The flatness problem and $\Lambda$

Abstract

By way of a complete integration of the Friedmann equations, in terms of observables, it is shown that for the cosmological constant $\Lambda >0$ there exist non-flat FLRW models for which the total density parameter $\Omega$ remains $\sim 1$ throughout the entire history of the universe. Further, it is shown that in a precise quantitative sense these models are not finely tuned. When observations are brought to bear on the theory, and in particular the WMAP observations, they confirm that we live in just such a universe. The conclusion holds when the classical notion of $\Lambda$ is extended to dark energy.

Final form to appear in Physical Review Letters. Further information at http://grtensor.org/Robertson/

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• Astrophysics in 2005
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• Exact and Perturbed Friedmann-Lemaitre Cosmologies
• Horizon, homogeneity and flatness problems -- do their resolutions really depend upon inflation?
• Damping of cosmological tensor modes in Horndeski theories after GW170817
• A cyclic universe with colour fields