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Quantum Kerr-de Sitter black holes in three dimensions

Panella, Emanuele, Svesko, Andrew·2023·Journal of High Energy Physics

Abstract

A bstract: We use braneworld holography to construct a three-dimensional quantum-corrected Kerr-de Sitter black hole, exactly accounting for semi-classical backreaction effects due to a holographic conformal field theory. By contrast, classically there are no de Sitter black holes in three-dimensions, only geometries with a single cosmological horizon. The quantum Kerr black hole shares many qualitative features with the classical four-dimensional Kerr-de Sitter solution. Of note, backreaction induces inner and outer black hole horizons which hide a ring singularity. Moreover, the quantum-corrected geometry has extremal, Nariai, and ultracold limits, which appear as fibered products of a circle and two-dimensional anti-de Sitter, de Sitter, and Minkowski space, respectively. The thermodynamics of the classical bulk black hole, described by the rotating four-dimensional anti-de Sitter C-metric, has an interpretation on the brane as thermodynamics of the quantum black hole, obeying a semi-classical first law where the Bekenstein-Hawking area entropy is replaced by the generalized entropy. For purposes of comparison, we derive the renormalized quantum stress-tensor due to a free conformally coupled scalar field in the classical Kerr-de Sitter conical geometry and perturbatively solve for its backreaction.

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  • The rotating and charged holographic quantum black holes do not match the non-holographic perturbatively-corrected counterparts.

    “The rotating and charged holographic quantum black holes, meanwhile, do not match to the non-holographic perturbatively-corrected counterparts (cf.[27,40,45]).”

    From Three-Dimensional Quantum Black Holes: A Primer (2024) · cites this paper as [27]

  • Starting from the rotating C-metric (4.40) with κ = +1 and replacing a → -a, and imposing bulk regularity, the metric on the brane in canonically normalized coordinates is (4.114).

    “Starting from the rotating C-metric (4.40) with κ = +1 and replacing a → -a, and imposing bulk regularity, the metric on the brane in canonically normalized coordinates is [27] foot_14”

    From Three-Dimensional Quantum Black Holes: A Primer (2024) · cites this paper as [27]

  • The radial dependence of the renormalized stress-tensor due to a conformally coupled scalar field is significantly more complicated than the holographic stress-tensor.

    “Further, as in the qBTZ case, the radial dependence of the renormalized stress-tensor due to a conformally coupled scalar field (found perturbatively in [27]) is significantly more complicated than the holographic stress-tensor.”

    From Three-Dimensional Quantum Black Holes: A Primer (2024) · cites this paper as [27]

  • Substituting the geometry (4.114) into the gravity field equations results in a holographic stress-tensor with components of essentially the same form as (4.64).

    “Substituting the geometry (4.114) into the gravity field equations results in a holographic stress-tensor with components of essentially the same form as (4.64) -see [27] for explicit details.”

    From Three-Dimensional Quantum Black Holes: A Primer (2024) · cites this paper as [27]

  • In the near-horizon regime, the limiting geometries appear as fibered products of a circle and two-dimensional anti-de Sitter, de Sitter, and Minkowski space, respectively.

    “In the near-horizon regime, the geometries appear as fibered products of a circle and two-dimensional anti-de Sitter, de Sitter, and Minkowski space, respectively.”

    From Three-Dimensional Quantum Black Holes: A Primer (2024) · cites this paper as [27]

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Authors
Panella, E., & Svesko, A.
Venue
Journal of High Energy Physics
Published
2023-06-21
Volume
2023
Issue
6
ISSN
1029-8479
Cited by
33
References
1
Language
en

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