Asymptotically flat black holes in<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mn>2</mml:mn><mml:mo mathvariant="bold">+</mml:mo><mml:mn>1</mml:mn></mml:mrow></mml:math>dimensions

Alkaç, Gökhan; Kilicarslan, Ercan; Tekin, Bayram

doi:10.1103/physrevd.93.084003

Cited by 11 publications

(7 citation statements)

References 33 publications

(41 reference statements)

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“…that admits asymptotically flat and rotating black holes [11,12]. Let us apply the above procedure to detect the event horizons of these black holes.…”

Section: Two Examples In 2+1 Dimensionsmentioning

confidence: 99%

Event horizon detecting invariants

Tavlayan

Tekin

2020

Phys. Rev. D

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Some judiciously chosen local curvature scalars can be used to invariantly characterize event horizons of black holes in D > 3 dimensions, but they fail for the three dimensional Bañados-Teitelboim-Zanelli (BTZ) black hole since all curvature invariants are constant. Here we provide an invariant characterization of the event horizon of the BTZ black hole using the curvature invariants of codimension one hypersurfaces instead of the full spacetime. Our method is also applicable to black holes in generic dimensions but is most efficient in three, four, and five dimensions. We give four dimensional Kerr, five dimensional Myers-Perry and three dimensional warped-anti-de Sitter, and the three dimensional asymptotically flat black holes as examples.PACS numbers:

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“…that admits asymptotically flat and rotating black holes [11,12]. Let us apply the above procedure to detect the event horizons of these black holes.…”

Section: Two Examples In 2+1 Dimensionsmentioning

confidence: 99%

Event horizon detecting invariants

Tavlayan

Tekin

2020

Phys. Rev. D

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“…Interestingly, b enables us to find other types of black hole solutions. For example, there is a black hole solution with radius r = µ/b even when Λ = 0 as long as b and µ are positive [18,19,20]. Black hole solutions in the general case, i.e., m 2 = λ have also been found, e.g., the Lifshitz black hole [16] and black holes in the AdS background [21,22].…”

Section: Bht Massive Gravity and Static Circularly Symmetric Black Homentioning

confidence: 99%

Null geodesics and repulsive behavior of gravity in $(2+1)$D massive gravity

Nakashi

Kobayashi

S.Ueda

et al. 2019

Progress of Theoretical and Experimental Physics

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We study the null geodesics in a static circularly symmetric (SCS) black hole spacetime which is a solution in the (2 + 1)-dimensional massive gravity proposed by Bergshoeff, Hohm and Townsend (BHT massive gravity). We obtain analytic solutions for the null geodesic equation in the SCS black hole background and find the explicit form of deflection angles. We see that for various values of the impact parameter, the deflection angle can be positive, negative or even zero in this black hole spacetime. The negative deflection angle indicates the repulsive behavior of the gravity which comes from the gravitational hair parameter that is the most characteristic quantity of the BHT massive gravity.

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“…Since the seminal discovery of the BTZ solution [1,2], the catalog of three-dimensional black holes has grown in different directions. On the one hand, higher-curvature modifications of Einstein's theory such as New Massive Gravity [3] and its extensions [4][5][6] allow for new solutions which differ from the BTZ one e.g., in being locally inequivalent from AdS 3 , in possessing asymptotically flat, dS 3 or Lifshitz asymptotes, or in including curvature (rather than conical or BTZ-like) singularities [7][8][9][10][11][12][13][14][15][16][17]. Including extra fields also allows for progress, and additional solutions are known for Einstein-Maxwell [18][19][20][21][22][23][24][25] as well as for Einstein-Maxwell-dilaton [26][27][28][29] and Maxwell-Brans-Dicke type [30,31] theories.…”

Section: Introductionmentioning

confidence: 99%

Regular black holes in three dimensions

Bueno,

Cano,

Moreno

et al. 2021

Preprint

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We find a plethora of new analytic black holes and globally regular horizonless spacetimes in three dimensions. The solutions involve a single real scalar field φ which always admits a magnetic-like expression proportional to the angular coordinate. The new metrics, which satisfy gttgrr = −1 and represent continuous generalizations of the BTZ one, solve the equations of Einstein gravity corrected by a new family of densities (controlled by unconstrained couplings) constructed from positive powers of (∂φ) 2 and certain linear combinations of R ab ∂aφ∂ b φ and (∂φ) 2 R. Some of the solutions obtained describe black holes with one or several horizons. A set of them possesses curvature singularities, while others have conical or BTZ-like ones. Interestingly, in some cases the black holes have no singularity at all, being completely regular. Some of the latter are achieved without any kind of fine tuning or constraint between the action parameters and/or the physical charges of the solution. An additional class of solutions describes globally regular and horizonless geometries.

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Asymptotically flat black holes in2+1dimensions

Cited by 11 publications

References 33 publications

Event horizon detecting invariants

Event horizon detecting invariants

Null geodesics and repulsive behavior of gravity in $(2+1)$D massive gravity

Regular black holes in three dimensions

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