Stability of motion and thermodynamics in charged black holes in $f(T)$ gravity

Nashed, G. G. L.; Saridakis, Emmanuel N.

doi:10.48550/arxiv.2111.06359

Cited by 2 publications

(2 citation statements)

References 58 publications

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“…Additionally, the stability analysis of the geodesic motion of particles around a BH is an important research topic in the field of gravitational physics, which plays a vital role in exploring the properties of black holes and gravity. Under different contexts of BH, people have conducted extensive research on the stability of black holes through the application of geodesic deviation equation, such as charged black holes in f (T) theory [21], rotating (anti-) de-Sitter black holes in f (R) theory [22], and non-trivial black holes [23], etc [24][25][26][27]. In this paper, we also discuss the stability of the geodesic motion of particles around black holes in the GBD gravity theory.…”

Section: Of 12mentioning

confidence: 99%

Properties of Spherically Symmetric Black Hole in the Framework of GBD Modified Gravitational Theory

Xu¹,

Li²,

Yang³

et al. 2023

Preprint

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The many problems faced by the theory of general relativity (GR) have always motivated us to explore the modified theory of GR. Considering the importance of studying the black hole (BH) entropy and its correction in gravity physics, we study the correction of thermodynamic entropy for a kind of spherically symmetric black holes under the generalized Brans-Dicke (GBD) theory of modified gravity. We derive and calculate the entropy and heat capacity. It is found that when the value of event horizon radius~$r_+$~is small, the effect of the entropy correction term on the entropy is very obvious, while for larger values~$r_+$~, the contribution of the correction term on entropy can be almost ignored. In addition, we can observe that as the radius of the event horizon increases, the heat capacity of BH in GBD theory will change from a negative value to a positive value, indicating that there is a phase transition in black holes. Given that studying the structure of geodesic lines is important for exploring the physical characteristics of a strong gravitational field, we also investigate the stability of the geodesic motion of particles in static spherically symmetric BHs within the framework of GBD theory. Concretely, we analyzes the dependence of the innermost stable circular orbit on model parameters. Also, the geodesic deviation equation is also applied to investigate the stable circular orbit of particles in GBD theory. The conditions for the stability of BH solution and the limited range of radial coordinates required to achieve stable circular orbit motion are given. Finally, we show the locations of stable circular orbits, and obtain the angular velocity, the specific energy and angular momentum of the particles which move in circular orbits.

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Section: Of 12mentioning

confidence: 99%

Properties of Spherically Symmetric Black Hole in the Framework of GBD Modified Gravitational Theory

Xu¹,

Li²,

Yang³

et al. 2023

Preprint

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“…There it has been shown that such modifications to the gravitational action may be able to naturally produce dark matter and dark energy effects [14]- [17]. Stellar structure has also been studied in some detail [18] - [26] as well as black holes [27] - [33]. A nice review of the subject may be found in [34].…”

Section: Introductionmentioning

confidence: 99%

On spherically symmetric vacuum solutions and horizons in covariant $f(T)$ gravity theory

DeBenedictis,

Ilijić,

Sossich

2022

Preprint

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In this paper we study properties that the vacuum must possess in the minimal extension to the teleparallel equivalent of general relativity (TEGR) where the action is supplemented with a quadratic torsion term. No assumption is made about the weakness of the quadratic term although in the weak-field regime the validity of our previously derived perturbative solution is confirmed. Regarding the exact nature of the vacuum, it is found that if the center of symmetry is to be regular, the mathematical conditions on the tetrad at the isotropy point mimic those of general relativity. With respect to horizons it is found that, under very mild assumptions, a smooth horizon cannot exist unless the quadratic torsion coupling, 𝛼, vanishes, which is the TEGR limit (with the Schwarzschild tetrad as its solution). This analysis is then supplemented with computational work utilizing asymptotically Schwarzschild boundary data. It is verified that in no case studied does a smooth horizon form. For 𝛼 > 0 naked singularities occur which break down the equations of motion before a horizon can form. For 𝛼 < 0 there is a limited range of 𝛼 where a vacuum horizon might exist but, if present, the horizon is singular. Therefore physically acceptable black hole horizons are problematic in the studied theory at least within the realm of vacuum static spherical symmetry. These results also imply that static spherical matter distributions generally must have extra restrictions on their spatial extent and stress-energy bounds so as to render the vacuum solution invalid in the singular region and make the solutions finite.

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Stability of motion and thermodynamics in charged black holes in $f(T)$ gravity

Cited by 2 publications

References 58 publications

Properties of Spherically Symmetric Black Hole in the Framework of GBD Modified Gravitational Theory

Properties of Spherically Symmetric Black Hole in the Framework of GBD Modified Gravitational Theory

On spherically symmetric vacuum solutions and horizons in covariant $f(T)$ gravity theory

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