First Friedmann Equation. The first of the friedmann equations defines a density parameter useful for comparing different cosmological models. Let s refer to it as the acceleration equation.
The first friedmann equation describes the rate at which cosmological expansion accelerates or decelerates. When is the matter dark plus baryonic density today is the spatial curvature density today and is the cosmological constant or vacuum density today. C is the critical density for which the geometry is flat.
First general relativistic models by einstein predicted a contracting universe 1917 introduction of cosmological constant by einstein 1922 the friedmann equation predicted an expanding universe 1928 georges lemaitre independently concluded the same lemaitre was the first to propose a primeval atom theory later known as the big bang.
The first friedmann equation is often seen in terms of the present values of the density parameters that is h 2 h 0 2 ω r a 4 ω m a 3 ω k a 2 ω λ. The first friedmann equation describes how based on what is in the universe its expansion rate will change over time. The first friedmann equation is often seen in terms of the present values of the density parameters that is here is the radiation density today i e. The first friedmann equation is often seen in terms of the present values of the density parameters that is h 2 h 0 2 ω 0 r a 4 ω 0 m a 3 ω 0 k a 2 ω 0 λ.
