Dynamical Lorentz symmetry breaking in a tensor bumblebee model

Assunção, J. F.; Mariz, T.; Nascimento, J. R.; Petrov, A. Yu.

doi:10.1103/physrevd.100.085009

Cited by 29 publications

(15 citation statements)

References 51 publications

(71 reference statements)

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“…Moreover, we find that the singularity occurs for the effective metrics (2.21)-(2.22) at α = ± 1 2 . As α = 1 2 , one can find the null geodesic condition in the effective metric (2.21) becomes 24) which implies that the dispersion relation for arbitrary photon does not depend on its fourvelocity componentsṙ andθ at the arbitrary spacetime point. Similarly, as α = − 1 2 , the dispersion relation for arbitrary photon in the effective metric (2.22) does not depend on its four-velocity componentsṫ andφ at arbitrary position.…”

Section: Jhep07(2020)054mentioning

confidence: 96%

“…is supposed to own a minimum at B µ B µ = ∓b 2 . The condition B µ B µ = ∓b 2 is satisfied when the vector field has a nonzero vacuum value [14][15][16][17][18][19][20][21][22][23][24]…”

Section: Equation Of Motion For the Photons Coupled To Bumblebee Fielmentioning

confidence: 99%

“…value of a bumblebee field B µ under a suitable potential. Recently, the bumblebee gravity model has been extensively studied in literature [16][17][18][19][20][21][22][23][24]. An exact Schwarzschild-like black hole solution in this bumblebee gravity model is obtained and some classical tests are studied [14].…”

Section: Introductionmentioning

confidence: 99%

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Polarization effects in Kerr black hole shadow due to the coupling between photon and bumblebee field

Chen

Jing

2020

J. High Energ. Phys.

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We present firstly the equation of motion for the photon coupled to a special bumblebee vector field in a Kerr black hole spacetime and find that the propagation of light depends on its polarization due to the birefringence phenomenon. The dependence of black hole shadow on the light's polarization is dominated by the rotation of black hole. In the non-rotating case, we find that the black hole shadow is independent of the polarization of light. However, the status is changed in the rotating case, in which the black hole shadow depends on the light's polarization and the coupling between bumblebee vector field and electromagnetic field. These features of black hole shadow casted by polarized lights could help us to understand the bumblebee vector field with Lorentz symmetry breaking and its interaction with electromagnetic field.

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Section: Jhep07(2020)054mentioning

confidence: 96%

Section: Equation Of Motion For the Photons Coupled To Bumblebee Fielmentioning

confidence: 99%

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Polarization effects in Kerr black hole shadow due to the coupling between photon and bumblebee field

Chen

Jing

2020

J. High Energ. Phys.

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“…There exist a class of models, which can be indicated as the related to the Einstein-aether theory. As an example of such model, we would like to consider the so-called bumblebee model (see, e.g., [27][28][29][30]). Such a model differs from the Einstein-aether theory by one term only: it is the term λ(g ik B i B k ± b 2 ) 2 introduced into the Lagrangian instead of the term λ(g ik U i U k − 1).…”

Section: Einstein-aether Theory: Historical Motives and Related Modelsmentioning

confidence: 99%

Spontaneous Color Polarization as A Modus Originis of the Dynamic Aether

Balakin

Kiselev

2020

Universe

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We suggest the phenomenological model of emergence of the dynamic aether as a result of decay of the SU(N) symmetric field configuration containing the multiplet of vector fields. The scenario of the transition to the dynamic aether, which is characterized by one unit timelike vector field that is associated with the aether velocity, is based on the idea of spontaneous color polarization analogous to the spontaneous electric polarization in ferroelectric materials. The mechanism of spontaneous color polarization is described in the framework of anisotropic cosmological model of the Bianchi-I type; it involves consideration of the idea of critical behavior of the eigenvalues of the tensor of color polarization in the course of the Universe accelerated expansion. The interim stage of transition from the color aether to the canonic dynamic aether takes the finite period of time, the duration of which is predetermined by the phenomenologically introduced critical value of the expansion scalar.

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“…In 1989, Kostelecký and Samuel [2] proposed the bumblebee gravity theory as the simplest model for studying the spontaneous Lorentz symmetry breaking (LSB), in which a bumblebee field with a vacuum expectation value leads to spontaneous breaks in Lorentz symmetry. The interest towards in bumblebee gravity theory has increased over the years [3][4][5][6][7][8][9][10][11][12][13][14][15]. In particular, some new exact solutions have been recently found.…”

Section: Introductionmentioning

confidence: 99%

Finite-Distance Gravitational Deflection of Massive Particles by the Kerr-like Black Hole in the Bumblebee Gravity Model

Li¹,

Овгун²

2019

Preprint

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In this paper, we study the weak gravitational deflection angle of relativistic massive particles by the Kerr-like black hole in the bumblebee gravity model. In particular, we focus on weak field limits and calculate the deflection angle for a receiver and source at a finite distance from the lens. To this end, we use the Gauss-Bonnet theorem of a two-dimensional surface defined by a generalized Jacobi metric. The spacetime is asymptotically non-flat due to the existence of a bumblebee vector field. Thus the deflection angle is modified and can be divided into three parts: the surface integral of the Gaussian curvature, the path integral of a geodesic curvature of the particle ray and the change in the coordinate angle. In addition, we also obtain the same results by defining the deflection angle. The effects of the Lorentz breaking constant on the gravitational lensing are analyzed. We then consider the finite-distance correction for the deflection angle of massive particles.

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Dynamical Lorentz symmetry breaking in a tensor bumblebee model

Cited by 29 publications

References 51 publications

Polarization effects in Kerr black hole shadow due to the coupling between photon and bumblebee field

Polarization effects in Kerr black hole shadow due to the coupling between photon and bumblebee field

Spontaneous Color Polarization as A Modus Originis of the Dynamic Aether

Finite-Distance Gravitational Deflection of Massive Particles by the Kerr-like Black Hole in the Bumblebee Gravity Model

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