Charged star in (2+1)-dimensional gravity

Banerjee, Ayan; Rahaman, Farook; Chattopadhyay, Tanuka

doi:10.1007/s10509-015-2267-x

Cited by 3 publications

(5 citation statements)

References 29 publications

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“…Let us now explore the physical features of our model. The Einstein field equations must in this case satisfy certain physical requirements [19]. For the interior solution, the density ρ and the pressures P r and P t must be positive and finite everywhere.…”

Section: Interior Solutionmentioning

confidence: 99%

“…There are various choices for E(r) but the acceptable ones are those that leads to a positive and continuous field strength tensor in the interior region. Thus we choose the following exponential function [19]:…”

Section: The Interior Solution For Charged Black Holesmentioning

confidence: 99%

“…Finding the interior metric of such an object can be useful for describing the interior region of stellar objects. In [19,20], simplified models such as interior solutions for BTZ black holes for charged and uncharged cases are suggested based on the assumption that the interior region of these black holes are filled with an anisotropic fluid. In this study, we obtain exact interior solutions for (d + 1)-dimensional black holes with toroidal horizons.…”

Section: Introductionmentioning

confidence: 99%

“…Equations (19) shows that M is the conserved charge and the mass of the (d + 1)-dimensional black holes with toroidal horizons. The calculation procedures for the conserved charges of some other black holes may be found in [26].…”

Section: Introductionmentioning

confidence: 99%

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Black holes with toroidal horizons in ( $$d+1$$ d + 1 )-dimensional space-time

Sharifian¹,

Mirza²,

Mirzaiyan³

2017

Gen Relativ Gravit

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We investigate black holes with toroidal horizons in (d + 1)-dimensional space-time. Using the solution phase space method, we calculated conserved charges for these black holes before exploring some features of this metric including its entropy and thermodynamic quantities. Another aspect of the study involves obtaining a general exact static interior solution for uncharged black holes with toroidal horizons in (d + 1)-dimensional space-time. Finally, an interior solution for charged black holes is obtained.

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Section: Interior Solutionmentioning

confidence: 99%

Section: The Interior Solution For Charged Black Holesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Black holes with toroidal horizons in ( $$d+1$$ d + 1 )-dimensional space-time

Sharifian¹,

Mirza²,

Mirzaiyan³

2017

Gen Relativ Gravit

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show abstract

“…In the relativistic astrophysics, it is fascinating to investigate the static anisotropic objects. This investigation leads to describe the interior region of stellar objects [42] [43] [44].…”

mentioning

confidence: 99%

Higher-dimensional black hole solutions with scalar hair and dilaton field and toroidal horizons and interior solution

Younesizadeh

2022

Can. J. Phys.

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In this paper we investigate the black hole solutions with toroidal horizons in scalar hair/dilaton gravity. First, we obtain the field equations in n-dimensions, then we propose some different models(Ansatz) and find the exact solutions for these type of ansatzs. These solutions are not asymptotically (anti-)de Sitter or flat, except in one special case. We also show that the BTZ and BTZ-like solutions will emerge from some of these solutions as a special case. We also show that when the event horizon radius gets bigger and bigger, the temperature will be the same in various dimensions. The only difference is noticeable near the origin(this statement is clear in diagrams). For these solutions, we obtained a new version of the Smarr formula as well. Also, we show that the presence of the scalar field makes the black holes to be more stable near the origin except for the BTZ case. We can say in general that the presence of scalar field is an important factor in black hole’s stability investigations. In the critical behavior analysis we find that there is no evidence to show the existence of P-V criticality. We present here a class of interior solutions corresponding to the solution in scalar hair gravity exterior. The solution which is obtained in linear case is regular and well-behaved at the stellar interior.

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BH solutions with toroidal horizon in dilaton gravity inspired by power-law electrodynamics: PV criticality and quasinormal modes

Younesizadeh

Ahmed

Ahmad

et al. 2020

Int. J. Mod. Phys. A

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In this work, a new class of black hole solutions in dilaton gravity has been obtained where the dilaton field is coupled with nonlinear Maxwell invariant as a source. The background space–time in this works is considered as the [Formula: see text]-dimensional toroidal metric. In the presence of the dilaton field (for some unique values of [Formula: see text][Formula: see text] a ), the electric field increases as we got farther away from the origin. In the absence of the dilaton field [Formula: see text], the electric field always decreases as one goes farther away from the origin. In the thermodynamical analysis, we obtain the Smarr formula for our solution. We find that the presence of the dilaton field makes the solutions to be locally stable near the origin. Also, this field vanishes the global stability near the origin compared to the no dilaton field case [Formula: see text]. We can say that the dilaton field has a crucial impact on the thermodynamical stability and it is a key factor in stability analysis. We study the quasinormal modes (QNMs) of black hole solutions in dilaton gravity. For this purpose, we use the WKB approximation method upto first order corrections. We have shown the perturbations decay in corresponding diagrams when the dilaton parameter [Formula: see text] and coupling constant [Formula: see text] change. Motivated by the thermodynamical analogy of black holes and Van der Waals liquid/gas systems, in this work, we investigate PV criticality of the obtained solution. We extend the phase space by considering the cosmological constant as thermodynamic pressure. We obtain the equation of state (EOS) and plot the relevant PV [Formula: see text] diagrams. We also present a class of interior solutions corresponding to the exterior solution in dilaton gravity. The solution which is obtained for a linear equation of state is regular and well-behaved at the stellar interior. a Dilaton field representation.

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Charged star in (2+1)-dimensional gravity

Cited by 3 publications

References 29 publications

Black holes with toroidal horizons in ( $$d+1$$ d + 1 )-dimensional space-time

Black holes with toroidal horizons in ( $$d+1$$ d + 1 )-dimensional space-time

Higher-dimensional black hole solutions with scalar hair and dilaton field and toroidal horizons and interior solution

BH solutions with toroidal horizon in dilaton gravity inspired by power-law electrodynamics: PV criticality and quasinormal modes

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