Black hole motion in Euclidean space as a diffusion process

Ropotenko, K.

doi:10.1103/physrevd.85.104032

Cited by 5 publications

(4 citation statements)

References 9 publications

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“…Recently, Ropotenko [20] showed that, by analogy with conventional Landau quantization, quantization of black hole is nothing but the Landau quantization. [21] This method is based on the standard commutation rules of quantum mechanics and makes use of the fundamental properties of the Euclidean Rindler space. As is wellknown, in transforming from Schwarzschild to Euclidean Rindler coordinates the Schwarzschild time transforms to a periodic angle w. This allows one to introduce the Hawking temperature T H .…”

Section: Area and Entropy Quantization For Non-extremal Gb Ds Black H...mentioning

confidence: 99%

Area and Entropy Spectrum of Gauss—Bonnet Gravity in de Sitter Space-Times for Black Hole Event Horizon

Chen¹,

Ren²

2013

Commun. Theor. Phys.

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In this paper, we use the modified Hod's treatment and the Kunstatter's method to study the horizon area spectrum and entropy spectrum in Gauss-Bonnet de-Sitter space-time, which is regarded as the natural generalization of Einstein gravity by including higher derivative correction terms to the original Einstein-Hilbert action. The horizon areas have some properties that are very different from the vacuum solutions obtained from the frame of Einstein gravity. With the new physical interpretation of quasinormal modes, the area/entropy spectrum for the event horizon for nearextremal Gauss-Bonnet de Sitter black holes are obtained. Meanwhile, we also extend the discussion of area/entropy quantization to the non-extremal black holes solutions.

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Section: Area and Entropy Quantization For Non-extremal Gb Ds Black H...mentioning

confidence: 99%

Area and Entropy Spectrum of Gauss—Bonnet Gravity in de Sitter Space-Times for Black Hole Event Horizon

Chen¹,

Ren²

2013

Commun. Theor. Phys.

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“…They provide the theory of diffusion problems in the Schwarzschild and Kruskal-Szekeres manifolds to represent the Black Holes. From the Bunster-Carlip equation, Ropotenko has derived a diffusion equation of black hole on Kerr-Newman space-time, and its solution has a Gaussian distribution form [31]. He also found the entropy of the diffusion process as well as the Bekenstein-Hawking entropy [32].…”

Section: Introductionmentioning

confidence: 99%

Brownian Motion Around Black Hole

Romadani¹

2021

Advances in Social Science, Education and Humanities Research

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Brownian motion theory is always challenging to describe diffusion phenomena around a black hole, with the main issue is how to extend the classical theory of Brownian motion to the general relativity framework. In this study, we extended the Brownian motion theory in a curved space-time come from a strong gravitational field on the Schwarzschild black hole. The Brownian motion theory in Schwarzschild space-time was derived by using the Fokker-Planck equation, and the stationary solution was analyzed by Ito, Stratonovich-Fisk, and Hanggi-Klimontovich Approach. The numerical result was found that the Brownian motion in Schwarzschild space-time 1   was reduced to the standard Brownian motion in Newtonian classical theory. According to the Hanggi-Klimontovich approach for 1   the result showed a consistent with the relativistic Maxwell distribution. The Fokker-Planck equation in Schwarzschild space-time was also formulated as a generalization of relativistic Brownian motion theory. This work could open a promising interpretation to formulate the diffusion phenomena around a massive object in the general relativity framework.

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“…In [1], I derived a diffusion equation for a Schwarzschild black hole from the Bunster-Carlip equations and showed that the black hole evolution in Euclidean sector exhibits a diffusion process. Namely I showed that the Bunster-Carlip equationsh i ∂ψ ∂t + Mψ = 0,…”

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confidence: 99%

“…So, as in the case of a Schwarzschild black hole, one can introduce the corresponding temporal Θ and spatial τ coordinates for a Kerr-Newman black hole. I define the Hamiltonian of a Kerr-Newman black hole as that of a particle moving in the potential U = ΩJ + 1 2 ΦQ,…”

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confidence: 99%