Modification to tunneling radiation of arbitrary spin fermions in stationary axisymmetric Sen black hole space–time

Considering the modified Lorentz dispersion relation, combined with the Dirac equation and Rarita–Schwinger equation of fermions in stationary axisymmetric Sen black hole space–time, the fermion tunneling radiation of the black hole is modified accurately, and meaningful physical quantities such as the modified fermion tunneling rate, event horizon temperature, and entropy of the black hole are obtained. The discussion of the conclusions shows that the effect of the Lorentz dispersion relation and Lorentz violation theory on particle dynamics must be considered in curved space–time during the study of quantum theory and Hawking tunneling radiation.

Phenomenological modification of horizon temperature

In this paper, a study of the accelerated expansion problem of the large scale universe is presented. To derive Friedmann like equations, describing the background dynamics of the recent universe, we take into account, that it is possible to interpret the spacetime dynamics as an emergent phenomenon. It is a consequence of the deep study of connection between gravitation and thermodynamics. The models considered are based on phenomenological modifications of the horizon temperature. In general, there are various reasons to modify the horizon temperature, one of which is related to the feedback from the spacetime on the horizon, generating additional heat. In order to constrain the parameters of the models, we use Om analysis and the constraints on this parameter at z = 0.0, z = 0.57 and z = 2.34.

GENERALIZED SECOND LAW OF THERMODYNAMICS IN WORMHOLE GEOMETRY

In this paper, the generalized second law (GSL) of thermodynamics is studied at the apparent horizon of the evolving wormhole. It is shown that the GSL holds at the apparent horizon of the evolving wormhole together with the assumption that the horizon temperature is equal to the temperature of the phantom energy.

TOPOLOGICAL INTERPRETATION OF THE HORIZON TEMPERATURE

A class of metrics gab(xi) describing spacetimes with horizons (and associated thermodynamics) can be thought of as a limiting case of a family of metrics gab(xi;λ)without horizons when λ→0. We construct specific examples in which the curvature corresponding gab(xi;λ) becomes a Dirac delta function and gets concentrated on the horizon when the limit λ→0 is taken, but the action remains finite. When the horizon is interpreted in this manner, one needs to remove the corresponding surface from the Euclidean sector, leading to winding numbers and thermal behavior. In particular, the Rindler spacetime can be thought of as the limiting case of (horizon-free) metrics of the form [g00=ε2+a2x2; gμν=-δμν] or [g00=-gxx=(ε2+4a2x2)1/2, gyy=gzz=-1] when ε→0. In the Euclidean sector, the curvature gets concentrated on the origin of tE-x plane in a manner analogous to Aharanov–Bohm effect (in which the vector potential is a pure gauge everywhere except at the origin) and the curvature at the origin leads to nontrivial topological features and winding number.

ON ARITHMETIC DETECTION OF GREY PULSES WITH APPLICATION TO HAWKING RADIATION

Micron-sized black holes do not necessarily have a constant horizon temperature distribution. The black hole remote-sensing problem means to find out the "surface" temperature distribution of a small black hole from the spectral measurement of its (Hawking) grey pulse. This problem has been previously considered by Rosu, who used Chen's modified Möbius inverse transform. Here, we hint on a Ramanujan generalization of Chen's modified Möbius inverse transform that may be considered as a special wavelet processing of the remote-sensed grey signal coming from a black hole or any other distant grey source.