Stability of generalized Einstein-Maxwell-scalar black holes

Gannouji, Radouane; Baez, Yolbeiker Rodríguez

doi:10.1007/jhep02(2022)020

Cited by 11 publications

(13 citation statements)

References 68 publications

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“…A similar study was performed in Ref. [82] for the Lagrangian L = G 2 (φ, X, F )+ G 4 (φ)R, but our analysis is more general in that the scalar field sector is described by the full Horndeski Lagrangian. By doing this, we can accommodate the stabilities of hairy BH solutions present in all the theories mentioned above, especially those containing the GB term.…”

Section: Introductionmentioning

confidence: 84%

“…The analysis of BH perturbations in this case was also addressed in Ref. [82], but the angular stability conditions of even-parity perturbations were missing. In the following, we will investigate all the linear stability conditions.…”

Section: A Nonminimally Coupled K-essence With a Gauge Fieldmentioning

confidence: 99%

“…(5.26) of Ref. [82] (one needs to replace G 2 → f 2 and G 4 → f 1 /2 for the notation used in [82]).…”

Section: A Nonminimally Coupled K-essence With a Gauge Fieldmentioning

confidence: 99%

“…We decompose the types of perturbations into the odd-and even-parity sectors and derive all the linear stability conditions of five dynamical perturbations. In particular we will derive the propagation speeds of even-parity perturbations along the angular direction in the limit of large multipoles l, which are missing in most of the papers about BH perturbations in the literature [50,82]. We note that, in full Horndeski theories with a perfect fluid, all the linear stability conditions including the angular propagation speeds were derived in Ref.…”

Section: Introductionmentioning

confidence: 99%

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Black hole perturbations in Maxwell-Horndeski theories

Kase¹,

Tsujikawa²

2023

Preprint

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We study the linear stability of black holes in Maxwell-Horndeski theories where a U (1) gaugeinvariant vector field is coupled to a scalar field with the Lagrangian of full Horndeski theories. The perturbations on a static and spherically symmetric background can be decomposed into oddand even-parity modes under the expansion of spherical harmonics with multipoles l. For l ≥ 2, the odd-parity sector contains two propagating degrees of freedom associated with the gravitational and vector field perturbations. In the even-parity sector, there are three dynamical perturbations arising from the scalar field besides the gravitational and vector field perturbations. For these five propagating degrees of freedom, we derive conditions for the absence of ghost/Laplacian stabilities along the radial and angular directions. We also discuss the stability of black holes for l = 0 and l = 1, in which case no additional conditions are imposed to those obtained for l ≥ 2. We apply our general results to Einstein-Maxwell-dilaton-Gauss-Bonnet theory and Einstein-Born-Infeld-dilaton gravity and show that hairy black hole solutions present in these theories can be consistent with all the linear stability conditions. In regularized four-dimensional Einstein-Gauss-Bonnet gravity with a Maxwell field, however, exact charged black hole solutions known in the literature are prone to instabilities of even-parity perturbations besides a strong coupling problem with a vanishing kinetic term of the radion mode.

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Section: Introductionmentioning

confidence: 84%

Section: A Nonminimally Coupled K-essence With a Gauge Fieldmentioning

confidence: 99%

“…(5.26) of Ref. [82] (one needs to replace G 2 → f 2 and G 4 → f 1 /2 for the notation used in [82]).…”

Section: A Nonminimally Coupled K-essence With a Gauge Fieldmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Black hole perturbations in Maxwell-Horndeski theories

Kase¹,

Tsujikawa²

2023

Preprint

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“…In contrast, a small q may drag a part of V 2 to the negative regime. By following the formalism of [92,93], we notice that being negative on V 2 (or V 1 , although we abbreviated this part of the discussion since V 1 was observed to stay positive for all the reasonable q's, e.g., those considered in Fig. 2) can introduce instabil- FIG.…”

Section: B Calculate For the Qnmsmentioning

confidence: 99%

Odd-parity perturbations of the wormhole-like geometries and quasi-normal modes in Einstein-Æther theory

Zhang¹,

Wang²,

Zhu³

2023

Preprint

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The Einstein-AEther theory has drawn a lot of attentions in recent years. As a representative case of gravitational theories that break the Lorentz symmetry, it plays an important role in testing the Lorentz-violating effects and shedding light on the attempts to construct quantum gravity. Since the first detection to the gravitational wave, the event GW150914, a brand new window has been opened to testing the theory of gravity with gravitational wave observations. At the same time, the study of gravitational waves itself also provides us a serendipity of accessing the nature of a theory. In this paper, we focus on the odd-parity gravitational perturbations to a background that describes a wormhole-like geometry under the Einstein-AEther theory. Taking advantage of this set of analytic background solutions, we are able to simplify the Lagrangian and construct a set of coupled single-parameter dependent master equations, from which we solve for the quasi-normal modes that carry the physical information of the emitted gravitational waves. Basically, the results reflect a consistency between Einstein-AEther theory and general relativity. More importantly, as long as the no-ghost condition and the latest observational constraints are concerned, we notice that the resultant quasi-normal mode solutions intimate a kind of dynamical instability. Thus, the solutions are ruled out based on their stability against small linear perturbations.

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Odd-parity perturbations in the most general scalar–vector–tensor theory

Baez

Gonzalez-Espinoza

2023

Class. Quantum Grav.

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In the context of the most general scalar-vector-tensor theory, we study the stability of static spherically symmetric black holes under linear odd-parity perturbations. We calculate the action to second order in the linear perturbations to derive a master equation for these perturbations. For this general class of models, we obtain the conditions of no-ghost and Laplacian instability. Then, we study in detail the generalized Regge-Wheeler potential of particular cases to find their stability conditions.

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Stability of generalized Einstein-Maxwell-scalar black holes

Cited by 11 publications

References 68 publications

Black hole perturbations in Maxwell-Horndeski theories

Black hole perturbations in Maxwell-Horndeski theories

Odd-parity perturbations of the wormhole-like geometries and quasi-normal modes in Einstein-Æther theory

Odd-parity perturbations in the most general scalar–vector–tensor theory

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