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

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 $\sqrt{2(a^2+Q^2)}/{r^2_+}< \omega< m\varOmega_H+q\varPhi_H$,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.

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 Superradiant stability of five and six-dimensional extremal Reissner–Nordstrom black holes

2021 ◽  
Vol 81 (10) ◽  
Author(s):  
Jia-Hui Huang ◽  
Tian-Tian Cao ◽  
Mu-Zi Zhang
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Numerical Methods ◽  
Effective Potential ◽  
Scalar Perturbation ◽  
Polynomial Equations ◽  
Potential Well ◽  
Massive Scalar ◽  
Higher Dimensional ◽  
The Stability

AbstractWe revisit the superradiant stability of five and six-dimensional extremal Reissner–Nordstrom black holes under charged massive scalar perturbation with a new analytical method. In each case, it is analytically proved that the effective potential experienced by the scalar perturbation has only one maximum outside the black hole horizon and no potential well exists for the superradiance modes. So the five and six-dimensional extremal Reissner–Nordstrom black holes are superradiantly stable. The new method we developed is based on the Descartes’ rule of signs for the polynomial equations. Our result provides a complementary support of previous studies on the stability of higher dimensional extremal Reissner–Nordstrom black holes based on numerical methods.

scholarly journals Analytic study of superradiant stability of Kerr–Newman black holes under charged massive scalar perturbation

2021 ◽  
Vol 81 (5) ◽  
Author(s):  
Jun-Huai Xu ◽  
Zi-Han Zheng ◽  
Ming-Jian Luo ◽  
Jia-Hui Huang
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Effective Potential ◽  
Careful Analysis ◽  
Equation Of Motion ◽  
Analytic Study ◽  
Scalar Perturbation ◽  
Massive Scalar ◽  
Radial Equation ◽  
Newman Black Hole

AbstractThe superradiant stability of a Kerr–Newman black hole and charged massive scalar perturbation is investigated. We treat the black hole as a background geometry and study the equation of motion of the scalar perturbation. From the radial equation of motion, we derive the effective potential experienced by the scalar perturbation. By a careful analysis of this effective potential, it is found that when the inner and outer horizons of Kerr–Newman black hole satisfy $$\frac{r_-}{r_+}\leqslant \frac{1}{3}$$ r - r + ⩽ 1 3 and the charge-to-mass ratios of scalar perturbation and black hole satisfy $$ \frac{q}{\mu }\frac{Q}{ M}>1 $$ q μ Q M > 1 , the Kerr–Newman black hole and scalar perturbation system is superradiantly stable.

Quantum gravity effects on spectroscopy of Kerr-Newman black hole in gravity’s rainbow

2021 ◽  
Author(s):  
Chengzhou Liu ◽  
Jin-Jun Tao
Keyword(s):  
Black Hole ◽  
Quantum Gravity ◽  
Event Horizon ◽  
Planck Scale ◽  
Area Spectrum ◽  
Entropy Spectrum ◽  
Gravity’S Rainbow ◽  
Gravity's Rainbow ◽  
Gravity Effects ◽  
Newman Black Hole

Abstract Quantum gravity effects on spectroscopy for the charged rotating gravity’s rainbow are investigated. By utilizing an action invariant obtained from particles tunneling through the event horizon, the entropy and area spectrum for the modified Kerr-Newman black hole are derived. The equally spaced entropy spectrum characteristic of Bekenstein’s original derivation is recovered. And, the entropy spectrum is independent of the energy of the test particles, although the gravity’s rainbow itself is the energy dependent. Such, the quantum gravity effects of gravity’s rainbow has no influence on the entropy spectrum. On the other hand, due to the spacetime quantum effects, the obtained area spectrum is different from the original Bekenstein spectrum. It is not equidistant and has the dependence on the horizon area. And that, by analyzing the area spectrum from a specific rainbow functions, a minimum area with Planck scale is derived for the event horizon. At this, the area quantum is zero and the black hole radiation stops. Thus, the black hole remnant for the gravity’s rainbow is obtained from the area quantization. In addition, the entropy for the modified Kerr-Newman black hole is calculated and the quantum correction to the area law is obtained and discussed.

COMPUTING THE ENTROPY OF KERR–NEWMAN BLACK HOLE WITHOUT BRICK WALLS METHOD

2008 ◽  
Vol 23 (20) ◽  
pp. 3155-3163 ◽  
Author(s):  
LI-CHUN ZHANG ◽  
YUE-QIN WU ◽  
HUAI-FAN LI ◽  
ZHAO REN
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Uncertainty Principle ◽  
Generalized Uncertainty Principle ◽  
Space Time ◽  
Quantum States ◽  
Brick Wall ◽  
Wall Model ◽  
Brick Wall Model ◽  
Newman Black Hole

By using the entanglement entropy method, the statistical entropy of the Bose and Fermi fields in a thin film is calculated and the Bekenstein–Hawking entropy of Kerr–Newman black hole is obtained. Here, the Bose and Fermi fields are entangled with the quantum states in Kerr–Newman black hole and are outside of the horizon. The divergence of brick-wall model is avoided without any cutoff by the new equation of state density obtained with the generalized uncertainty principle. The calculation implies that the high density quantum states near the event horizon are strongly correlated with the quantum states in black hole. The black hole entropy is a quantum effect. It is an intrinsic characteristic of space–time. The ultraviolet cutoff in the brick-wall model is unreasonable. The generalized uncertainty principle should be considered in the high energy quantum field near the event horizon. From the calculation, the constant λ introduced in the generalized uncertainty principle is related to polar angle θ in an axisymmetric space–time.

scholarly journals Correlation functions in finite temperature CFT and black hole singularities

2021 ◽  
Vol 2021 (6) ◽  
Author(s):  
D. Rodriguez-Gomez ◽  
J.G. Russo
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Correlation Functions ◽  
Finite Temperature ◽  
Proper Time ◽  
Black Brane ◽  
Point Function ◽  
Black Hole Singularity ◽  
Point Correlation ◽  
Scaling Dimension

Abstract We compute thermal 2-point correlation functions in the black brane AdS5 background dual to 4d CFT’s at finite temperature for operators of large scaling dimension. We find a formula that matches the expected structure of the OPE. It exhibits an exponentiation property, whose origin we explain. We also compute the first correction to the two-point function due to graviton emission, which encodes the proper time from the event horizon to the black hole singularity.

scholarly journals Geodesic motion of neutral particles around a Kerr–Newman black hole

2017 ◽  
Vol 34 (23) ◽  
pp. 235008 ◽  
Author(s):  
Chen-Yu Liu ◽  
Da-Shin Lee ◽  
Chi-Yong Lin
Keyword(s):  
Black Hole ◽  
Geodesic Motion ◽  
Neutral Particles ◽  
Newman Black Hole
Sign in / Sign up

Export Citation Format

Share Document