A general static and spherically symmetric black hole in traceless metric-affine bumblebee gravity

@misc{filho2026general,
  title = {{A general static and spherically symmetric black hole in traceless metric-affine bumblebee gravity}},
  author = {A. A. Araújo Filho and N. Heidari and V. B. Bezerra and Francisco S. N. Lobo},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.29675},
  eprint = {2609.29675},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.29675},
}

TY  - UNPB
TI  - A general static and spherically symmetric black hole in traceless metric-affine bumblebee gravity
AU  - A. A. Araújo Filho
AU  - N. Heidari
AU  - V. B. Bezerra
AU  - Francisco S. N. Lobo
PY  - 2026
DA  - 2026/09/01
PB  - arXiv
DO  - 10.48550/arxiv.2609.29675
UR  - https://arxiv.org/abs/2609.29675
AB  - We construct and analyze a general exact static and spherically symmetric black hole solution in traceless metric-affine bumblebee gravity by considering a vacuum expectation value with temporal and radial components. The temporal component remains constant and the auxiliary geometry is Ricci flat, while Lorentz symmetry breaking is transferred to the physical metric through the metric-affine deformation. After introducing the areal radius and normalizing the Killing time at spatial infinity, the geometry is controlled by a single invariant deformation parameter. The resulting spacetime is asymptotically conical, possesses a regular Killing horizon, and retains the causal structure of the Schwarzschild black hole, with a curvature singularity located at the origin. Initially, we examine its thermodynamic properties, gravitational Doppler effect, and tidal forces. Lorentz symmetry breaking modifies the Hawking temperature and the magnitude of the tidal field, although the characteristic ratio between radial stretching and transverse compression is preserved. The thermodynamic-topology analysis reveals no critical point within the admissible black hole sector. Furthermore, massless scalar perturbations are also investigated through WKB and characteristic time domain solution, showing decaying profiles throughout the sampled parameter range and deformation-dependent quasinormal frequencies. Finally, light deflection and perihelion advance are used to establish stringent Solar System bounds on the invariant deformation, which, at leading order, depends on a combination of the temporal and norm sectors of the bumblebee field.
ER  -