Finite action for three dimensional gravity with a minimally coupled scalar field

Gegenberg, J.; Martínez, Cristián; Troncoso, Ricardo

doi:10.1103/physrevd.67.084007

Cited by 53 publications

(55 citation statements)

References 39 publications

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“…The counterterms needed to render the action finite explicitly depend on the scalar field. This was also shown for the D = 3 case of [3] in the article [14].…”

Section: Discussionmentioning

confidence: 74%

Asymptotically anti–de Sitter spacetimes and scalar fields with a logarithmic branch

et al. 2004

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Abstract:We consider a self-interacting scalar field whose mass saturates the BreitenlohnerFreedman bound, minimally coupled to Einstein gravity with a negative cosmological constant in D ≥ 3 dimensions. It is shown that the asymptotic behavior of the metric has a slower fall-off than that of pure gravity with a localized distribution of matter, due to the backreaction of the scalar field, which has a logarithmic branch decreasing as r −(D−1)/2 ln r for large radius r. We find the asymptotic conditions on the fields which are invariant under the same symmetry group as pure gravity with negative cosmological constant (conformal group in D − 1 dimensions). The generators of the asymptotic symmetries are finite even when the logarithmic branch is considered but acquire, however, a contribution from the scalar field. *

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“…The counterterms needed to render the action finite explicitly depend on the scalar field. This was also shown for the D = 3 case of [3] in the article [14].…”

Section: Discussionmentioning

confidence: 74%

Asymptotically anti–de Sitter spacetimes and scalar fields with a logarithmic branch

et al. 2004

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“…These two effects have been observed in similar setups and for various dimensions in Refs. [5,10,27,28,32]. Indeed, the scalar field would not contribute to the conserved charges if it falls off as φ ∼ r −3/2+ε , whereas here the asymptotic behavior of the scalar field (2.7) is…”

Section: Summary and Discussionmentioning

confidence: 99%

“…This is a generic effect observed for scalar fields with a self-interacting potential unbounded form below in asymptotically AdS spacetimes [5,27,28,10]. The variation of the boundary term at the horizon, is obtained using…”

Section: Thermodynamicsmentioning

confidence: 99%

Exact black hole solution with a minimally coupled scalar field

2004

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An exact four-dimensional black hole solution of gravity with a minimally coupled self-interacting scalar field is reported. The event horizon is a surface of negative constant curvature enclosing the curvature singularity at the origin, and the scalar field is regular everywhere outside the origin. This solution is an asymptotically locally AdS spacetime. The strong energy condition is satisfied on and outside the event horizon. The thermodynamical analysis shows the existence of a critical temperature, below which a black hole in vacuum undergoes a spontaneous dressing up with a nontrivial scalar field in a process reminiscent of

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“…(22) of Ref. [15] (see also [5] and [24]) the mass M and the angular momentum J of the hairy black hole described by Eqs. (4)-(9) are found to be…”

Section: Mass Angular Momentum and Thermodynamicsmentioning

confidence: 99%

Rotating hairy black hole and its microscopic entropy in three spacetime dimensions

2013

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We present a spinning hairy black hole in gravity minimally coupled to a self-interacting real scalar field in three spacetime dimensions. The black hole is characterized by having a single horizon which encloses a curvature singularity and the scalar field is regular everywhere. The mass and angular momentum are shown to be finite. The presence of a scalar field with a slower fall-off at infinity leads an anti-de Sitter asymptotic behavior which differs from the one found by Brown and Henneaux, but has the same symmetry group as in pure gravity. A scalar soliton, which is a finite mass regular solution devoid of integration constants, plays the role of the ground state. The existence of this soliton is the key to derive the semiclassical entropy of the rotating hairy black hole using the counting of microscopic states provided by the Cardy formula.

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Finite action for three dimensional gravity with a minimally coupled scalar field

Cited by 53 publications

References 39 publications

Asymptotically anti–de Sitter spacetimes and scalar fields with a logarithmic branch

Asymptotically anti–de Sitter spacetimes and scalar fields with a logarithmic branch

Exact black hole solution with a minimally coupled scalar field

Rotating hairy black hole and its microscopic entropy in three spacetime dimensions

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