scholarly journals Effective potential of a black hole in thermal equilibrium with quantum fields

1994 ◽  
Vol 49 (10) ◽  
pp. 5257-5265 ◽  
Author(s):  
David Hochberg ◽  
Thomas W. Kephart ◽  
James W. York
Keyword(s):  
Black Hole ◽  
Effective Potential ◽  
Thermal Equilibrium ◽  
Quantum Fields

BACK REACTION IN SCHWARZSCHILD–de SITTER SPACETIME WITH A MASSLESS QUANTUM FIELD

2006 ◽  
Vol 21 (02) ◽  
pp. 169-179
Author(s):  
P. I. KURIAKOSE ◽  
V. C. KURIAKOSE
Keyword(s):  
Black Hole ◽  
Effective Potential ◽  
Thermal Equilibrium ◽  
Back Reaction ◽  
De Sitter Spacetime ◽  
Quantum Field ◽  
De Sitter ◽  
Spacetime Geometry ◽  
Sitter Spacetime ◽  
Massless Quantum

Back reaction in the Schwarzschild–de Sitter black hole in thermal equilibrium with conformal massless quantum field is discussed using the method of York. The presence of quantum field and back reaction ensures the entropy of dressed black hole. In the perturbed spacetime geometry, the nature of the effective potential and the orbits of massless and massive particles are also investigated.

scholarly journals Analysis of Superradiation Stability of Kerr-Newman Black Hole Using Curve integral

2021 ◽  
Author(s):  
Wen-Xiang Chen
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Effective Potential ◽  
Laurent Series ◽  
Potential Well ◽  
Cauchy Integral ◽  
Newman Black Hole

Abstract In this article, a new variable y is added here to expand the results of the above article.We use the properties of the Laurent series and the Cauchy integral. When y is greater than a certain limit, the effective potential of the equation does not have a pole, then there is no potential well outside the event horizon, when p 2(a 2 + Q2)/r2 + < ω < mΩH + qΦH,so the Kerr-Newman black hole is superradiantly stable at that time.

scholarly journals Analysis of Superradiation Stability of Kerr-Newman Black Hole Using Curve integral

2021 ◽  
Author(s):  
Wen-Xiang Chen
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Effective Potential ◽  
Laurent Series ◽  
Potential Well ◽  
Cauchy Integral ◽  
Newman Black Hole

Abstract In this article, a new variable y is added here to expand the results of the above article.We use the properties of the Laurent series and the Cauchy integral. When y is greater than a certain limit, the effective potential of the equation does not have a pole, then there is no potential well outside the event horizon, when p 2(a 2 + Q2)/r2 + < ω < mΩH + qΦH,so the Kerr-Newman black hole is superradiantly stable at that time.

ENTROPY OF SCHWARZSCHILD–de SITTER BLACK HOLE IN NON-THERMAL-EQUILIBRIUM

2001 ◽  
Vol 16 (11) ◽  
pp. 719-723 ◽  
Author(s):  
REN ZHAO ◽  
JUNFANG ZHANG ◽  
LICHUN ZHANG
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Thermal Equilibrium ◽  
Gordon Equation ◽  
Brick Wall ◽  
De Sitter ◽  
Logarithmic Term ◽  
Klein Gordon ◽  
Klein Gordon Equation ◽  
Wall Method

Starting from the Klein–Gordon equation, we calculate the entropy of Schwarzschild–de Sitter black hole in non-thermal-equilibrium by using the improved brick-wall method-membrane model. When taking the proper cutoff in the obtained result, we obtain that both black hole's entropy and cosmic entropy are proportional to the areas of event horizon. We avoid the logarithmic term and stripped term in the original brick-wall method. It offers a new way of studying the entropy of the black hole in non-thermal-equilibrium.

scholarly journals Islands and Page curves for evaporating black holes in JT gravity

2020 ◽  
Vol 2020 (8) ◽  
Author(s):  
Timothy J. Hollowood ◽  
S. Prem Kumar
Keyword(s):  
Black Hole ◽  
Thermal Equilibrium ◽  
Evaporation Rate ◽  
Analytical Description ◽  
Extremal Black Hole ◽  
Thermal Bath ◽  
Slow Evaporation ◽  
Extremal Surface ◽  
Relaxational Process ◽  
Entanglement Structure

Abstract The effect of a CFT shockwave on the entanglement structure of an eternal black hole in Jackiw-Teitelboim gravity, that is in thermal equilibrium with a thermal bath, is considered. The shockwave carries energy and entropy into the black hole and heats the black hole up leading to evaporation and the eventual recovery of equilibrium. We find an analytical description of the entire relaxational process within the semiclassical high temperature regime. If the shockwave is inserted around the Page time then several scenarios are possible depending on the parameters. The Page time can be delayed or hastened and there can be more than one transition. The final entropy saddle has a quantum extremal surface that generically starts inside the horizon but at some later time moves outside. In general, increased shockwave energy and slow evaporation rate favour the extremal surface to be inside the horizon. The shockwave also disrupts the scrambling properties of the black hole. The same analysis is then applied to a shockwave inserted into the extremal black hole with similar conclusions.

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