First Friedmann Equation. 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. This term originally was used as a means to determine the geometry of the field where.
Alexander Friedmann 1888 1925 Cosmology Equations Scientist from es.pinterest.com
C is the critical density for which the geometry is flat. The first friedmann equation describes the rate at which cosmological expansion accelerates or decelerates. 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.
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 0 r a 4 omega 0 m a 3 omega 0 k a 2 omega 0 lambda. C is the critical density for which the geometry is flat. 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. The first friedmann equation describes how based on what is in the universe its expansion rate will change over time.
