Magnetic Black Holes in the Vector-Tensor Horndeski Theory

Verbin, Y.

doi:10.48550/arxiv.2011.02515

Cited by 5 publications

(7 citation statements)

References 13 publications

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“…In Einstein-Maxwell theory with the U(1) gauge-invariant HVT term, Horndeski derived an electrically charged BH solution on the static and spherically symmetric background [37]. The readers may refer to [38][39][40] for more detailed analyses of the background BH solution and also to [41][42][43] for the cosmological application of the same theory. The coupling β affects the electric field strength and gives rise to a nontrivial BH solution different from the Reissner-Nordström (RN) geometry.…”

Section: Introductionmentioning

confidence: 99%

Linear stability of vector Horndeski black holes

Chen,

Felice,

Tsujikawa

2024

J. Cosmol. Astropart. Phys.

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Horndeski's vector-tensor (HVT) gravity is described by a Lagrangian in which the field strength fμν = ∂μAν-∂νAμ of a vector field Aμ interacts with a double dual Riemann tensor Lμναβ in the form βLμναβ Fμν Fαβ , where β is a constant. In Einstein-Maxwell-HVT theory, there are static and spherically symmetric black hole (BH) solutions with electric or magnetic charges, whose metric components are modified from those in the Reissner-Nordström geometry. The electric-magnetic duality of solutions is broken even at the background level by the nonvanishing coupling constant β. We compute a second-order action of BH perturbations containing both the odd- and even-parity modes and show that there are four dynamical perturbations arising from the gravitational and vector-field sectors. We derive all the linear stability conditions associated with the absence of ghosts and radial/angular Laplacian instabilities for both the electric and magnetic BHs. These conditions exhibit the difference between the electrically and magnetically charged cases by reflecting the breaking of electric-magnetic duality at the level of perturbations. In particular, the four angular propagation speeds in the large-multipole limit are different from each other for both the electric and magnetic BHs. This suggests the breaking of eikonal correspondence between the peak position of at least one of the potentials of dynamical perturbations and the radius of photon sphere. For the electrically and magnetically charged cases, we elucidate parameter spaces of the HVT coupling and the BH charge in which the BHs without naked singularities are linearly stable.

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Section: Introductionmentioning

confidence: 99%

Linear stability of vector Horndeski black holes

Chen,

Felice,

Tsujikawa

2024

J. Cosmol. Astropart. Phys.

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“…Unlike the case of scalar-tensor theories, however, vector-tensor theories have received much less attention in this respect. Black hole solutions in the vector-tensor model of Horndeski [12], that features gauge invariance, were examined already in [16] and generalized recently in [17]. Black hole solutions of the more general vector-tensor theories [13,14] were discussed in [18][19][20][21][22][23].…”

Section: Introductionmentioning

confidence: 99%

Horndeski-Proca stars with vector hair

et al. 2022

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We study Proca stars in a vector-tensor gravity model inspired by Horndeski's generalized Einstein-Maxwell field equations, supplemented with a mass term for the vector field. We discuss the effects of the nonminimal coupling term on the properties of the resulting Proca stars. We show that the sign of the coupling constant is crucial in determining the generic properties of these generalized Proca star solutions, as soon as the magnitude of the coupling constant is sufficiently large to allow for significant deviations from the standard Proca star case. For negative coupling constant we observe a new type of limiting behavior for the generalized Proca stars, where the spacetime splits into an interior region with matter fields and an exterior Schwarzschild region.

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“…To the best of our knowledge we here explore for the first time the existence of wormhole solutions in vectortensor theories. In contrast, black holes and neutron stars have already been addressed and investigated in various vector-tensor theories [65][66][67][68][69][70][71][72]. In particular, we here consider Einstein-vector-Gauss-Bonnet (EvGB) theories that retain the vacuum solutions of General Relativity, but allow in addition for vectorized solutions [73][74][75][76][77][79][80][81][82].…”

Section: Introductionmentioning

confidence: 99%

Symmetric wormholes in Einstein-vector-Gauss-Bonnet theory

Barton,

Kiefer,

Kleihaus

et al. 2022

Preprint

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We construct wormholes in Einstein-vector-Gauss-Bonnet theory where a real massless vector field is coupled to the higher curvature Gauss-Bonnet invariant. We consider three coupling functions which depend on the square of the vector field. The respective domains of existence of wormholes possess as their boundaries i) black holes, ii) solutions with a singular throat, iii) solutions with a degenerate throat and iv) solutions with cusp singularities. Depending on the coupling function wormhole solutions can feature a single throat or an equator surrounded by a double throat. The wormhole solutions need a thin shell of matter at the throat, in order to be symmetrically continued into the second asymptotically flat region. These wormhole spacetimes allow for bound and unbound particle motion as well as light rings.

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Magnetic Black Holes in the Vector-Tensor Horndeski Theory

Cited by 5 publications

References 13 publications

Linear stability of vector Horndeski black holes

Linear stability of vector Horndeski black holes

Horndeski-Proca stars with vector hair

Symmetric wormholes in Einstein-vector-Gauss-Bonnet theory

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