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In this paper, by applying the correction of Lorentz dispersion relation, the fermion tunneling radiation of the stationary axisymmetric Kerr-TAUB-NUT black hole in curved space-time is studied. Based on the modified Lorentz dispersion relation, the revised Rarita-Schwinger equation has been obtained. Then, we get the dynamic equation of fermions via semi-classical theory, which is the modified Hamilton-Jacobi equation. So at the event horizon the tunneling radiation in the space-time of stationary axisymmetric Kerr-TAUB-NUT black hole has been effectively investigated. At last, the modified tunneling radiation and Hawking temperature have been obtained in the same space-time.

According to the Dirac equation and the Rarita-Schwinger equation, the Hamilton-Jacobi equation in curved space-time for the spin 1/2 and 3/2 fermions have been derived. Therefore, we find the Hamilton-Jacobi equation is a fundamental equation in the semiclassical theory. By utilizing this Hamilton-Jacobi equation, we investigate the quantum tunneling radiation from slowly varying Reissner-Nordstrom (R-N) black hole. The results show that the Hawking temperature do not only related to the properties of slowly varying R-N black hole, but also depended on the time. Meanwhile, it finds that the Hamilton-Jacobi equation can help people more easily and effectively calculated thermodynamic properties black hole.

We derive the Hamilton-Jacobi equation from the Dirac equation, then, with the help of the Hamilton-Jacobi equation, the the tunneling radiation behavior of the non-stationary spherical symmetry de Sitter black hole is discussed, at last, we obtained the tunneling rate and Hawking temperature. Our results showed that the Hamilton-Jacobi equation is a fundamental dynamic equation, it can widely be derived from the dynamic equations which describe the particles with any spin. Therefore, people can easy calculate the tunneling behavior from the black holes.

By imposing Bohn-Sommerfeld quantization rule and the laws of black hole thermodynamics to the modified adiabatic covariant action, the spectroscopy of the Kerr black hole is obtained in different coordinate frames. The result shows that the area spectrum is equidistant spacing, and the Bekenstein’s original result \({\Delta } A=8\pi {l_{p}^{2}}\) is also recovered. Especially, in contrast to the quasinormal mode method, in our analysis there is no need to impose the small angular momentum limit for the Kerr black hole spectroscopy.

The Hawking radiation of black hole in Einstein-Proca theory is discussed in this paper. The Einstein-Proca black hole is more general than Reissner-Nordstrom black hole, because Proca field is massive vector field. We calculate several quantum perturbations in this spacetime, and obtain the Hawking radiation at the horizon in Einstein-Proca theory.

In this paper, we use expansion method with eikonal limit to calculate the scalar and Dirac quasinormal modes of black hole with x-matter, which is a spherical symmetrical vacuum black hole in a brane-world scenario. The spacetime includes x-matter as the dark energy. From the results, we find the x-matter accelerates quasinormal frequency and slows damping rate of amplitude.

In this paper, using asymptotic iteration method and eikonal limit, the massive scalar quasinormal modes (QNM) is studied in regular Hayward spacetime, which is much similar to Schwarzschild black hole when r→∞ but there is no singularity at the center. We analyze the QNM frequencies ω by varying the parameter β (it is related to mass of black hole and cosmological constant), spherical harmonic index L and the mass of scalar field m. The results show that the effect of β could lead to the real part of ω increase but the imaginary part decrease, which imply that the existence of cosmological constant would impact on the process of a black hole relaxing after it has been perturbed.

According to the basic rules of finite difference method,we calculate massive charged scalar field quasinormal modes of Reissner-Nordstrom-de Sitter Black Hole with a global monopole, which shows that when electronic quantity of scalar field e is comparatively small, all the factors including angular quantum number, the mass of scalar field, the size of horizon and the breaking scale will influence the frequency spectrum of quasinormal modes. When e is more than some definite critical value, second-order transition will appear and after that the curve of frequency spectrum rises, the black hole is no longer steady, which means when e is greater than some definite critical value, the structure of black hole can be changed. While the size of angular quantum number and breaking scale will influence the happening time of second-order transition. When breaking scale is less than some definite critical value, the second-order transition can be vanished.

In this paper, the dynamical effect of electromagnetic wave is researched in spherical symmetrical Finsler spacetime. The results show that the effect of tangent vector, which can be determined by the angular momentum and energy of observed particles, can’t change the gravitational lens, but can influence the radar echo delay in spherical symmetrical Finsler spacetime. On the other hand, we also use the first order WKB method to study the electromagnetic perturbation with tangent vector effect of Finsler black hole.

The massive scalar quasinormal modes are researched in higher dimensional small Dilatonic spacetime via 6-order WKB approach and finite difference method. In this paper, we study the effect of quasinormal modes frequency in several dimensional cases, and the results show that, if the out event horizon keeps constant, the frequencies are higher but the black holes are more stable when dimension is higher or inner horizon is larger. On the other hand, we also focus on the effect of parameter a and scalar particle mass m. The calculation shows that the effect of m is observably stronger than the effect of a.

A spherically symmetric uncharged regular black hole is proposed in this paper. The black hole’s density in proportion to $r^{3n}e^{-r^{3n+3}}$ , and the curvature tensor in the region of r=0 keep finity. When n=0 in our model, this spacetime is no other than Dymnikova regular black hole. What’s more, there are better properties in this spacetime when n>0. We then discuss the temperature and Hawking radiation of the black hole’s horizon.

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.

Using the method proposed by Banerjee and Majhi, we researched fermion tunneling from cylindrical symmetric black hole, and obtained the correctional entropy. In our work, we first prove that the ratios of the wave function’s components are constants near the horizon, so the reasonable action form of the Dirac equation can then be gotten. From the method beyond semiclassical approximation, we finally calculate the Hawking temperature and correctional entropy.

The quantum tunneling from the apparent horizon of rainbow-FRW universe is studied in this paper. We apply the semi-classical approximation, which is put forward by Parikh and Wilczek et al., to research on the scalar field particles tunneling from the apparent horizon of the rainbow-FRW universe, and then use the spin 1/2 Fermions tunneling theory, which brought forward by Kerner and Mann firstly, to research on the Fermions Hawking radiation via semi-classical approximation. Finally, we discuss the meanings of the quantum effect via Finsler geometry.

In this paper, using the Gravity’s Rainbow theory, we introduce rainbow metric into rainbow Robertson-Walker metric, and obtain a model which depends on the energy of probe particles. Furthermore, we research on an exact inflationary solution of the model, and it can be consistent with the conclusions of observation. The results of our research show that some details in inflation depend on the energy of particles which are observed by observers.

We find a new exact inflationary solution to non-minimally coupled scalar field from a specific H(φ). The inflation is driven by the evolution of the scalar field with a new inflation potential. The spectral index of the scalar density fluctuations ns is consistent with the result of WMAP3 for the power-law flat ΛCDM model. Our solution relaxes the constraint to the quartic coupling constant, e.g. when ξ=103, λ≤8.9×10−11.

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.

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.

Developing Hamilton-Jacobi method, we discuss the Hawking radiation of Kerr-NUT black hole by considering the self-gravitation interaction as well as the energy conservation and angular momentum conservation. The result shows that the factual spectrum deviates from the precisely thermal one and the tunneling rate is related to the change of Bekenstein-Hawking entropy, which is accordant with that obtained by Parikh and Wilczek’s method and gives an interesting correction to the Hawking radiation of the black hole.

Using the Friedmann equation in rainbow Universe, we obtain an exact scalar field Inflationary Solution, which is a modification of the exact scalar field with negative potential −V0+m2φ2/2. Because the rainbow metric is Finsler metric, the result in this paper implies that the research of Finsler geometry in Cosmology should lead to several new physics theories.

Very recent work of Kerner and Mann involving fermions tunnelling from the Rindler space-time and a general non-rotating black hole is extended to the case of Reissner-Nordstrom-anti-de Sitter black hole. Due to the couple between the gravity field and electromagnetic field, we introduce the Dirac equation of the charged particles to determine the action of the radiation. We further consider the correction of the thermal spectrum in the unfixed background space time. It is shown that when the energy and charge conservations are considered, the tunnelling rate of fermions is also related to the change of Bekenstein-Hawking entropy, implying the underlying unitary theory is satisfied.

Very recently, a conceptually clean and economical anomaly cancellation method, based on the initial work of Robinson and Wilczek, on Hawking radiation was proposed. On the basis of this formalism, we investigate Hawking radiation from the higher dimensional Schwarzschild de Sitter and Anti-de Sitter black holes. To describe the observable physics in de Sitter space, we construct the effective field theory between the event horizon and cosmological horizon. Our result shows that when the underlying diffeomorphism symmetries are saved at the quantum level, Hawking radiation, from not only the event horizon but also the cosmological horizon in the higher dimensional space time, can be determined by the covariant compensating fluxes of energy momentum tensor. Meanwhile, we also discuss the exact radiation spectrum by incorporating the self-gravitational interaction and back reaction of the outgoing modes.

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.

The recent work of Robinson and Wilczek that Hawking radiation can be determined by the compensating fluxes is extended to the charged and magnetized Reissner-Nordstrom de Sitter black hole. We reconstruct the electromagnetic field tensor and the Lagrangian of the field corresponding to the source with electric and magnetic charges to redefine an equivalent charge and gauge potential. We construct the effect field theory between the event horizon and cosmological horizon to respectively determine the compensating fluxes from them, which are shown to exactly equal to those of Hawking radiation, by the covariant anomaly cancellation conditions.

Applying Parikh’s semi-classical quantum tunneling method, the tunneling radiation characteristic of the charged particle from the event horizon of the Reissner–Nordstrom–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.

Applying the Hamilton–Jacobi method, we investigate the Hawking radiation as tunneling from the non-stationary Vaidya–Bonner black hole by considering the unfixed background space-time and self-gravitational interaction. The result shows the actual radiation spectrum deviates from the purely thermal one and the tunneling rate is related not only to the change of Bekenstein–Hawking entropy but also to the integral to the black hole mass and charge. This implies information loss is possible.

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.

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.

A thin layer of the event horizon vicinity to the two-dimension black hole with a global monopole is considered as a system of the Casimir type. The energy-momentum tensor is derived in Boulware vacuum, Hartle-Hawking vacuum and Unruh vacuum respectively. The values are derived in the massless scalar field which satisfies the Dirichlet boundary conditions. Using the Wald's axioms, the result is got which is the same with the one derived by the usual regularized methods. Meanwhile, the energy, energy density, and pressure acting on the boundaries at the asymptotically flat background also are calculated too, and from the energy, Casimir force is derived. The Casimir energy and Casimir force are compared respectively in the background before and after radiation.

The tunneling radiation of Ressiner-Nordstrom black hole is studied by developing Hamilton-Jacobi method. The result shows the actual radiation spectrum deviates from the pure thermal one and the tunneling probability are related to the change of Bekenstein-Hawking entropy, which is accordant with Parikh and Wilczek's and gives a new method to correct Hawking pure thermal radiation of Ressiner-Nordstrom 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.

Applying Parikh’s semi-classical tunneling method, Hawking radiation of charged massive particles via tunneling from charged spherical black hole in vacuum for Vector Graviton Metric theory (VGM) of gravitation is investigated. Because the derivation respects conservation of energy and charge, the tunneling rate of particles is relevant to the change of Bekenstein-Hawking entropy and the exact spectrum is not precisely thermal. The result employs an underlying unitary theory.

Applying Parikh's quantum tunneling method, the tunneling characteristics of stationary Kaluza-Klein black hole is researched. The result shows that the tunneling rate across the event horizon of the black hole is relevant to the change of Bekenstein-Hawking entropy and the derived radiation spectrum deviates from pure thermal when the self-gravitation, energy conservation and angular momentum conservation are taken into consideration. Finally, we use the obtained results to reduce to stationary Kerr black hole and static Swarzschild black hole, and find that only ignoring the spectrum at higher energies the tunneling radiation spectrum is consistent with Hawking pure thermal one.

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.

Parikh-Wilzcek’s recent work, which treats the Hawking radiation as semi-classical tunneling process from the event horizon of four dimensional Schwarzshild and Reissner- Nordstrom black hole, indicates that self-gravitation gives a correction to the Hawking precisely thermal spectrum and the tunneling rate is related to the change of Bekenstein- Hawking, but satisfies the underlying unitary theory. In this paper, we extend the model to study the Hawking radiation of charged particles via tunneling from arbitrarily dimensional Reissner-Nordstrom black holes, and obtain the same result as Parikh-Wilzcek’s. Meanwhile, in this framework, we point out that the first law of the black hole thermodynamics is reliable and the information conservation is only suitable for the reversible process.

Taking energy conservation and angular momentum conservation into account, the tunneling radiation characteristics of stationary axisymmetric Sen black hole is studied in this paper with the quantum tunneling method and the results show that the tunneling rate of particle at the event horizon of the black hole is relevant to Bekenstein–Hawking entropy and that the radiation spectrum is not strictly pure thermal.

We discuss the general approach to finding exact inflationary solutions in generalized Einstein theories. These solutions are found by taking the Hubble parameter directly as a function of the field ϕ and then determining the evolution of the expansion scale factor and the potential from it. This method allows the full dynamic behavior of the field to be investigated in terms of the function H(ϕ) without needing to assume that friction terms in the field equations dominate or that the field's kinetic energy is negligible.

In this paper, the quantum tunneling of the non-stationary Kerr-Newman black hole is investigated via Hamilton-Jacobi equation and two types of general tortoise coordinate transformations. The tunneling rates, the Hawking temperatures and radiation spectrums are derived respectively. Our result shows that the new type of general tortoise coordinate transformation is more reasonable.