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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Bumblebee theory on an FLRW background yields a cosmological model whose single free parameter is fitted to supernovae observations, producing deceleration and dark energy behaviors that are compared to Lambda-CDM.
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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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Cosmological implications of Bumblebee theory on an FLRW background
Bumblebee theory on an FLRW background yields a cosmological model whose single free parameter is fitted to supernovae observations, producing deceleration and dark energy behaviors that are compared to Lambda-CDM.