Charged Einstein-aether black holes and Smarr formula

Ding, Chikun; Wang, Anzhong; Wang, Xinwen

doi:10.1103/physrevd.92.084055

Cited by 74 publications

(90 citation statements)

References 58 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The boundary conditions on the metric components are such that the solution is asymptotically flat, while those for the aether components are such that lim r→+∞ u a = (1, 0, 0, 0). (2.18) As shown in [49], there exist two types of exact static and charged spherically symmetric black hole solutions in Einstein-aether theory. The first solution corresponds to the special choice of coupling constants c 14 = 0 and c 123 = 0 where c 123 ≡ c 1 + c 2 + c 3 , while the second solution corresponds to c 123 = 0.…”

Section: B Static and Charged Spherically Symmetric Einstein-aether mentioning

confidence: 99%

Shadows and deflection angle of charged and slowly rotating black holes in Einstein-Æther theory

et al. 2019

View full text Add to dashboard Cite

In this paper, we study the shadow cast by two types of charged and slowly rotating black holes in Eisntein-AEther theory of gravity. This two types of black holes are corresponding to two specific combinations of the coupling constants of the aether field, i.e., c14 = 0 but c123 = 0 for the first type and c123 = 0 for the second type, respectively. For both types of black holes, in addition to the mass and charge of the black holes, we show that the presence of the aether field can also affect the size of the shadow. For the first type black hole, it is shown that the shadow size increases with the parameter c13, while for the second type black hole, the shadow size still increases with c13 but decreases with the parameter c14. With these properties of these aether parameters, we also discuss the observational constraints on these parameters by using the data of the first black hole image by the Event Horizon Telescope. In addition, we also explore the effect of the aether field on the the deflection angle of light and the time delay by using the Gauss-Bonnet theorem. It is shown that, for a specific combination c123 = 0, the deflection angle/time delay is slightly affected by the aether parameter c13 at the leading order. *

show abstract

Section: B Static and Charged Spherically Symmetric Einstein-aether mentioning

confidence: 99%

Shadows and deflection angle of charged and slowly rotating black holes in Einstein-Æther theory

et al. 2019

View full text Add to dashboard Cite

show abstract

“…However, this seems true only for neutral case. When the black hole is charged, such a law is still absent [28]. In addition, using the Hamilton-Jacobi method, quantum tunneling of non-relativistic particles with a general non-linear dispersion relation was studied [29], and it was found that different species of particles in general experience different temperatures, 9) where κ U H is the surface gravity calculated from Eq.…”

Section: Introductionmentioning

confidence: 99%

No static black hole hairs in gravitational theories with broken Lorentz invariance

et al. 2017

Self Cite

View full text Add to dashboard Cite

In this paper, we revisit the issue of static hairs of black holes in gravitational theories with broken Lorentz invariance in the case that the speed c φ of the khronon field becomes infinitely large, c φ = ∞, for which the sound horizon of the khronon field coincides with the universal horizon, and the boundary conditions at the sound horizon reduce to those given normally at the universal horizons. As a result, less boundary conditions are present in this extreme case in comparison with the case c φ = finite. Then, it would be expected that static hairs might exist. However, we show analytically that even in this case static hairs still cannot exist, based on a decoupling limit analysis. We also consider the cases in which c φ is finite but with c φ 1, and obtain the same conclusion.

show abstract

“…In this section we can calculate the surface gravity at the universal horizon of a charged Einstein-aether black hole [39]. The static spherically symmetric spacetime in Einstein-Maxwell-aether theory takes the Eddington-Finklestein coordinates form (2.3).…”

Section: Surface Gravity Of a Charged Einstein-aether Black Holementioning

confidence: 99%