Density fluctuations in the universe after the recombination period
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It is shown that the cosmic matter gas after the recombination period can be regarded in a very good approximation as a general relativistic Boltzmann gas in the very vicinity of equilibrium. As a consequence, spatial temperature fluctuations (ΔT/T)≊10−5 imply immense density fluctuations up to (Δp/p)≊105.
KeywordsRecombination Temperature Fluctuation Density Fluctuation Spatial Temperature Cosmic Matter
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