly

Hawking radiation from the cylindrical symmetric black hole, which is asymptotically anti-de Sitter not only in the transverse direction but also in the string or membrane direction, is discussed from the anomaly point of view. We implement the covariant anomaly cancellation method, the more refined formalism that was proposed by Banerjee and Kulkarni recently than the initial work of Robinson et al., to discuss the near-horizon gauge and gravitational anomalies. Our result shows that Hawking radiation from the cylindrical configurations with horizons also can be reproduced by the anomaly cancellation method.     

Hawking Radiation as Tunneling from Garfinkle-Horowitz-Stromingen Dilaton Black Hole

Applying quantum tunneling method, this paper has studied the Hawking radiation of Garfinkle-Horowitz-Stromingen dilaton black hole. In this way, the emission rates of massless particles and massive particles tunneling across the event horizon of black holes is obtained. The result shows that the radiation spectrum of these two different kinds of outgoing particles is related to the change of Bekenstein-Hawking entropy, which is no longer precisely thermal.     

Unthermal Charged Massive Hawking Radiation from a Reissner-Nordström Black Hole

Using Damour-Ruffini’s method, the massive charged particles’ Hawking radiation from a Reissner-Nordström black hole is investigated. When the back-reaction of particles’ energy and charge to spacetime is considered, we get the unthermal spectrum. It is possible that the information will get out from the black hole with the corrected spectrum. It can be used to explain the information loss paradox, and the underlying unitary theory will be satisfied. The same conclusion as the works finished before can be drawn. However, our work is different from them, and the method is more simple and explicit.     

Dirac Particles＇ Hawking Radiation from a Schwarzschild Black Hole

Considering energy conservation and the backreaction of particles to spacetime, we investigate the massless/massive Dirac particles＇ Hawking radiation from a Schwarzschild black hole, The exact expression of the emission rate near the horizon is obtained and the result indicates that Hawking radiation spectrum is not purely thermal. The result obtained is consistent with the results obtained before. It satisfies the underlying unitary theory and offers a possible mechanism to explain the information loss paradox. Whereas the improved Damour-Rufflni method is more concise and understandable,     

Tunnelling Effect and Hawking Radiation from a Vaidya Black Hole

We extend Parikh＇s study to the non-stationary black hole. As an example of the non-stationary black hole, we investigate the tunnelling effect and Hawking radiation from a Vaidya black hole whose Bondi mass is identical to its mass parameter. The Hawking radiation is considered as a tunnelling process across the event horizon and we calculate the tunnelling probability. It is found that the is the function of Bondi mass re（υ）. result is different from Parikh＇s study because dr H/dυ     

Hawking Radiation of Charged and Magnetized Particles from the Kerr-Newman-Kasuya Black Hole via Covariant Anomaly

Hawking radiation of a particle with electric and magnetic charges from the Kerr-Newman-Kasuya black hole is discussed in the dragging coordinate frame via the anomaly cancellation method, initiated by Robinson and Wilczek. We redefine an equivalent charge of the charged and magnetized black hole by reconstructing the electromagnetic field tensor. We adopt the refined covariant anomaly cancellation method to determining the compensating fluxes of charge flow and energy momentum tensor, which are proved to precisely match with those of the 2-dimensional blackbody radiation at the Hawking temperature with an appropriate chemical potential.     

Anomalies and Hawking Radiation of NUT-Kerr-Newman de Sitter Black Hole

Hawking radiation of NUT-Kerr-Newman de Sitter black hole is studied via anomalous point of view in this paper. The results show that the charged current and energy-momentum tensor fluxes, to restore gauge invariance and general coordinate covariance at the quantum level in the effective field theory, are exactly equal to those of Hawking radiation from the event horizon (EH) and the cosmological horizon (CH) of NUT-Kerr-Newman de Sitter black hole, respectively.     

Hawking Radiation of the Charged Particle Via Tunneling from the Reissner-Nordström Black Hole

Since Parikh and Wilczek proposed a semiclassical tunneling method to investigate the Hawking radiation of static and spherically symmetric black holes, the method has been extensively developed to study various black holes. However, in almost all of the subsequent papers, there exists a important shortcoming that the geodesic equation of the massive particle is defined inconsistently with that of the massless particle. In this paper, we propose a new idea to reinvestigate the tunneling radiation from the event horizon of the Reissner-Nordström black hole. In our treatment, by starting from the Lagrangian analysis on the action, we redefine the geodesic equation of the massive and massless particle via tunneling from the event horizon of the Reissner-Nordström black hole, which overcomes the shortcoming mentioned above. The highlight of our work is a new and important development for the Parikh-Wilczek’s semiclassical tunneling method.     

Where Does Hawking Radiation of a Dynamical Black Hole Come from?

Using the gravitational anomaly method proposed by Robinson and Wilczek, Hawking radiation from the apparent horizon of a Vaidya black hole is calculated. The thermodynamics can be built successfully on the apparent horizon. In the meantime, when a time-dependent perturbation is given to the apparent horizon, the first law of thermodynamics can also be constructed successfully at a new supersurface near the apparent horizon. The expressions of the characteristic position and temperature are consistent with the previous result where the viewpoint is that the thermodynamics should be built on the event horizon. Based on the results, the thermodynamics should be constructed on the apparent horizon exactly while the event horizon thermodynamics is just one of the perturbations near the apparent horizon.     

Corrected Hawking Tunneling Radiation in the Higher Dimensional Reissner-Nordström Black Hole

Based on the generalized uncertainty principle, in which the quantum gravitational effects are properly taken in to account, the corrected Bekenstein-Hawking entropy of the higher dimensional Reissner-Nordström black hole, up to the square order of Planck length, has been calculated. Using the corrected entropy, the black hole radiation probability has been calculated in the tunneling formalism, which is corrected up to the same order of the Planck length and a generalized quantum tunneling through the event horizon of the black hole is obtained.     

On Hawking Radiation via Tunneling from the Reissner-Nordström-de Sitter Black Hole with a Global Monopole

In this paper, we start from the Lagrangian analysis on the action to naturally produce the geodesic equation of the massive particle via tunneling. Then, basing on the new definition for the geodesic equation, we revisit the Hawking radiation of the charged massive particle via tunneling from the Reissner-Nordström-de Sitter black hole with a global monopole. In our treatment, the geodesic equation of the charged massive particle is defined uniformly with that of the massless particle, which overcomes the shortcomings of its previous definition, and is more suitable for the tunneling mechanism. It is noteworthy that, the highlight of our work is a new and important development of the Parikh-Wilczek’s tunneling method.     

Radiation Energy Flux and Radiation Power of Schwarzschild Black Hole

Applying the entropy density near the event horizon, we obtained the result that the radiation energy flux of the black hole is always proportional to the quartic of the temperature of its event horizon. That is to say, the thermal radiation of the black hole always satisfies the generalized Stefan–Boltzmann law. The derived generalized Stefan–Boltzmann coefficient is no longer a constant. When the cut-off distance and the thin film thickness are both fixed, it is a proportional coefficient which is related to the black hole mass, the kinds of radiation particles and space–time metric near the event horizon. In this paper, we have put forward a thermal particle model in curved space–time. By this model, the result has been obtained that when the thin film thickness and the cut-off distance are both fixed, the radiation energy flux received by observer far away from the Schwarzschild black hole is proportional to the average radial effusion velocity of the radiation particles in the thin film, and inversely proportional to the square of the distance between the observer and the black hole.     

Hawking Radiation of Photons in a Vaidya–de Sitter Black Hole

Hawking evaporation of photons in a Vaidya–de Sitter black hole is investigated by using the method of generalized tortoise coordinate transformation. Both the location and the temperature of the event horizon depend on the time. It is shown that Hawking radiation of photons exists only for the complex Maxwell scalar ₀ in the advanced Eddington–Finkelstein coordinate system. This asymmetry of Hawking radiation for different components of Maxwell fields probably arises from the asymmetry of spacetime in the advanced Eddington–Finkelstein coordinate system. It is shown that the black body radiant spectrum of photons resembles that of Klein–Gordon particles.     

Kerr-Newman-Kasuya Black Hole Tunnelling Radiation

The radiation of black hole contributes to the shrinking of the event horizon such that the background spacetime should not be fixed. In this study we take into account the self-gravitation effect to study the radiation of Kerr Newman-Kasuya black hole as tunnelling. Using the facts of energy conservation and angular momentum conservation we derive the tunnelling rate and show that the spectrum of the radiation as tunnelling is not purely thermal.     

Quantum Tunnelling and Hawking Radiation of Schwarzchild-Anti-de Sitter Black Hole with Topological Defect

We extend Parikh＇s recent work to Schwarzchild-anti-de Sitter black hole with topological defect whose Arnowitt-Deser-Misner （ADM） mass is no longer identical to its mass parameter. We view the Hawking radiation as a tunnelling process across the event horizon and the cosmological horizon. From the tunnelling probability, we find a leading correction to the semi-classical emission rate. The result employs an underlying unitary theory.     

Hawking Radiation via Tunnelling from Arbitrarily Dimensional Schwarzschild Black Holes

We extend Parikh＇s recent work to the arbitrarily dimensional Schwarzschild black holes whose Arnowitt-Deser-Misner （ADM） mass is identical to its mass parameter. We view Hawking radiation as a tunnelling process across the event horizon. From the tunnelling probability we also find a leading correction to the semiclassical emission rate. The result consists with an underlying unitary theory.     

Entropy of Kerr-Newman Black Hole to All Orders in the Planck Length

Using the quantum statistical method, the difficulty of solving the wave equation on the background of the black hole is avoided. We directly solve the partition functions of Bose and Fermi field on the background of an axisymmetric Kerr-Newman black hole using the new equation of state density motivated by the generalized uncertainty principle in the quantum gravity. Then near the black hole horizon, we calculate entropies of Bose and Fermi field between the black hole horizon surface and the hypersurface with the same inherent radiation temperature measured by an observer at an infinite distance. In our results there are not cutoffs and little mass approximation introduced in the conventional brick-wall method. The series expansion of the black hole entropy is obtained. And this series is convergent. It provides a way for studying the quantum statistical entropy of a black hole in a non-spherical symmetric spacetime.     

New Coordinates for the Evaporating Vaidya Black Hole

Drawbacks of the ingoing Eddington-Finkelstein coordinates in describing the quantum thermal properties of the evaporating Vaidya black hole are presented. A new coordinate system we proposed previously [Acta Phys. Sin. 46 （1997） 1273] is employed. In this new coordinate system, the thermal radiation temperature of the Vaidya black hole is discussed again with the back reaction method.