The meVSL model's parameter b reduces the baryon drag sound horizon, raising inferred H0, and changes the cosmological time-dilation exponent to n=1-b/4; the paper forecasts SN sample sizes to detect this.
Solutions to the Quasi-flatness and Quasi-lambda Problems
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Big Bang models of the Universe predict rapid domination by curvature, a paradox known as the flatness problem. Solutions to this problem usually leave the Universe exactly flat for every practical purpose. Explaining a nearly but not exactly flat current Universe is a new problem, which we label the quasi-flatness problem. We show how theories incorporating time-varying coupling constants could drive the Universe to a late-time near-flat attractor. A similar problem may be posed with regards to the cosmological constant $\Lambda$, the quasi-lambda problem, and we exhibit a solution to this problem as well.
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Alleviating the Hubble Tension via Cosmological Time Dilation in the meVSL Model
The meVSL model's parameter b reduces the baryon drag sound horizon, raising inferred H0, and changes the cosmological time-dilation exponent to n=1-b/4; the paper forecasts SN sample sizes to detect this.