Rotating black holes in three-dimensional Hořava gravity

Sotiriou, Thomas P.; Vega, Ian; Vernieri, Daniele

doi:10.1103/physrevd.90.044046

Cited by 65 publications

(109 citation statements)

References 29 publications

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“…Before discussing the case of spinning BHs, it is of interest to review the construction and basic properties of the static, spherically symmetric BHs, the SZ solutions [20,21]. As we shall see, they contain valuable information, and share some key properties with their rotating counterparts, being easier to study since they are found by solving a set of ordinary differential equations.…”

Section: Spherically Symmetric Black Holesmentioning

confidence: 99%

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Spinning black holes in shift-symmetric Horndeski theory

Delgado

Herdeiro

Radu

2020

J. High Energ. Phys.

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We construct spinning black holes (BHs) in shift-symmetric Horndeski theory. This is an Einstein-scalar-Gauss-Bonnet model wherein the (real) scalar field couples linearly to the Gauss-Bonnet curvature squared combination. The BH solutions constructed are stationary, axially symmetric and asymptotically flat. They possess a non-trivial scalar field outside their regular event horizon; thus they have scalar hair. The scalar "charge" is not, however, an independent macroscopic degree of freedom. It is proportional to the Hawking temperature, as in the static limit, wherein the BHs reduce to the spherical solutions found by Sotirou and Zhou. The spinning BHs herein are found by solving non-perturbatively the field equations, numerically. We present an overview of the parameter space of the solutions together with a study of their basic geometric and phenomenological properties. These solutions are compared with the spinning BHs in the Einstein-dilaton-Gauss-Bonnet model and the Kerr BH of vacuum General Relativity. As for the former, and in contrast with the latter, there is a minimal BH size and small violations of the Kerr bound. Phenomenological differences with respect to either the former or the latter, however, are small for illustrative observables, being of the order of a few percent, at most.

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Section: Spherically Symmetric Black Holesmentioning

confidence: 99%

“…This invariance results from the fact that in four spacetime dimensions the GB term alone is a total divergence. BHs in the model (1.2) with (1.6) have been first discussed by Sotiriou and Zhou (SZ) [20,21]. This model falls within the Horndeski class [22], for which a no-scalar-hair theorem had been established [23].…”

Section: Introductionmentioning

confidence: 99%

Spinning black holes in shift-symmetric Horndeski theory

Delgado

Herdeiro

Radu

2020

J. High Energ. Phys.

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“…For additional studies of these solutions, see [24][25][26][27]. In this case one adds a negative cosmological constant Λ to the action above…”

Section: Asymptotically Lifshitz Solutionsmentioning

confidence: 99%

Horava-Lifshitz black hole hydrodynamics

Eling

2014

J. High Energ. Phys.

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Abstract:We consider the holographic hydrodynamics of black holes in generally covariant gravity theories with a preferred time foliation. Gravitational perturbations in these theories have spin two and spin zero helicity modes with generically different speeds. The black hole solutions possess a spacelike causal boundary called the universal horizon. We relate the flux of the spin zero perturbation across the universal horizon to the new dissipative transport in Lifshitz field theory hydrodynamics found in arXiv:1304.7481. We construct in detail the hydrodynamics of one such black hole solution, and calculate the ratio of the shear viscosity to the entropy density.

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“…Extending GR via the addition of a scalar field and gravitational terms has also been the core of the Horndeski [31] and Galileon [32] theories. In the context of these theories, the no-hair theorems were re-formulated [33,34] but were again evaded, and additional black-hole solutions were constructed [35][36][37][38].…”

Section: Introductionmentioning

confidence: 99%

“…Setting this coupling function to be of an exponential form leads to the dilatonic theory, in the context of which the dilatonic black holes [13], the first counter-example of the scalar no-hair theorem [30], were found. For a linear coupling function, the shift-symmetric Galileon black holes [37] were also derived. These solutions have the characteristic feature of scalar hair: a regular, non-trivial scalar field which is associated with the black hole, a feature forbidden by GR.…”

Section: Introductionmentioning

confidence: 99%

Large and ultracompact Gauss-Bonnet black holes with a self-interacting scalar field

2020

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We consider the Einstein-scalar-Gauss-Bonnet theory, and study the case where a negative cosmological constant is replaced by a more realistic, negative scalar-field potential. We study different forms of the coupling function between the scalar field and the Gauss-Bonnet term as well as of the scalar potential. In all cases, we obtain asymptotically-flat, regular black-hole solutions with a non-trivial scalar field which naturally dies out at large distances. For a quadratic negative potential, two distinct subgroups of solutions emerge: the first comprises light black holes with a large horizon radius, and the second includes massive, ultra-compact black holes. The most ultra-compact solutions, having approximately the 1/20 of the horizon radius of the Schwarzschild solution with the same mass, emerge for the exponential and linear coupling functions. For other polynomial forms of the scalar potential, the subgroup of ultra-compact solutions disappears, and the black holes obtained may have a horizon radius larger or smaller than the Schwarzschild solution depending on the particular value of their mass.

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Rotating black holes in three-dimensional Hořava gravity

Cited by 65 publications

References 29 publications

Spinning black holes in shift-symmetric Horndeski theory

Spinning black holes in shift-symmetric Horndeski theory

Horava-Lifshitz black hole hydrodynamics

Large and ultracompact Gauss-Bonnet black holes with a self-interacting scalar field

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