Full classification of static spherical vacuum solutions in bumblebee gravity with general VEVs reveals degeneracies at ξ=κ/2 and permits exact Schwarzschild solutions with non-zero matter.
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An exact Schwarzschild-like solution in a bumblebee gravity model
11 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
We have obtained an exact vacuum solution from a gravity sector contained in the minimal standard-model extension. The theoretical model assumes a Riemann spacetime coupled to the bumblebee field which is responsible for the spontaneous Lorentz symmetry breaking. The solution achieved in a static and spherically symmetric scenario establishes a Schwarzschild-like black hole. In order to study the effects of the spontaneous Lorentz symmetry breaking, we have investigated some classics tests including the advance of the perihelion, bending of light and Shapiro's time-delay. Furthermore, we have computed some upper-bounds from which the most stringent one attains a sensitivity at the $10^{-13}$ level.
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representative citing papers
Bumblebee gravity perturbations decouple exactly into gravitational and vector sectors, with gravitational modes dynamically immune to Lorentz violation and odd-even parities strictly isospectral.
Black hole entropy in diffeomorphism-invariant nonminimal gravity decomposes as S_H = S_W + S_1 + ΔS, with the extra terms required for bumblebee and Weyl-vector Gauss-Bonnet solutions but not for regular Kalb-Ramond branches.
A complex bumblebee model is formulated with gauge and longitudinal couplings; one-loop RG functions are derived and the leading-log effective potential indicates possible dynamical Lorentz violation.
Ten new exact vacuum solutions, including black holes with zero entropy, arise in extended bumblebee gravity because varying the action and imposing the vector VEV constraint do not commute.
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 coupled to NLED yields charged black hole solutions that become regular and horizonless when mass and charge are tuned to specific functions of the couplings.
In a Kerr-Sen-like spacetime from Bumblebee gravity, increasing the Lorentz symmetry breaking rate and Bumblebee charge enlarges the allowed region for energy extraction via magnetic reconnection and moves it closer to the horizon, with peak efficiency when cosmic censorship is marginally violated.
Rotating black holes with a nonminimally coupled Lorentz-violating background act as optical diodes by producing direction-dependent shadows that morph from quasi-symmetric to teardrop upon path reversal.
Partial-wave calculations of scattering cross sections, absorption, and greybody factors for spin-0 particles on charged black holes in bumblebee and Kalb-Ramond Lorentz-violating models.
EMRI waveforms in bumblebee gravity allow LISA to constrain the Lorentz symmetry breaking parameter ell at the level of O(10^{-4}).
citing papers explorer
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Full Classification of Static Spherical Vacuum Solutions to Bumblebee Gravity with General VEVs
Full classification of static spherical vacuum solutions in bumblebee gravity with general VEVs reveals degeneracies at ξ=κ/2 and permits exact Schwarzschild solutions with non-zero matter.
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Gravitational-Bumblebee perturbations: Exact decoupling and isospectrality
Bumblebee gravity perturbations decouple exactly into gravitational and vector sectors, with gravitational modes dynamically immune to Lorentz violation and odd-even parities strictly isospectral.
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Black Hole Entropy Beyond the Wald Term in Nonminimally Coupled Gravity: A Covariant Phase Space Decomposition
Black hole entropy in diffeomorphism-invariant nonminimal gravity decomposes as S_H = S_W + S_1 + ΔS, with the extra terms required for bumblebee and Weyl-vector Gauss-Bonnet solutions but not for regular Kalb-Ramond branches.
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Complex bumblebee model
A complex bumblebee model is formulated with gauge and longitudinal couplings; one-loop RG functions are derived and the leading-log effective potential indicates possible dynamical Lorentz violation.
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New Exact Vacuum Solutions in Extended Bumblebee Gravity
Ten new exact vacuum solutions, including black holes with zero entropy, arise in extended bumblebee gravity because varying the action and imposing the vector VEV constraint do not commute.
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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}.
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When Bumblebee Meets NLED: Lorentz-Violating Black Holes and Regular Spacetimes
Bumblebee gravity coupled to NLED yields charged black hole solutions that become regular and horizonless when mass and charge are tuned to specific functions of the couplings.
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Energy extraction from a rotating black hole via magnetic reconnection: Bumblebee gravity
In a Kerr-Sen-like spacetime from Bumblebee gravity, increasing the Lorentz symmetry breaking rate and Bumblebee charge enlarges the allowed region for energy extraction via magnetic reconnection and moves it closer to the horizon, with peak efficiency when cosmic censorship is marginally violated.
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Macroscopic Optical Nonreciprocity: A Black Hole as an Optical Diode
Rotating black holes with a nonminimally coupled Lorentz-violating background act as optical diodes by producing direction-dependent shadows that morph from quasi-symmetric to teardrop upon path reversal.
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Scattering, absorption and greybody factor of scalar particles by Lorentz-violating charged black holes
Partial-wave calculations of scattering cross sections, absorption, and greybody factors for spin-0 particles on charged black holes in bumblebee and Kalb-Ramond Lorentz-violating models.
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Constraining Lorentz symmetry breaking in bumblebee gravity with extreme mass-ratio inspirals
EMRI waveforms in bumblebee gravity allow LISA to constrain the Lorentz symmetry breaking parameter ell at the level of O(10^{-4}).