Solar system constraints on asymptotically flat IR modified Hořava gravity through light deflection

Liu, Molin; Lu, Jun-Wang; Yu, Benhai; Lu, Jianbo

doi:10.1007/s10714-010-1123-0

Cited by 16 publications

(23 citation statements)

References 110 publications

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“…For the case ω KS M 2 ≥ 1/2, the solution describes a black hole with an event horizon, while for ω KS M 2 < 1/2 it describes a naked singularity. The limits/constraints on ω KS obtained by using the observational tests do not exclude the existence of the compact objects described by KS solution [4][5][6]. For example, the Solar system test gives the limit of ω KS > 3.2 × 10 20 cm 2 and implies that the total mass of the object cannot exceed 2.6 × 10 4 M [6].…”

Section: Introductionmentioning

confidence: 97%

Gravitational lensing around Kehagias–Sfetsos compact objects surrounded by plasma

Hensh¹,

Abdujabbarov²,

Schee³

et al. 2019

Eur. Phys. J. C

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We study the optical properties of the Kehagias-Sfetsos (KS) compact objects, characterized by the "Hořava" parameter ω KS , in the presence of plasma, considering its homogeneous or powerlaw density distribution. The strong effects of both "Hořava" parameter ω KS and plasma on the shadow cast by the KS compact objects are demonstrated. Using the weak field approximation, we investigate the gravitational lensing effect. Strong dependence of the deflection angle of the light on both the "Horava" and plasma parameter is explicitly shown. The magnification of image source due to the weak gravitational lensing is given for both the homogeneous and inhomogeneous plasma. *

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Section: Introductionmentioning

confidence: 97%

Gravitational lensing around Kehagias–Sfetsos compact objects surrounded by plasma

Hensh¹,

Abdujabbarov²,

Schee³

et al. 2019

Eur. Phys. J. C

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“…tional limits on ω [17][18][19] do not exclude the existence of stellar-mass K-S naked singularities. In fact, various tests indicate values compatible with the naked singularity, not a black hole solution for the family of K-S metrics.…”

Section: Introductionmentioning

confidence: 99%

Perfect fluid tori orbiting Kehagias–Sfetsos naked singularities

et al. 2015

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We construct perfect fluid tori in the field of the Kehagias-Sfetsos (K-S) naked singularities. These are spherically symmetric vacuum solutions of the modified Hořava quantum gravity, characterized by a dimensionless parameter ωM 2 , combining the gravitational mass parameter M of the spacetime with the Hořava parameter ω, reflecting the role of the quantum corrections. In dependence on the value of ωM 2 , the K-S naked singularities demonstrate a variety of qualitatively different behavior of their circular geodesics that is fully reflected in the properties of the toroidal structures, demonstrating clear distinction to the properties of the torii in the Schwarzschild spacetimes. In all of the K-S naked singularity spacetimes the tori are located above an "antigravity" sphere where matter can stay in a stable equilibrium position, which is relevant for the stability of the orbiting fluid toroidal accretion structures. The signature of the K-S naked singularity is given by the properties of marginally stable tori orbiting with the uniform distribution of the specific angular momentum of the fluid, l = const. In the K-S naked singularity spacetimes with ωM 2 > 0.2811, doubled tori with the same l = const can exist; mass transfer between the outer torus and the inner one is possible under appropriate conditions, while only outflow to the outer space is allowed in complementary conditions. In the K-S spacetimes with ωM 2 < 0.2811, accretion from cusped perfect fluid tori is not possible due to the non-existence of unstable circular geodesics.

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“…However, if the product ωM 2 < 1 2 , there are no horizons and the curvature singularity at r = 0 becomes visible to asymptotic observers, which is called a naked singularity. The observational constraints on the value of ω presented in [12,17,18], do not exclude the existence of the KS naked singularities, hence, in light of these observational facts, it is very important to focus on the naked singularities in the KS spacetimes. It is shown in [19] that the optical signatures of the KS naked singularity is different from the signatures of the standard black holes in classical general relativity.…”

Section: Introductionmentioning

confidence: 99%

Quantum probe of Hořava-Lifshitz gravity

Gürtuğ

Mangut

2018

Journal of Mathematical Physics

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Particle probe analysis of the Kehagias -Sfetsos black hole spacetime of Hořava-Lifshitz gravity is extended to wave probe analysis within the framework of quantum mechanics. The timelike naked singularity that develops when ωM 2 < 1/2, is probed with quantum fields obeying Klein-Gordon and Chandrasekhar-Dirac equations. Quantum field probe of the naked singularity has revealed that both the spatial part of the wave and the Hamiltonian operators of Klein-Gordon and Chandrasekhar-Dirac equations are essentially self-adjoint and thus, the naked singularity in the Kehagias -Sfetsos spacetime become quantum mechanically non -singular.

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Solar system constraints on asymptotically flat IR modified Hořava gravity through light deflection

Cited by 16 publications

References 110 publications

Gravitational lensing around Kehagias–Sfetsos compact objects surrounded by plasma

Gravitational lensing around Kehagias–Sfetsos compact objects surrounded by plasma

Perfect fluid tori orbiting Kehagias–Sfetsos naked singularities

Quantum probe of Hořava-Lifshitz gravity

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