Stability of the Schwarzschild-de Sitter black hole in the dRGT massive gravity theory

I derive general conditions in order to explain the origin of the Vainshtein radius inside dRGT. The set of equations, which I have called "Vainshtein" conditions are extremal conditions of the dynamical metric (gμν) containing all the degrees of freedom of the theory. The Vainshtein conditions are able to explain the coincidence between the Vainshtein radius in dRGT and the scale [Formula: see text], obtained naturally from the Schwarzschild de-Sitter (S-dS) space inside general relativity (GR). In GR, this scale was interpreted as the maximum distance in order to get bound orbits. The same scale corresponds to the static observer position if we want to define the black hole temperature in an asymptotically de-Sitter space. In dRGT, the scale marks a limit after which the extra degrees of freedom of the theory become relevant.

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Thermal corrections of Born–Infeld–anti-de Sitter black hole in massive gravity

Modern Physics Letters A ◽

10.1142/s0217732319502225 ◽

2019 ◽

Vol 34 (27) ◽

pp. 1950222

Author(s):

Abdul Jawad ◽

Shahid Chaudhary

Keyword(s):

Black Hole ◽

Critical Points ◽

Thermal Fluctuations ◽

Massive Gravity ◽

Vital Role ◽

De Sitter ◽

Logarithmic Corrections ◽

The Impact

The impact of thermal fluctuations on the thermodynamics of Born–Infeld–anti-de Sitter black hole is being investigated. For this purpose, we analyze the consequences of logarithmic corrections on thermodynamics potentials like Helmholtz and Gibbs. We find out the relations for critical points and stability and observe that thermal corrections play a vital role in them.

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Probing correlation between photon orbits and phase structure of charged AdS black hole in massive gravity background

International Journal of Modern Physics A ◽

10.1142/s0217751x19502312 ◽

2019 ◽

Vol 34 (35) ◽

pp. 1950231 ◽

Cited By ~ 3

Author(s):

M. Chabab ◽

H. El Moumni ◽

S. Iraoui ◽

K. Masmar

Keyword(s):

Phase Transition ◽

Black Holes ◽

Black Hole ◽

Phase Structure ◽

Black Hole Solution ◽

Massive Gravity ◽

Direct Link ◽

De Sitter ◽

Thermodynamic Phase ◽

The Impact

The phase structure of charged anti-de Sitter black hole in massive gravity is investigated using the unstable circular photon orbits formalism, concretely we establish a direct link between the null geodesics and the critical behavior thermodynamic of such black hole solution. Our analysis reveals that the radius and the impact parameter corresponding to the unstable circular orbits can be used to probe the thermodynamic phase structure. We also show that the latter are key quantities to characterize the order of Van der Waals-like phase transition. Namely, we found a critical exponent around [Formula: see text]. All these results support further that the photon trajectories can be used as a useful and crucial tool to probe the thermodynamic black holes criticality.

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De Sitter vacua in ghost-free massive gravity theory

Physics Letters B ◽

10.1016/j.physletb.2015.10.012 ◽

2015 ◽

Vol 751 ◽

pp. 19-24 ◽

Cited By ~ 4

Author(s):

Charles Mazuet ◽

Mikhail S. Volkov

Keyword(s):

Massive Gravity ◽

Gravity Theory ◽

De Sitter ◽

De Sitter Vacua

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Greybody factor for massive fermion emitted by a black hole in de Rham-Gabadadze-Tolley massive gravity theory

Physical Review D ◽

10.1103/physrevd.104.084054 ◽

2021 ◽

Vol 104 (8) ◽

Author(s):

P. Boonserm ◽

C. H. Chen ◽

T. Ngampitipan ◽

P. Wongjun

Keyword(s):

Black Hole ◽

Massive Gravity ◽

Gravity Theory ◽

Massive Fermion ◽

De Rham

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Hawking evaporation of black holes in massive gravity

The European Physical Journal C ◽

10.1140/epjc/s10052-020-08678-1 ◽

2020 ◽

Vol 80 (11) ◽

Author(s):

Meng-Shi Hou ◽

Hao Xu ◽

Yen Chin Ong

Keyword(s):

Black Holes ◽

Black Hole ◽

Null Geodesic ◽

Massive Gravity ◽

Late Time ◽

De Sitter ◽

Emission Surface ◽

Metric Function ◽

The Impact ◽

Hawking Evaporation

AbstractWe study the Hawking evaporation of a class of black hole solutions in dRGT massive gravity, in which the graviton mass gives rise to an effective negative cosmological constant. We found that the effective emission surface can be either proportional to the square of the effective AdS length scale, or corresponds to the square of the impact parameter of the null geodesic that falls onto the photon orbit of the black hole. Furthermore, depending on the black hole parameters, the emission surface could switch from one to another as the black hole loses mass during the evaporation process. Furthermore, the black holes can either evaporate completely or become a remnant at late time. Our result is more generally applicable to any asymptotically anti-de Sitter-like black hole solution in any theory whose metric function has a term linear in the coordinate radius, with massive gravity being only a concrete example.

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Reentrant Phase Transitions and Triple Points of Topological AdS Black Holes in Born-Infeld-Massive Gravity

Advances in High Energy Physics ◽

10.1155/2017/3819246 ◽

2017 ◽

Vol 2017 ◽

pp. 1-11 ◽

Cited By ~ 14

Author(s):

Ming Zhang ◽

De-Cheng Zou ◽

Rui-Hong Yue

Keyword(s):

Black Holes ◽

Black Hole ◽

Phase Transitions ◽

Dimensional Space ◽

Massive Gravity ◽

Nonlinear Electrodynamics ◽

Coupling Coefficients ◽

De Sitter ◽

Ads Black Holes ◽

Recent Developments

Motivated by recent developments of black hole thermodynamics in de Rham, Gabadadze, and Tolley (dRGT) massive gravity, we study the critical behaviors of topological Anti-de Sitter (AdS) black holes in the presence of Born-Infeld nonlinear electrodynamics. Here the cosmological constant appears as a dynamical pressure of the system and its corresponding conjugate quantity is interpreted as thermodynamic volume. This shows that, besides the Van der Waals-like SBH/LBH phase transitions, the so-called reentrant phase transition (RPT) appears in four-dimensional space-time when the coupling coefficients cim2 of massive potential and Born-Infeld parameter b satisfy some certain conditions. In addition, we also find the triple critical points and the small/intermediate/large black hole phase transitions for d=5.

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Quasinormal Frequencies of a Two-Dimensional Asymptotically Anti-de Sitter Black Hole of the Dilaton Gravity Theory

Frontiers in Astronomy and Space Sciences ◽

10.3389/fspas.2021.713422 ◽

2021 ◽

Vol 8 ◽

Author(s):

M. I. Hernández-Velázquez ◽

A. López-Ortega

Keyword(s):

Black Hole ◽

Differential Equations ◽

Iteration Method ◽

Gravity Theory ◽

Asymptotic Iteration Method ◽

Two Dimensional ◽

Dilaton Gravity ◽

De Sitter ◽

Second Order Differential Equations ◽

Klein Gordon

We numerically calculate the quasinormal frequencies of the Klein-Gordon and Dirac fields propagating in a two-dimensional asymptotically anti-de Sitter black hole of the dilaton gravity theory. For the Klein-Gordon field we use the Horowitz-Hubeny method and the asymptotic iteration method for second order differential equations. For the Dirac field we first exploit the Horowitz-Hubeny method. As a second method, instead of using the asymptotic iteration method for second order differential equations, we propose to take as a basis its formulation for coupled systems of first order differential equations. For the two fields we find that the results that produce the two numerical methods are consistent. Furthermore for both fields we obtain that their quasinormal modes are stable and we compare their quasinormal frequencies to analyze whether their spectra are isospectral. Finally we discuss the main results.

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Phase transition and entropic force of de Sitter black hole in massive gravity

The European Physical Journal C ◽

10.1140/epjc/s10052-021-08842-1 ◽

2021 ◽

Vol 81 (1) ◽

Author(s):

Yubo Ma ◽

Yang Zhang ◽

Lichun Zhang ◽

Liang Wu ◽

Ying Gao ◽

...

Keyword(s):

Phase Transition ◽

Black Holes ◽

Black Hole ◽

Massive Gravity ◽

Space Time ◽

Black Hole Horizon ◽

Thermodynamic Quantities ◽

Cosmological Horizon ◽

Entropic Force ◽

De Sitter

AbstractIt is well known that de Sitter(dS) black holes generally have a black hole horizon and a cosmological horizon, both of which have Hawking radiation. But the radiation temperature of the two horizons is generally different, so dS black holes do not meet the requirements of thermal equilibrium stability, which brings certain difficulties to the study of the thermodynamic characteristics of black holes. In this paper, dS black hole is regarded as a thermodynamic system, and the effective thermodynamic quantities of the system are obtained. The influence of various state parameters on the effective thermodynamic quantities in the massive gravity space-time is discussed. The condition of the phase transition of the de Sitter black hole in massive gravity space-time is given. We consider that the total entropy of the dS black hole is the sum of the corresponding entropy of the two horizons plus an extra term from the correlation of the two horizons. By comparing the entropic force of interaction between black hole horizon and the cosmological horizon with Lennard-Jones force between two particles, we find that the change rule of entropic force between the two system is surprisingly the same. The research will help us to explore the real reason of accelerating expansion of the universe.

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Circular Geodesics Stability in a Static Black Hole in New Massive Gravity

Galaxies ◽

10.3390/galaxies8010014 ◽

2020 ◽

Vol 8 (1) ◽

pp. 14

Author(s):

Andrés Aceña ◽

Ericson López ◽

Franklin Aldás

Keyword(s):

Black Holes ◽

Black Hole ◽

Massive Gravity ◽

Gravity Theory ◽

Asymptotic Region ◽

Stability Regions ◽

Static Black Hole ◽

Existence And Stability ◽

The Stability ◽

Usual Pattern

We study the existence and stability of circular geodesics in a family of asymptotically AdS static black holes in New Massive Gravity theory. We show that the mathematical sign of the hair parameter determines the existence of such geodesics. For a positive hair parameter, the stability regions follow the usual pattern, with the innermost geodesic being null, unstable, and separated from the horizon, followed by a region of unstable timelike geodesics and then a region of stable timelike geodesics, which extends in the asymptotic region.

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