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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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}.
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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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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}.