The research on the quantum tunneling characteristics and the radiation spectrum of the stationary axisymmetric black hole

Abstract

At the event horizon and the cosmological horizon of the stationary axisymmetricKerr-Newman black hole in the de Sitter space-time background, the tunneling rate of the charged particles is relevant with Bekenstein-Hawking entropy and the real radiation spectrum is not strictly pure thermal, but consistent with the underlying unitary theory in quantum mechanics. This is a feasible interpretation for the paradox of the black hole information loss. Taking the self-gravitation action, energy conservation, angular momentum conservation and charge conservation into account, the derived radiation spectrum is a correct amendment to the Hawking pure thermal spectrum.Kerr-Newman de Sitter black hole, energy conservation, charge conservation, angular momentum conservation, funneling rate, Bekenstein-Hawking entropyIn 1975, Hawking [1] put forward the paradox of the black hole information loss, which can cast back to the beginning of the 1970s. When no hair theorem of black hole was propounded by Carter and Robinson [2,3] , they also pointed out that most information has lost via the process of the forming of black hole, while the observer can merely study its mass, charge and angular momentum. According to the classical theory, it is relatively easy to comprehend the information loss. For it will permanently exist as a classical black hole, and there is no emitting particle at the horizon, accordingly the black hole information is considered as a conservational constant and, meanwhile, the paradox of the black hole information loss does not occur. On the contrary, the situation is changed via considering quantum effect. In 1974, Hawking proved that there exists thermal radiation in black hole with real temperature, and that its radiation spectrum is pure thermal. He held that vacuum fluctuation causes a quantum tunneling near the horizon, namely a pair of virtual particles spontaneously forms just inside the horizon: the positive energy virtual particle can tunnel out to be real particle, while the negative energy particle is absorbed by the black hole. Or particle pairs form near the outside of horizon: the negative energy virtual particle tunnels inside the ho-

The dynamical model and quantization of the Schwarzschild black hole

“…black hole, Fock representation, mass spectrum, quantum area spectrum, wave function of horizon area After Bekenstein's [1] and Hawking's [2] initial work, the thermodynamics and the statistic mechanics of black holes have been one of the important research areas. Especially in recent years, many authors have already obtained some interesting results on the thermal radiation and the entropy of black holes [3][4][5][6][7][8][9][10][11] . Many conclusions with various different methods revealed that the black hole's entropy is proportional to the horizon area.…”

Quantum Tunneling from Apparent Horizon of Rainbow-FRW Universe

“…Via the point of view, people have put forward several methods, such as anomalies theory, to research on the Hawking radiation [3][4][5][6]. On the other hand, the Hawking radiation could be viewed as the realized particles radiation which becomes from virtual particles inside black holes across the horizon, and Parikh and Wilczek et al have brought forward the semi-classical approximation to research on the tunneling radiation via the point of view [7][8][9][10][11][12][13][14][15]. In the semi-classical approximation method, the WKB approximation is used, so that the tunneling rate ∝ exp(−2 Im S) is applied (S is the first term from the expanding classical action via ), and then, considering the relation between tunneling rate and Hawking temperature ∝ exp(−ω/T ), the Hawking temperature of the horizon can be obtained.…”

Correction value to charged Bekenstein-Hawking black hole entropy

“…This supported the information conservation in Hawking radiation [25,26] . After this, in Parikh framework the primary result of Parikh was generalized to much static and stable spacetime [27][28][29][30][31][32][33][34][35][36][37][38][39][40] . Energy spectrum of any black hole radiation particles is e ,…”