First Friedmann Equation. The first friedmann equation describes how based on what is in the universe its expansion rate will change over time. The first of the friedmann equations defines a density parameter useful for comparing different cosmological models.
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. Displaystyle frac h 2 h 0 2 omega r a 4 omega m a 3 omega k a 2 omega lambda. The first friedmann equation describes the rate at which cosmological expansion accelerates or decelerates.
Show that the first friedman equation can be presented in the form sum limits i omega i 1 where omega i are relative densities of the components omega i equiv frac rho i rho cr quad rho cr frac 3h 2 8 pi g quad rho curv frac 3 8 pi g frac k a 2 and rho curv describes the contribution to the total density of the spatial curvature.
The first friedmann equation describes the rate at which cosmological expansion accelerates or decelerates. The first of the friedmann equations defines a density parameter useful for comparing different cosmological models. Displaystyle frac h 2 h 0 2 omega r a 4 omega m a 3 omega k a 2 omega lambda. It expresses the basic idea of the field equations which is that non tidal curvature left hand side is caused by the matter that is present locally right hand side.
