scholarly journals Hawking Radiation-Quasinormal Modes Correspondence for Large AdS Black Holes

2017 ◽  
Vol 2017 ◽  
pp. 1-6 ◽  
Author(s):  
Dao-Quan Sun ◽  
Zi-Liang Wang ◽  
Miao He ◽  
Xian-Ru Hu ◽  
Jian-Bo Deng
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Effective Mass ◽  
Effective Temperature ◽  
Hawking Radiation ◽  
Radiation Spectrum ◽  
Quasinormal Modes ◽  
The Other ◽  
Five Dimensions ◽  
Ads Black Holes

It is well-known that the nonstrictly thermal character of the Hawking radiation spectrum generates a natural correspondence between Hawking radiation and black hole quasinormal modes. This main issue has been analyzed in the framework of Schwarzschild black holes, Kerr black holes, and nonextremal Reissner-Nordstrom black holes. In this paper, by introducing the effective temperature, we reanalyze the nonstrictly thermal character of large AdS black holes. The results show that the effective mass corresponding to the effective temperature is approximatively the average one in any dimension. And the other effective quantities can also be obtained. Based on the known forms of frequency in quasinormal modes, we reanalyze the asymptotic frequencies of the large AdS black hole in three and five dimensions. Then we get the formulas of the Bekenstein-Hawking entropy and the horizon’s area quantization with functions of the quantum “overtone” number n.

scholarly journals Deforming charged black holes with dipolar differential rotation boundary

2020 ◽  
Vol 80 (7) ◽  
Author(s):  
Tong-Tong Hu ◽  
Shuo Sun ◽  
Hong-Bo Li ◽  
Yong-Qiang Wang
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Chemical Potential ◽  
Dimensional Space ◽  
Quasinormal Modes ◽  
Fixed Temperature ◽  
First Case ◽  
Ads Black Holes ◽  
Horizon Geometry ◽  
Black Hole Solutions

Abstract Motivated by the recent studies of the novel asymptotically global $$\hbox {AdS}_4$$AdS4 black hole with deformed horizon, we consider the action of Einstein–Maxwell gravity in AdS spacetime and construct the charged deforming AdS black holes with differential boundary. In contrast to deforming black hole without charge, there exists at least one value of horizon for an arbitrary temperature. The extremum of temperature is determined by charge q and divides the range of temperature into several parts. Moreover, we use an isometric embedding in the three-dimensional space to investigate the horizon geometry. The entropy and quasinormal modes of deforming charged AdS black hole are also studied in this paper. Due to the existence of charge q, the phase diagram of entropy is more complicated. We consider two cases of solutions: (1) fixing the chemical potential $$\mu $$μ; (2) changing the value of $$\mu $$μ according to the values of horizon radius and charge. In the first case, it is interesting to find there exist two families of black hole solutions with different horizon radii for a fixed temperature, but these two black holes have same horizon geometry and entropy. The second case ensures that deforming charged AdS black hole solutions can reduce to standard RN–AdS black holes.

scholarly journals Perturbative and nonperturbative quasinormal modes of 4D Einstein–Gauss–Bonnet black holes

2020 ◽  
Vol 80 (8) ◽  
Author(s):  
Almendra Aragón ◽  
Ramón Bécar ◽  
P. A. González ◽  
Yerko Vásquez
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Imaginary Part ◽  
Quasinormal Modes ◽  
Scalar Fields ◽  
The Other ◽  
Coupling Constant ◽  
De Sitter ◽  
Other Hand

Abstract We study the propagation of probe scalar fields in the background of 4D Einstein–Gauss–Bonnet black holes with anti-de Sitter (AdS) asymptotics and calculate the quasinormal modes. Mainly, we show that the quasinormal spectrum consists of two different branches, a branch perturbative in the Gauss–Bonnet coupling constant $$\alpha $$α and another branch, nonperturbative in $$\alpha $$α. The perturbative branch consists of complex quasinormal frequencies that approximate the quasinormal frequencies of the Schwarzschild AdS black hole in the limit of a null coupling constant. On the other hand, the nonperturbative branch consists of purely imaginary frequencies and is characterized by the growth of the imaginary part when $$\alpha $$α decreases, diverging in the limit of null coupling constant; therefore they do not exist for the Schwarzschild AdS black hole. Also, we find that the imaginary part of the quasinormal frequencies is always negative for both branches; therefore, the propagation of scalar fields is stable in this background.

scholarly journals Hawking Radiation-Quasi-Normal Modes Correspondence and Effective States for Nonextremal Reissner-Nordström Black Holes

2014 ◽  
Vol 2014 ◽  
pp. 1-9 ◽  
Author(s):  
C. Corda ◽  
S. H. Hendi ◽  
R. Katebi ◽  
N. O. Schmidt
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Hawking Radiation ◽  
Radiation Spectrum ◽  
Normal Modes ◽  
Particle Emission

It is known that the nonstrictly thermal character of the Hawking radiation spectrum harmonizes Hawking radiation with black hole (BH) quasi-normal modes (QNM). This paramount issue has been recently analyzed in the framework of both Schwarzschild BHs (SBH) and Kerr BHs (KBH). In this assignment, we generalize the analysis to the framework ofnonextremalReissner-Nordström BHs (RNBH). Such a generalization is important because in both Schwarzschild and Kerr BHs an absorbed (emitted) particle has only mass. Instead, in RNBH the particle has charge as well as mass. In doing so, we expose that, for the RNBH, QNMs can be naturally interpreted in terms of quantum levels for both particle emission and absorption. Conjointly, we generalize some concepts concerning the RNBH's “effective states.”

scholarly journals λ Phase Transition in Horava Gravity

2018 ◽  
Vol 2018 ◽  
pp. 1-14 ◽  
Author(s):  
Wei Xu
Keyword(s):  
Phase Transition ◽  
Black Holes ◽  
Black Hole ◽  
Phase Space ◽  
Five Dimensions ◽  
Ads Black Holes ◽  
Horava Gravity ◽  
Temperature Constraint ◽  
The One ◽  
Similar Phase

We present another example of superfluid black hole containing λ phase transition in Horava gravity. After studying the extended thermodynamics of general dimensional Horava-Lifshitz AdS black holes, it is found that only the one with spherical horizon in four and five dimensions has λ phase transition, which is a line of (continuous) second-order phase transitions and was famous in the discussion of superfluidity of liquid He4. The “superfluid” black hole phase and “normal” black hole phase are also distinguished. Particularly, six-dimensional Horava-Lifshitz AdS black holes exhibit infinitely many critical points in P-ν plane and the divergent points for specific heat, for which they only contain the “normal” black hole phase and the “superfluid” black hole phase disappears due to the physical temperature constraint; therefore there is no similar phase transition. In more than six dimensions, there is no P-ν critical behavior. After choosing the appropriate ordering field, we study the critical phenomena in different planes of thermodynamical phase space. We also calculate the critical exponents, which are the same as the van der Waals fluid.

Five-Dimensional Kerr–AdS Black Holes, First Law and Counterterms

2007 ◽  
Vol 22 (31) ◽  
pp. 5700-5708 ◽  
Author(s):  
Adel Awad
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Vacuum Energy ◽  
Einstein Space ◽  
Subtraction Technique ◽  
Five Dimensions ◽  
First Law Of Thermodynamics ◽  
Ads Black Holes

Using counterterm subtraction technique we calculate the action and other thermodynamical quantities for the general Kerr–AdS black hole in five dimensions. We show that the resulting thermodynamical quantities do satisfy the first law of thermodynamics upon choosing the non-rotating Einstein space as a boundary. Furthermore, the vacuum energies and conformal anomalies calculated from both sides of the AdS/CFT duality match exactly. Comparing this result to previous known results, one is lead to raise the question: why some choices of the boundary metric produce quantities that do not satisfy the first law? Answering such a question will help us understand the relevance of the AdS vacuum energy on the gravity side.

scholarly journals Multioscillating black holes

2021 ◽  
Vol 2021 (5) ◽  
Author(s):  
Takaaki Ishii ◽  
Keiju Murata ◽  
Jorge E. Santos ◽  
Benson Way
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Einstein Gravity ◽  
The Other ◽  
Complex Scalar ◽  
Fixed Energy ◽  
Angular Momenta ◽  
Ads Black Holes ◽  
Hairy Black Holes ◽  
Scalar Hair

Abstract We study rotating global AdS solutions in five-dimensional Einstein gravity coupled to a multiplet complex scalar within a cohomogeneity-1 ansatz. The onset of the gravitational and scalar field superradiant instabilities of the Myers-Perry-AdS black hole mark bifurcation points to black resonators and hairy Myers-Perry-AdS black holes, respectively. These solutions are subject to the other (gravitational or scalar) instability, and result in hairy black resonators which contain both gravitational and scalar hair. The hairy black resonators have smooth zero-horizon limits that we call graviboson stars. In the hairy black resonator and graviboson solutions, multiple scalar components with different frequencies are excited, and hence these are multioscillating solutions. The phase structure of the solutions are examined in the microcanonical ensemble, i.e. at fixed energy and angular momenta. It is found that the entropy of the hairy black resonator is never the largest among them. We also find that hairy black holes with higher scalar wavenumbers are entropically dominant and occupy more of phase space than those of lower wavenumbers.

HAMILTON–JACOBI ANSATZ TO STUDY THE HAWKING RADIATION OF KERR–NEWMAN–KASUYA BLACK HOLES

2007 ◽  
Vol 22 (28) ◽  
pp. 5173-5178 ◽  
Author(s):  
DEYOU CHEN ◽  
SHUZHENG YANG
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Hawking Radiation ◽  
Radiation Spectrum ◽  
Space Time ◽  
Tunneling Rate ◽  
The Self ◽  
Jacobi Method ◽  
Background Space

Taking the self-gravitation interaction and unfixed background space–time into account, we study the Hawking radiation of Kerr–Newman–Kasuya black holes using Hamilton–Jacobi method. The result shows that the tunneling rate is related to the change of Bekenstein–Hawking entropy and the radiation spectrum deviates from the purely thermal one, which is accordant with that obtained using Parikh and Wilczek's method and gives a correction to the Hawking radiation of the black hole.

Covariant perturbations of Schwarzschild black holes in f(R) gravity

2016 ◽  
Vol 26 (06) ◽  
pp. 1750048 ◽  
Author(s):  
Anne Marie Nzioki ◽  
Rituparno Goswami ◽  
Peter K. S. Dunsby
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Wave Equations ◽  
Quasinormal Modes ◽  
The Other ◽  
Primordial Black Holes ◽  
Hole Formation ◽  
High Multipoles ◽  
Theories Of Gravity ◽  
Scalar Perturbations

We consider general perturbations of a Schwarzschild black holes in the context of [Formula: see text] gravity. A reduced set of frame independent master variables are determined, which obey two closed wave equations — one for the transverse, trace-free, tensor perturbations and the other for the additional scalar degree of freedom which characterize fourth-order theories of gravity. We show that for the tensor modes, the underlying dynamics in [Formula: see text] gravity is governed by a modified Regge–Wheeler tensor which obeys the same Regge–Wheeler equation as in General Relativity (GR). We find that the possible sources of scalar quasinormal modes (QNMs) that follow from scalar perturbations for the lower multipoles result from primordial black holes, while higher mass, stellar black holes are associated with extremely high multipoles, which can only be produced in the first stage of black hole formation. Since scalar quasinormal modes are short ranged, this scenario makes their detection beyond the range of current experiments.

scholarly journals TWO-DIMENSIONAL DILATONIC BLACK HOLES AND HAWKING RADIATION

2002 ◽  
Vol 17 (10) ◽  
pp. 609-618 ◽  
Author(s):  
ELIAS C. VAGENAS
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Hawking Radiation ◽  
Radiation Spectrum ◽  
Charged Black Hole ◽  
Two Dimensional ◽  
Nonzero Temperature ◽  
Area Formula ◽  
Tunneling Process ◽  
Standard Methodology

Hawking radiation emanating from two-dimensional charged and uncharged dilatonic black holes — dimensionally reduced from (2+1) spinning and spinless, respectively, BTZ black holes — is viewed as a tunneling process. Two-dimensional dilatonic black holes (AdS(2) included) are treated as dynamical background in contrast to the standard methodology where the background geometry is fixed when evaluating Hawking radiation. This modification to the geometry gives rise to a nonthermal part in the radiation spectrum. Nonzero temperature of the extremal two-dimensional charged black hole is found. The Bekenstein–Hawking area formula is easily derived for these dynamical geometries.

scholarly journals EFFECTIVE TEMPERATURE, HAWKING RADIATION AND QUASINORMAL MODES

2012 ◽  
Vol 21 (11) ◽  
pp. 1242023 ◽  
Author(s):  
CHRISTIAN CORDA
Keyword(s):  
Black Holes ◽  
Quantum Gravity ◽  
Excited States ◽  
Effective Temperature ◽  
Hawking Radiation ◽  
Quantum Physics ◽  
Quasinormal Modes ◽  
Gravity Theory ◽  
Large N ◽  
Physics Of Black Holes

Parikh and Wilczek have shown that Hawking radiation's spectrum cannot be strictly thermal. Such a nonstrictly thermal character implies that the spectrum is also not strictly continuous and thus generates a natural correspondence between Hawking radiation and black hole's quasinormal modes. This issue endorses the idea that, in an underlying unitary quantum gravity theory, black holes result in highly excited states. We use this key point to re-analyze the spectrum of black hole's quasinormal modes by introducing a black hole's effective temperature. Our analysis changes the physical understanding of such a spectrum and enables a re-examination of various results in the literature which realizes important modifications on quantum physics of black holes. In particular, the formula of the horizon's area quantization and the number of quanta of area are modified into functions of the quantum "overtone" number n. Consequently, Bekenstein–Hawking entropy, its sub-leading corrections and the number of microstates, i.e. quantities which are fundamental to realize unitary quantum gravity theory, are also modified. They become functions of the quantum overtone number too. Previous results in the literature are re-obtained in the very large n limit.

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