scholarly journals Initiating the Effective Unification of Black Hole Horizon Area and Entropy Quantization with Quasi-Normal Modes

2014 ◽  
Vol 2014 ◽  
pp. 1-12 ◽  
Author(s):  
C. Corda ◽  
S. H. Hendi ◽  
R. Katebi ◽  
N. O. Schmidt
Keyword(s):  
Black Hole ◽  
Quantum Gravity ◽  
Surface Area ◽  
Normal Modes ◽  
Black Hole Horizon ◽  
Area Spectrum ◽  
Level Spacing ◽  
Horizon Area ◽  
Entropy Quantization

Black hole (BH) area quantization may be the key to unlocking a unifying theory of quantum gravity (QG). Surmounting evidence in the field of BH research continues to support a horizon (surface) area with a discrete and uniformly spaced spectrum, but there is still no general agreement on the level spacing. In the specialized and important BH case study, our objective is to report and examine the pertinent groundbreaking work of thestrictly thermal and nonstrictly thermalspectrum level spacing of the BH horizon area quantization with included entropy calculations, which aims to tackle this gigantic problem. In particular, such work exemplifies a series of imperative corrections that eventually permits a BH’s horizon area spectrum to begeneralizedfrom strictly thermal to nonstrictly thermal with entropy results, thereby capturing multiple preceding developments by launching an effective unification between them. Moreover, the results are significant because quasi-normal modes (QNM) and “effective states” characterize the transitions between the established levels of the nonstrictly thermal spectrum.

scholarly journals Quasi-normal modes and the area spectrum of a near extremal de Sitter black hole with conformally coupled scalar field

2015 ◽  
Vol 30 (11) ◽  
pp. 1550057 ◽  
Author(s):  
Sharmanthie Fernando
Keyword(s):  
Black Hole ◽  
Wave Equation ◽  
Scalar Field ◽  
Normal Modes ◽  
Type Equation ◽  
Area Spectrum ◽  
Massless Scalar ◽  
Massless Scalar Field ◽  
De Sitter ◽  
Quasi Normal Mode

In this paper, we have studied a black hole in de Sitter space which has a conformally coupled scalar field in the background. This black hole is also known as the MTZ black hole. We have obtained exact values for the quasi-normal mode (QNM) frequencies under massless scalar field perturbations. We have demonstrated that when the black hole is near-extremal, that the wave equation for the massless scalar field simplifies to a Schrödinger type equation with the well-known Pöschl–Teller potential. We have also used sixth-order WKB approximation to compute QNM frequencies to compare with exact values obtained via the Pöschl–Teller method for comparison. As an application, we have obtained the area spectrum using modified Hods approach and show that it is equally spaced.

scholarly journals Distributions of extremal black holes in Calabi-Yau compactifications

2020 ◽  
Vol 2020 (10) ◽  
Author(s):  
George Hulsey ◽  
Shamit Kachru ◽  
Sungyeon Yang ◽  
Max Zimet
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Moduli Space ◽  
Black Hole Horizon ◽  
Extremal Black Hole ◽  
Vector Multiplet ◽  
Horizon Area ◽  
Extremal Black Holes

Abstract We study non-supersymmetric extremal black hole excitations of 4d $$ \mathcal{N} $$ N = 2 supersymmetric string vacua arising from compactification on Calabi-Yau threefolds. The values of the (vector multiplet) moduli at the black hole horizon are governed by the attractor mechanism. This raises natural questions, such as “what is the distribution of attractor points on moduli space?” and “how many attractor black holes are there with horizon area up to a certain size?” We employ tools developed by Denef and Douglas [1] to answer these questions.

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.

scholarly journals Maxwell–Boltzmann type Hawking radiation

2017 ◽  
Vol 32 (12) ◽  
pp. 1750071 ◽  
Author(s):  
Youngsub Yoon
Keyword(s):  
Black Hole ◽  
Hawking Radiation ◽  
Radiation Spectrum ◽  
Boltzmann Distribution ◽  
Black Hole Horizon ◽  
Not Given ◽  
Horizon Area ◽  
Einstein Distribution ◽  
Bose Einstein

Twenty years ago, Rovelli proposed that the degeneracy of black hole (i.e. the exponential of the Bekenstein–Hawking entropy) is given by the number of ways the black hole horizon area can be expressed as a sum of unit areas. However, when counting the sum, one should treat the area quanta on the black hole horizon as distinguishable. This distinguishability of area quanta is noted in Rovelli’s paper. Building on this idea, we derive that the Hawking radiation spectrum is not given by Planck radiation spectrum (i.e. Bose–Einstein distribution) but given by Maxwell–Boltzmann distribution.

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