Regular black holes in three dimensions

Bueno, Pablo; Cano, Pablo A.; Moreno, Javier; van der Velde, Guido

doi:10.48550/arxiv.2104.10172

Cited by 7 publications

(14 citation statements)

References 68 publications

(77 reference statements)

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“…Now, given that for α = 0 the enegy-momentum tensor θ µν induce a deformation in the metric, it is said that ( 17)-( 19) represent the equations of the decoupling sector. Furthermore, it is noticeable that (22) means that a decoupling without energy-momentum exchange can be reached either by imposing g = 0 or p + ρ = 0. The former requirement corresponds to the standard MGD where only g −1 rr undergoes a geometrical deformation.…”

Section: Gravitational Decoupling In 2 + 1 Dimensional Space-time Wit...mentioning

confidence: 99%

“…In the previous section we obtained that the decoupling sector is a system of three equations for five unknowns variables, { f , g, ρ θ , p θ r , p θ ⊥ }. Of course, this number decreases to four unknowns when the minimal geometric deformation is implemented, namely, when g → 0 which, besides from (22), implies…”

Section: + 1 Einstein-klein-gordon System: the Minimal Casementioning

confidence: 99%

“…In addition, black hole solutions for minimally and nonminimally coupled scalar fields have been constructed [18][19][20][21]. Very recently, a plethora of new analytic black holes and globally regular three-dimensional horizonless spacetimes have been reported [22]. Specifically, there have been several interesting advances in theories considering stationary rotating scalar field solutions in 2 + 1 dimensions, using Schwarzschild coordinates frame, for a static cyclic symmetric metric coupled minimally to a dilation in the presence of an exponential potential.…”

Section: Introductionmentioning

confidence: 99%

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2+1 Einstein–Klein–Gordon Black Holes by Gravitational Decoupling

et al. 2022

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In this work we study the 2+1-Einstein–Klein–Gordon system in the framework of Gravitational Decoupling. We associate the generic matter decoupling sector with a real scalar field so we can obtain a constraint which allows us to close the system of differential equations. The constraint corresponds to a differential equation involving the decoupling functions and the metric of the seed sector and will be independent of the scalar field itself. We show that when the equation admits analytical solutions, the scalar field and the self-interacting potential can be obtained straightforwardly. We found that, in the cases under consideration, it is possible to express the potential as an explicit function of the scalar field only for certain particular cases corresponding to limiting values of the parameters involved.

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Section: Gravitational Decoupling In 2 + 1 Dimensional Space-time Wit...mentioning

confidence: 99%

Section: + 1 Einstein-klein-gordon System: the Minimal Casementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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2+1 Einstein–Klein–Gordon Black Holes by Gravitational Decoupling

et al. 2022

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“…The BTZ BH solution has been studied by different fulfillments, from different physical viewpoints. For example, the construction of geodesic equations of the uncharged BTZ BHs [12], the quasi-normal modes [13][14][15][16], the scattering process of test particles [17,18], the hydrostatic equilibrium conditions for finite distributions [19], and solutions for fluid distributions matching the exterior BTZ spacetime [20][21][22][23][24]. Moreover, by taking into account a non-constant coupling parameter with the energy-scale, the scale-dependent version of the BTZ solution has been derived and analyzed [25][26][27][28][29].…”

Section: Introductionmentioning

confidence: 99%

New black hole solutions in three-dimensional $\mathit{f(R)}$ gravity

Nashed

Sheykhi

2021

Preprint

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We construct two new classes of analytical solutions in three-dimensional spacetime and in the framework of f (R) gravity. The first class represents a non-rotating black hole (BH) while the second class corresponds to a rotating BH solution. The Ricci scalar of these BH solutions have non-trivial values and are described by the gravitational mass M , two angular momentums J and J1, and an effective cosmological constant Λ ef f . Moreover, these solutions do not restore the 3-dimensional Bañados-Teitelboim-Zanelli (BTZ) solutions of general relativity (GR) which implies the novelty of the obtained BHs in f (R) gravity. Depending on the range of the parameters, these solutions admit rotating/non-rotating asymptotically AdS/dS BH interpretation in spite that the field equation of f (R) has no cosmological constant. Interestingly enough, we observe that in contrast to BTZ solution which has only causal singularity and scalar invariants are constant everywhere, the scalar invariants of these solutions indicate strong singularity for the spacetime. Furthermore, we construct the forms of the f (R) function showing that they behave as polynomial functions. Finally, we show that the obtained solutions are stable from the viewpoint that heat capacity has a positive value, and also from the condition of Ostrogradski which state that the second derivative of f (R) should have a positive value.

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“…These theories should not to be confused with the recently proposed models of Electromagnetic Quasitopological Gravities[38,39].…”

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confidence: 99%

Quasitopological electromagnetism: Reissner-Nordström black strings in Einstein and Lovelock gravities

Cisterna,

Henríquez-Báez,

Mora

et al. 2021

Preprint

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In this work, we provide consistent compactifications of Einstein-Maxwell and Einstein-Maxwell-Lovelock theories on direct product spacetimes of the form M D = M d × K p , where K p is a Euclidean internal manifold of constant curvature. For these compactifications to take place, it is required the distribution of a precise flux of p-forms over the internal manifold. The dynamic of the p-forms are demanded to be controlled by two types of interaction. First, by specific couplings with the curvature tensor and, second, by a suitable interaction with the electromagnetic field of the d-dimensional brane, the latter being dictated by a modification of the recently proposed theory of Quasitopological Electromagnetism. The field equations of the corresponding compactified theories, which are of second order, are solved and general homogenous charged black p-branes are constructed. We explicitly provide homogenous Reissner-Nordström black strings and black p-branes in Einstein-Maxwell theory and homogenous charged Boulware-Deser black p-branes for quadratic and cubic Maxwell-Lovelock gravities.

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Regular black holes in three dimensions

Cited by 7 publications

References 68 publications

2+1 Einstein–Klein–Gordon Black Holes by Gravitational Decoupling

2+1 Einstein–Klein–Gordon Black Holes by Gravitational Decoupling

New black hole solutions in three-dimensional $\mathit{f(R)}$ gravity

Quasitopological electromagnetism: Reissner-Nordström black strings in Einstein and Lovelock gravities

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