Sasakian manifold: Difference between revisions
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{{Unreferenced stub|auto=yes|date=December 2009}} | |||
The '''Density Contrast''' is a parameter used in [[galaxy formation]] to indicate where there are local enhancements in matter density. | |||
:<math>\Delta=\frac{\partial\varrho}{\varrho}</math> | |||
It is believed that after [[inflation (cosmology)|inflation]], although the universe was mostly uniform, some regions were slightly denser than others with contrast densities on the order of 1 trillionth. As the [[particle horizon|horizon distance]] expanded, the enclosed causally connected (i.e. gravitationally connected) masses increased until they reached the [[Jeans mass]] and began to collapse, which allowed [[galaxies]], [[galaxy clusters]], [[superclusters]], and [[Galaxy filament|filaments]] to form. | |||
{{DEFAULTSORT:Density Contrast}} | |||
[[Category:Physical cosmology]] | |||
[[Category:Cosmic inflation]] | |||
{{Astronomy-stub}} | |||
Latest revision as of 15:29, 11 April 2013
Template:Unreferenced stub The Density Contrast is a parameter used in galaxy formation to indicate where there are local enhancements in matter density.
It is believed that after inflation, although the universe was mostly uniform, some regions were slightly denser than others with contrast densities on the order of 1 trillionth. As the horizon distance expanded, the enclosed causally connected (i.e. gravitationally connected) masses increased until they reached the Jeans mass and began to collapse, which allowed galaxies, galaxy clusters, superclusters, and filaments to form.
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