scholarly journals Area spectrum of the Schwarzschild black hole

1996 ◽  
Vol 54 (8) ◽  
pp. 4982-4996 ◽  
Author(s):  
Jorma Louko ◽  
Jarmo Mäkelä
Keyword(s):  
Black Hole ◽  
Area Spectrum ◽  
Schwarzschild Black Hole

Black hole spectroscopy from a class of Plebański and Demiański space–times

2014 ◽  
Vol 92 (1) ◽  
pp. 46-50
Author(s):  
De-Jiang Qi
Keyword(s):  
Black Hole ◽  
Normal Modes ◽  
Kerr Black Hole ◽  
Black Hole Thermodynamics ◽  
Area Spectrum ◽  
Spherically Symmetric ◽  
Adiabatic Invariance ◽  
Schwarzschild Black Hole ◽  
Gravity System ◽  
Area Spectra

Recently, via adiabatic invariance, Majhi and Vagenas quantized the horizon area of the general class of a static spherically symmetric space–time. Very recently, applying the period of the gravity system with respect to the Euclidean time, Zeng and Liu derived area spectra of a Schwarzschild black hole and a Kerr black hole. It is noteworthy that the preceding methods are not useful for the quasi-normal modes. In this paper, based on those works, and as a further study, adopting near horizon approximation, applying the laws of black hole thermodynamics, we would like to investigate the black hole spectroscopy from a class of Plebański and Demiański space–times by using two different methods. The result shows that the area spectrum of the black hole is [Formula: see text], which confirms the initial proposal of Bekenstein, and the result is consistent with that already obtained by Maggiore with quasi-normal modes.

Area and entropy quantization of quantum-corrected Schwarzschild black hole surrounded by quintessence

2019 ◽  
Vol 34 (17) ◽  
pp. 1950091 ◽  
Author(s):  
Md. Shahjalal
Keyword(s):  
Black Hole ◽  
State Parameter ◽  
Minimal Change ◽  
Outgoing Wave ◽  
Area Spectrum ◽  
Length Scale ◽  
Quantum Deformation ◽  
Schwarzschild Black Hole ◽  
Uniform Area ◽  
Entropy Quantization

In this paper, the minimal change in the area and the entropy of quantum-corrected Schwarzschild black hole immersed in the quintessence matter is investigated. Utilizing two different approaches, namely, the periodicity of the outgoing wave and the black hole adiabatic property, the area spectrum is derived, which is independent of both the length scale coming from quantum deformation of the Schwarzschild black hole, and the quintessential state parameter, and which is in agreement with the uniform area spacing originally found by Bekenstein.

BLACK HOLE AREA SPECTRUM AND ENTROPY SPECTRUM VIA QUASINORMAL MODES IN A QUANTUM CORRECTED SPACETIME

2011 ◽  
Vol 26 (39) ◽  
pp. 2963-2971 ◽  
Author(s):  
CHENG-ZHOU LIU
Keyword(s):  
Black Hole ◽  
Imaginary Part ◽  
Quasinormal Modes ◽  
Area Spectrum ◽  
Entropy Spectrum ◽  
Schwarzschild Black Hole ◽  
The Real ◽  
Hole Area ◽  
Test Particles ◽  
Proper Frequency

The area spectrum and entropy spectrum of the modified Schwarzschild black hole in gravity's rainbow are investigated via the quasinormal modes of the black hole. Using the modified Hod's method and Kunstatter's method that employ the proper frequency from the imaginary part other than the real part of the quasinormal modes, the area and entropy spacing of the black hole are calculated. The results obtained from these two methods agree with each other and the equally spaced area and entropy spectrum are derived. The obtained area and entropy spectrum are independent of the energies of test particles and are the same as from the usual Schwarzschild black hole.

scholarly journals THERMODYNAMICS AND SPECTROSCOPY OF SCHWARZSCHILD BLACK HOLE SURROUNDED BY QUINTESSENCE

2013 ◽  
Vol 28 (04) ◽  
pp. 1350003 ◽  
Author(s):  
R. THARANATH ◽  
V. C. KURIAKOSE
Keyword(s):  
Black Hole ◽  
State Parameter ◽  
Area Spectrum ◽  
Thermodynamic Quantities ◽  
Entropy Spectrum ◽  
Schwarzschild Black Hole ◽  
Quantization Rule ◽  
Euclidean Time ◽  
Special Cases ◽  
Spectroscopic Behavior

The thermodynamic and spectroscopic behavior of Schwarzschild black hole surrounded by quintessence are studied. We have derived the thermodynamic quantities and studied their behavior for different values of quintessence parameter. We put the background spacetime into the Kruskal-like coordinate to find the period with respect to Euclidean time. Also assuming that the adiabatic invariant obeys Bohr–Sommerfeld quantization rule, detailed study of area spectrum and entropy spectrum have been done for special cases of the quintessence state parameter. We find that the spectra are equally spaced.

scholarly journals High overtones of dirac perturbations of a Schwarzschild black hole and the area spectrum of quantum black holes

2005 ◽  
Vol 35 (4b) ◽  
pp. 1149-1150 ◽  
Author(s):  
Karlúcio H. C. Castello-Branco ◽  
Roman A. Konoplya ◽  
Alexander Zhidenko
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Area Spectrum ◽  
Schwarzschild Black Hole

scholarly journals Black hole spectroscopy via an action invariance in noncommutative spacetimes

2017 ◽  
Vol 26 (1) ◽  
Author(s):  
ChengZhou Liu ◽  
HaiWen Liu
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Small Mass ◽  
Area Spectrum ◽  
Back Reaction ◽  
Entropy Spectrum ◽  
Schwarzschild Black Hole ◽  
The One ◽  
Original Derivation ◽  
Noncommutative Parameter

AbstractSpectroscopy for a modified Schwarzschild black hole in noncommutative spacetimes is investigated. By utilizing an action invariance of black holes, the equally spaced entropy spectrum characteristic of Bekenstein’s original derivation is recovered. The derived spectrum is independent of the noncommutative parameter θ, and holds for all the existed noncommutative black holes independent of mass. On the other hand, the obtained area spectrum is not always equidistant due to the noncommutativity effects of the modified spacetimes. For large black holes, the equally spaced area spectrum spectrum can be obtained at the leading order in θ. But, for small black holes, the derived area spectrum is not equidistant, and it depends the noncommutative parameter. In addition, the one loop back reaction effect on the spectroscopy of the noncommutative Schwarzschild black hole is discussed. In this calculation, due to the back reaction effect, the equidistant area spectrum can not be obtained for all the noncommutative black holes with both large and small mass. Conversely, the back reaction effect has no influence on the entropy spectrum. The obtained entropy spectrum is equidistant and consistent with the original Bekenstein’s spectrum for all the existed noncommutative Schwarzschild black holes.

The Schwarzschild black hole

2018 ◽  
Author(s):  
Nathalie Deruelle ◽  
Jean-Philippe Uzan
Keyword(s):  
Black Hole ◽  
Gravitational Field ◽  
Equilibrium Configuration ◽  
Original Form ◽  
Schwarzschild Black Hole ◽  
Schwarzschild Metric ◽  
Schwarzschild Geometry

This chapter discusses the Schwarzschild black hole. It demonstrates how, by a judicious change of coordinates, it is possible to eliminate the singularity of the Schwarzschild metric and reveal a spacetime that is much larger, like that of a black hole. At the end of its thermonuclear evolution, a star collapses and, if it is sufficiently massive, does not become stabilized in a new equilibrium configuration. The Schwarzschild geometry must therefore represent the gravitational field of such an object up to r = 0. This being said, the Schwarzschild metric in its original form is singular, not only at r = 0 where the curvature diverges, but also at r = 2m, a surface which is crossed by geodesics.

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