Exact solutions for asymptotically flat black holes in bumblebee gravity with temporal bumblebee field, analytic Y charge and X potential, and discovery of new cases including unbounded charge-mass ratio and wormhole configurations.
New Exact Vacuum Solutions in Extended Bumblebee Gravity
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
abstract
We investigate the static spherically symmetric vacuum solutions in a generalized bumblebee gravity model characterized by non-minimal couplings $B^2 R$ and $B^\mu B^\nu R_{\mu\nu}$. We demonstrate that the variation of the action and the imposition of the vacuum expectation value constraint are non-commutative, leading to a richer solution space than previously explored. A diverse set of solutions, including naked singularities, black holes, and wormholes, is obtained, and as many as ten exact solutions are presented. The thermodynamic properties of the new black hole solutions are also analyzed, and a subset of these solutions is found to have zero entropy. We argue that if such a non-minimally coupled vector-tensor gravity provides a fundamental description of the universe, it is best described by a Bumblebee-type theory, where the vector field acquires a VEV.
fields
gr-qc 3years
2026 3verdicts
UNVERDICTED 3representative citing papers
Bumblebee gravity is self-consistent in PPN up to 1.5PN order only for λ = −ξ/2, producing non-zero α1, α2, a logarithmic U_B potential, and a pulsar-timing bound |ℓ| ≲ 1.6×10^{-9}.
Bumblebee gravity parameters ℓ and Q shrink central dark regions, enhance brightness asymmetry, and alter polarization patterns in thick-disk images of Kerr-Sen-like black holes.
citing papers explorer
-
Asymptotically-flat Black holes in Bumblebee gravity: Exact solutions and Thermodynamics
Exact solutions for asymptotically flat black holes in bumblebee gravity with temporal bumblebee field, analytic Y charge and X potential, and discovery of new cases including unbounded charge-mass ratio and wormhole configurations.
-
Dynamic Aspects of Bumblebee Gravity: Post-Newtonian Approach
Bumblebee gravity is self-consistent in PPN up to 1.5PN order only for λ = −ξ/2, producing non-zero α1, α2, a logarithmic U_B potential, and a pulsar-timing bound |ℓ| ≲ 1.6×10^{-9}.
-
Imprints of Black Hole Shadows and Polarization Patterns of Various Thick Disks: Bumblebee gravity
Bumblebee gravity parameters ℓ and Q shrink central dark regions, enhance brightness asymmetry, and alter polarization patterns in thick-disk images of Kerr-Sen-like black holes.