INCREASE OF HAWKING RADIATION FROM BLACK HOLES BY DIRAC MONOPOLES

1996 ◽  
Vol 05 (04) ◽  
pp. 419-432 ◽  
Author(s):  
YU. P. GONCHAROV ◽  
N.E. FIRSOVA
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Hawking Radiation ◽  
Schwarzschild Black Hole ◽  
Complex Scalar ◽  
Total Luminosity ◽  
Complex Scalar Field

We study a mechanism of increasing Hawking radiation from a black hole by using the example of twisted topologically inequivalent configurations (TICs) of a complex scalar field on the Schwarzschild black hole. Physically this increase is tied with the natural presence of Dirac monopoles on black holes. We satisfy both analytical and numerical considerations and find that twisted TICs give the contribution of order 17% to the total luminosity (summed up over all the TICs) of a black hole.

scholarly journals DIRAC MONOPOLES AND HAWKING RADIATION IN KOTTLER SPACETIME

2002 ◽  
Vol 17 (32) ◽  
pp. 4947-4957
Author(s):  
A. A. BYTSENKO ◽  
YU. P. GONCHAROV
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Energy Density ◽  
Hawking Radiation ◽  
Natural Extension ◽  
Schwarzschild Black Hole ◽  
Complex Scalar ◽  
Radiation Process ◽  
Complex Scalar Field ◽  
The Given

The natural extension of Schwarzschild metric to the case of nonzero cosmological constant Λ known as the Kottler metric is considered and it is discussed under what circumstances the given metric could describe the Schwarzschild black hole immersed in a medium with nonzero energy density. Under the latter situation such an object might carry topologically inequivalent configurations of various fields. The given possibility is analyzed for complex scalar field and it is shown that the mentioned configurations might be tied with natural presence of Dirac monopoles on black hole under consideration. In turn, this could markedly modify the Hawking radiation process.

scholarly journals Wave Function for the Reissner–Nordström Black Hole

1997 ◽  
Vol 12 (20) ◽  
pp. 1491-1505 ◽  
Author(s):  
P. V. Moniz
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Wave Function ◽  
Scalar Field ◽  
Hawking Radiation ◽  
Apparent Horizon ◽  
Complex Scalar ◽  
Charge Rate ◽  
Quantum Behavior ◽  
Complex Scalar Field

We study the quantum behavior of Reissner–Nordström (RN) black holes interacting with a complex scalar field. A Maxwell field is also present. Our analysis is based on M. Pollock's1 method and is characterized by solving a Wheeler–DeWitt equation in the proximity of an apparent horizon of the RN space–time. Subsequently, we obtain a wave function Ψ RN [M,Q] representing the RN black hole when its charge, |Q|, is small in comparison with its mass, M. We then compare quantum-mechanically the cases of (i) Q=0 and (ii) M≥|Q|≠0. A special emphasis is given to the evolution of the mass-charge rate affected by Hawking radiation.

S-MATRICES FOR QUANTUM CHARGED MASSIVE SCALAR PARTICLES ON KERR BLACK HOLES

2001 ◽  
Vol 16 (22) ◽  
pp. 1465-1477 ◽  
Author(s):  
N. E. FIRSOVA
Keyword(s):  
Black Holes ◽  
Scalar Field ◽  
Hawking Radiation ◽  
Massive Scalar ◽  
Numerical Computations ◽  
Scattering Problems ◽  
Complex Scalar ◽  
Scalar Particles ◽  
Complex Scalar Field ◽  
Kerr Black Holes

The results obtained recently on the scattering problems connected with the contribution of the topologically inequivalent configurations of the massless complex scalar field on Kerr black holes to the Hawking radiation are extended to include the massive case as well. The corresponding S-matrices are examined and presented in the form convenient for numerical computations.

scholarly journals On the pattern of black hole information release

2014 ◽  
Vol 29 (09) ◽  
pp. 1450047 ◽  
Author(s):  
I. Y. Park ◽  
F. James
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Scattering Amplitudes ◽  
Cross Section ◽  
Schwarzschild Black Hole ◽  
Complex Scalar ◽  
Mass Growth ◽  
Complex Scalar Field ◽  
Black Hole Information ◽  
Flux Loss

We propose a step towards a resolution to black hole information paradox by analyzing scattering amplitudes of a complex scalar field around a Schwarzschild black hole. The scattering cross-section reveals much information on the incoming state but exhibits flux loss at the same time. The flux loss should be temporary, and indicate mass growth of the black hole. The black hole should Hawking-radiate subsequently, thereby, compensating for the flux loss. By examining the purity issue, we comment on the possibility that information bleaching may be the key to the paradox.

S-MATRICES FOR QUANTUM CHARGED MASSLESS SCALAR PARTICLES ON KERR BLACK HOLES

2000 ◽  
Vol 15 (28) ◽  
pp. 4463-4476
Author(s):  
N. E. FIRSOVA
Keyword(s):  
Black Holes ◽  
Scalar Field ◽  
Hawking Radiation ◽  
Massless Scalar ◽  
Numerical Computations ◽  
Scattering Problems ◽  
Complex Scalar ◽  
Scalar Particles ◽  
Complex Scalar Field ◽  
Kerr Black Holes

The scattering problems that arise when considering the contribution of the topologically inequivalent configurations (TIC's) of the massless complex scalar field on Kerr black holes to the Hawking radiation are studied. The corresponding S-matrices are examined and presented in the form convenient for numerical computations.

Entropy in a d-dimensional charged black hole

2018 ◽  
Vol 33 (27) ◽  
pp. 1850159 ◽  
Author(s):  
Shad Ali ◽  
Xin-Yang Wang ◽  
Wen-Biao Liu
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Hawking Radiation ◽  
Space Time ◽  
Charged Black Hole ◽  
Schwarzschild Black Hole ◽  
Proportionality Coefficient ◽  
Proportional Relation ◽  
Hamiltonian Analysis ◽  
Interior Volume

Christodoulou and Rovelli have shown that the interior volume of a Schwarzschild black hole grows linearly with time. The entropy of a scalar field in this interior volume of a Schwarzschild black hole has been calculated and shown to increase linearly with the advanced time too. In this paper, considering Hawking radiation from a d-dimensional charged black hole, we investigate the proportional relation between the entropy of the scalar field in the interior volume and the Bekenstein–Hawking entropy using the method of our previous work. We also derive this proportionality relation using Hamiltonian analysis and find a consistent result. We then investigate the proportionality coefficient with respect to d and find that it gradually decreases as the dimension of space–time increases.

The entropy evolution of a noncommutative black hole under Hawking radiation

2020 ◽  
Vol 35 (30) ◽  
pp. 2050194
Author(s):  
Peng Wen ◽  
Xin-Yang Wang ◽  
Wen-Biao Liu
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Hawking Radiation ◽  
New Physics ◽  
Evaporation Process ◽  
Final State ◽  
Loss Of Information ◽  
Proportion Function ◽  
Interior Volume

By calculating the entropy of a scalar field in the interior volume of noncommutative black holes and considering an infinitesimal process of Hawking radiation, a proportion function is constructed that reflects the evolution relation between the scalar field entropy and Bekenstein–Hawking entropy under Hawking radiation. Comparing with the case of Schwarzschild black holes, the new physics of this research can be expanded to the later stage of Hawking radiation. From the result, we find that the proportion function is still a constant in the earlier stage of Hawking radiation, which is identical to the case of Schwarzschild black holes. As Hawking radiation goes into the later stage, the behavior of the function will be dominated by the noncommutative effect. In this circumstance, the proportion function is no longer a constant and decreases with the evaporation process. When the noncommutative black hole evolves into its final state with Hawking radiation, the interior volume will converge to a certain value, which implies that the loss of information of the black hole during the evaporation process will finally be stored in the limited interior volume.

The entropy evolution of a Schwarzschild–(Anti) de Sitter black hole

2020 ◽  
Vol 29 (07) ◽  
pp. 2050048
Author(s):  
Xin-Yang Wang ◽  
Yi-Ru Wang ◽  
Wen-Biao Liu
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Hawking Radiation ◽  
Dynamical Variable ◽  
De Sitter ◽  
The One ◽  
Definition Of ◽  
Spherically Symmetry ◽  
Interior Volume

Based on the definition of the interior volume of spherically symmetry black holes, the interior volume of Schwarzschild–(Anti) de Sitter black holes is calculated. It is shown that with the cosmological constant ([Formula: see text]) increasing, the changing behaviors of both the position of the largest hypersurface and the interior volume for the Schwarzschild–Anti de Sitter black hole are the same as the Schwarzschild–de Sitter black hole. Considering a scalar field in the interior volume and Hawking radiation with only energy, the evolution relation between the scalar field entropy and Bekenstein–Hawking entropy is constructed. The results show that the scalar field entropy is approximately proportional to Bekenstein–Hawking entropy during Hawking radiation. Meanwhile, the proportionality coefficient is also regarded as a constant approximately with the increasing [Formula: see text]. Furthermore, considering [Formula: see text] as a dynamical variable, the modified Stefan–Boltzmann law is proposed which can be used to describe the variation of both the mass and [Formula: see text] under Hawking radiation. Using this modified law, the evolution relation between the two types of entropy is also constructed. The results show that the coefficient for Schwarzschild–de Sitter black holes is closer to a constant than the one for Schwarzschild–Anti de Sitter black holes during the evaporation process. Moreover, we find that for Hawking radiation carrying only energy, the evolution relation is a special case compared with the situation that the mass and [Formula: see text] are both considered as dynamical variables.

COMPLEX LINE BUNDLES OVER TWO-SPHERE AND BLACK HOLE PHYSICS

1994 ◽  
Vol 09 (34) ◽  
pp. 3175-3183 ◽  
Author(s):  
YU. P. GONCHAROV ◽  
J.V. YAREVSKAYA
Keyword(s):  
Black Hole ◽  
Black Hole Physics ◽  
Dimensional Space ◽  
Line Bundles ◽  
Complex Line ◽  
Schwarzschild Black Hole ◽  
Complex Scalar ◽  
Complex Scalar Field ◽  
Standing Problem ◽  
Complex Line Bundles

We discuss a long-standing problem of the global topological non-trivial properties of the four-dimensional space-times underlying black hole physics and observe that the standard space-time topology of the ℝ2×S2 form for black hole physics admits topologically inequivalent configurations of a complex scalar field on black hole by virtue of the availability of non-trivial complex line bundles over S2. Each configuration can be labeled by its Chern number n∈ℤ. For the Schwarzschild black hole we formulate an appropriate wave equation for these configurations in massless case and describe its solutions as a first step to study quantum effects for the above configurations within the framework of black hole physics.

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