BBN observations of light nuclei abundances constrain cosmological models with Weylian boundaries via modified Friedmann equations, numerical thermonuclear rate calculations, and MCMC analysis.
23 −0.17 Model III: v ( ϕ ) = γϕ 2 + δϕ 4 2.92 2.96 3.00 σ 0 1 2 3 /uni03BC σ = 2.971 ± 0.014 0 1 2 3 /uni03BC /uni03BC= 1.69 ± 0.63 Model III: v ( ϕ ) = σμ − /uni03BCϕ FIG
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Big Bang Nucleosynthesis constraints on the cosmological evolution in a Universe with a Weylian Boundary
BBN observations of light nuclei abundances constrain cosmological models with Weylian boundaries via modified Friedmann equations, numerical thermonuclear rate calculations, and MCMC analysis.