Hawking Radiation from NUT Kerr Newman Kusuya Black Hole via Effective Action and Covariant Anomalies

Using the theory of the anomalous (chiral) effective action and covariant anomalies method, the Hawking radiation from NUT-Kerr-Newman-Kusuya black hole is researched. In this paper, the electric charge parameter and magnetic monopole parameter are rewritten as equivalent parameter. In addition, we simplify the metric as 1+1 dimensional effective metric. Finally, with the method of anomalous effective action and covariant anomalies respectively, we calculate the chiral covariant current and covariant energy-momentum tensor.     

Dilaton Black Hole Tunneling Radiation in de Sitter Universe

The Hawking radiation via tunneling from the dilaton black hole in de Sitter universe is investigated using Parikh Wilczek＇s method. We show that if the self-gravitational interaction and energy conservation are taken into account, the modified radiation spectrum deviates from exact thermal spectrum and satisfies the unitary theory.     

The Tunneling Radiation Characteristics of Kerr-Newman de Sitter Black Hole

The strictly thermal spectrum in dragging coordinate system and the tunneling radiation characteristics of stationary axisymmetry Kerr-Newman de Sitter black hole is studied. The result shows that the tunneling rates at the event and cosmological horizon are related to the change of Bekenstein-Hawking entropy and that the factual radiation spectrum is not strictly pure thermal. Thus an exact correction to the Hawking thermal spectrum is present.     

Hawking Radiation of the Kerr–Newman Black Hole

Considering the unfixed background space-time and self-gravitational interaction, we review the Hawking radiation of the Kerr–Newman black hole by Hamilton–Jacobi method. The result shows the tunneling probability is related to the change of Bekenstein–Hawking entropy and the radiation spectrum deviates from the precisely thermal one, which is in accordance with Parikh and Wilczek’s result and gives another method to study the Hawking radiation of the black hole.     

Research on Hawking Radiation as Tunneling from Schwarzshild-anti-de Sitter Black Hole

After taking into account energy conservation and the particle’s self-gravitation interaction, Hawking radiation of the massive particle as tunneling from Schwarzshild-anti-de Sitter black hole is studied by using Parikh-Wilczek’s semi-classical quantum tunneling approach. Meanwhile, Hawking radiation as tunneling from the black hole is reexamined by developing Angheben–Nadalini–Vanzo–Zerbini (ANVZ) covariant method to cover energy conservation and the particle’s self-gravitation interaction. Both the results perfectly generalize those obtained by Parikh and Wilczek, and show that the tunneling rate is related to the change of Bekenstein-Hawking entropy, and the factual emission spectrum is not exactly thermal, but satisfies the underlying unitary theory. PACS: 04.70-s, 9760. Lf.     

Spectroscopy of a Kerr–Newman–Kasuya Black Hole

Majhi and Vagenas’s work showed that the entropy spectrum of a spherically symmetric black hole can be obtained without quasinormal modes. In this paper, we extend this work to a Kerr–Newman–Kasuya black hole and discuss its spectra of entropy and area. We find that the spectra are equally spaced and are independent on the parameters of black hole.     

Quantum Tunneling Radiation of Reissner-Nordström de Sitter Black Hole with a Global Monopole

Applying Parikh's quantum tunneling model, we study the quantum tunneling radiation of Reissner-Nordström de Sitter black hole with a global monopole. The result shows that the tunneling rates at the event horizon and the cosmic horizon are related to Bekenstein-Hawking entropy if we take the energy conservation into consideration, and the true radiate spectrum is not precisely thermal.     

Hawking Radiation Arising from the Electromagnetic Fields in the Kerr–Newman Black Hole

Hawking radiation arising from the electromagnetic fields in the Kerr–Newman black hole is studied exactly by using the Newman–Penrose formalism and the tortoise coordinate. It is shown that the thermal radiation spectrum due to the photons in the Kerr–Newman black hole does not depend on the spins of the particles, and the effect is exactly same as that of the Klein–Gordon scalar particles.     

Quasinormal Modes in Double-Charge de Sitter Black Hole

The black hole, as a hot topic to be regarded as a normally research to become a strong evidence for its existence, made more and more people get involved in its research. To calculating the quasinormal modes for massless scalar field and Maxwell’s field in double-charge de Sitter black hole by using WKB approximation method, there is a fact that the speed of weakening electromagnetic perturbation will be reduced. The quasinormal modes in black hole mainly depends on angular quantum number l when its real part is in lower-frequency circumstances. At the same time, imaginary part mainly depends on the overtone number n. When the black hole carries the same electronic quantity, the more the electronic charges have, the smaller the real part and imaginary part of quasinormal modes will be.     

Separability of Dirac equation in higher dimensional Kerr–NUT–de Sitter spacetime

It is shown that the Dirac equations in general higher dimensional Kerr–NUT–de Sitter spacetimes are separated into ordinary differential equations.     

Tunneling Radiation of a Torus-Like Black Hole in Anti-de Sitter Space-Time

An extension of the Parikh-Wilczek's semi-classical quantum tunneling method, the tunneling radiation of the charged particle from a torus-like black hole is investigated. Difference from the uncharged mass-less particle, the geodesics of the charged massive particle tunneling from the black hole is not light-like, but determined by the phase velocity. The derived result shows that the tunneling rate depends on the emitted particle's energy and electric charge, and takes the same functional form as uncharged particle. It proves also that the exact emission spectrum is not strictly pure thermal, but is consistent with the underlying unitary theory. PACS Numbers: 04.70.Dy, 97.60.Lf, 05.30.Ch.     

Tunneling Radiation Characteristic of the Charged Particle from the Reissner–Nordström–anti de Sitter Black Hole

Applying Parikh’s semi-classical quantum tunneling method, the tunneling radiation characteristic of the charged particle from the event horizon of the Reissner–Nordström–anti de Sitter black hole is researched. The result shows the derived spectrum is not purely thermal one, but is consistent with the underlying unitary theory, which gives a might explanation to the information loss paradox and is the correct amendment to the Hawking radiation.     

Entropy in Kerr–de Sitter Black Holes with Spin Fields

Generalized master equations due to spin fields are given. We obtain the entropy of electromagnetic, gravitational, Dirac, and scalar fields in a unified form by using the improved brick-wall method—membrane model. The results show that, as the cutoff is properly chosen, the entropy in the black hole satisfies the Bekenstein–Hawking area formula.     

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     

Strings in Kerr–Newman Black Holes

We study the evolution of strings in the equatorial plane of a Kerr–Newman black hole. Writing the equations of motion and the constraints resulting from Hamilton's principle, three classes of exact solutions are presented, for a closed string, encircling the black hole. They all depend on two arbitrary integration functions and two constants. A process for extracting energy is examined for the case of one of the three families of solutions. This is the analogue of the Penrose process for the case of a particle.     

A Note on Black Hole Information Paradox in de Sitter Spacetimes

The possibility of stable or quasi-stable Planck mass black hole remnants as solution to the black hole information paradox is commonly believed phenomenologically unacceptable. Since we need a black hole remnant for every possible initial state, the number of remnants is expected to be infinite and that would lead to remnant pair production in any physical process with a total available energy roughly exceeding the Planck mass. In this note I point out that a positive cosmological constant of the Universe would naturally lead to an upper bound on the number of possible remnants.     

A Note on Black Hole Information Paradox in de Sitter Spacetimes

The possibility of stable or quasi-stable Planck mass black hole remnants as solution to the black hole information paradox is commonly believed phenomenologically unacceptable. Since we need a black hole remnant for every possible initial state,the number of remnants is expected to be infinite and that would lead to remnant pair production in any physical process with a total available energy roughly exceeding the Planck mass. In this note I point out that a positive cosmological constant of the Universe would naturally lead to an upper bound on the numberof possible remnants.     

Hawking Radiation of Charged Particles via Tunneling from a Cylindrically Symmetric Black Hole in Anti-de Sitter Space-Time

Applying Parikh-Wilzcek＇s semi-classical quantum tunneling model, we study the Hawking radiation of charged particles as tunneling from the event horizon of a cylindrically symmetric black hole in anti-de Sitter space-time. The derived result shows that the tunneling rate of charged particles is related to the change of Bekenstein-Hawking entropy and that the radiation spectrum is not strictly pure thermal after taking the black hole background dynamical and self-gravitation interaction into account, but is consistent with the underlying unitary theory.     

R-Charged Black Hole and Neutrino Oscillation

In this paper we consider neutrino oscillation in general curved space-times. Then we calculate neutrino oscillation length in the R-charged black hole background, which is a five dimensional space-time, and compare it with the results of various backgrounds. We obtain effect of the electrical charge corresponding to the chemical potential on the oscillation length.