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An exact stationary axisymmetric vacuum solution within a metric--affine bumblebee gravity

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arxiv 2402.13014 v2 pith:B2PRORBT submitted 2024-02-20 gr-qc

A. A. Araújo Filho , J. R. Nascimento , A. Yu. Petrov , P. J. Porfírio This is my paper · ORCID
classification gr-qc
keywords solutionaxisymmetricbreakingbumblebeelorentzmetric--affinesymmetryvacuum
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abstract

Within the framework of the spontaneous Lorentz symmetry breaking, we consider a metric--affine generalization of the gravitational sector of the Standard--Model Extension (SME), including the Lorentz--violating (LV) coefficients $u$ and $s^{\mu\nu}$. In this model, we derive the modified Einstein field equations in order to obtain a new axisymmetric vacuum spinning solution for a particular bumblebee's profile. Such a solution has the remarkable property of incorporating the effects of Lorentz symmetry breaking (LSB) through the LV dimensionless parameter $X=\xi b^2$, as the LSB is turned off, $X=0$, we recover the well--established result, the Kerr solution, as expected. Afterwards, we calculate the geodesics, the radial acceleration and thermodynamic quantities for this new metric. We also estimate an upper bound for $X$ by using astrophysical data of the advance Mercury's perihelion.

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Forward citations

Cited by 5 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Signatures of Lorentz violation in bright ring for Sgr A* images by radiation ineffective accretion flows

    astro-ph.HE 2026-08 conditional novelty 6.0 of 10

    For a rotating Lorentz-violating black hole, increasing the LV parameter shrinks and broadens Sgr A*'s image ring, and EHT data bound the parameter over a spin-dependent range.

  2. Lorentz violating quadratic gravity

    hep-th 2026-03 reject novelty 6.0 of 10

    Bumblebee–quadratic gravity needs new Lorentz-violating counterterms at one loop, but the displayed computation has a gauge-parameter inconsistency and the classical Schwarzschild/de Sitter solutions are the robust part.

  3. Nonrelativistic effective potential of the bumblebee model

    hep-th 2025-12 conditional novelty 5.0 of 10

    The leading-order nonrelativistic potential in the bumblebee model is a Coulomb potential with charge rescaled by (1 - (mβξ/2)^2), producing a hydrogen level shift of order m^3β^2ξ^2.

  4. Exact Black Hole Solutions in Bumblebee Gravity with Lightlike or Spacelike VEVS

    gr-qc 2025-10 conditional novelty 5.0 of 10

    New exact Schwarzschild-like, (A)dS-like, and charged black holes in bumblebee gravity with a two-component vector VEV keep Lorentz-violating corrections even when the VEV is lightlike, with Wald and first-law entropi...

  5. Quasinormal Modes and Dynamical Evolution of Scalar Fields in the Einstein-Bumblebee Theory with a Cosmological Constant

    gr-qc 2025-02 conditional novelty 4.0 of 10

    For scalar perturbations of Einstein-Bumblebee black holes in de Sitter spacetime, increasing the Lorentz-violation parameter or the cosmological constant generally lowers the quasinormal mode frequency and damping rate.

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