Abstract
The very early universe must have been extremely homogeneous, even on scales far exceeding the particle horizon. Within the framework of the standard Friedmann cosmology, homogenization can only be achieved by quantum effects which violate classical causality. This could happen when the particle horizon was smaller than the Compton wavelength of the pion. The assumption that statistical departures from equilibrium started to grow after this epoch leads to a prediction of the density fluctuations at recombination. The amplitude ν of the fluctuations should have a maximum of about 0.007 on scales of 81017M. For smaller scales, ν ∝M +1/6, and for larger scales, ν ∝M −1/2. This suggests that superclusters condense out at a red shift of about 11, and clusters and then galaxies form shortly after by fragmentation.
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Clutton-Brock, M. Why is the universe homogeneous?. Astrophys Space Sci 30, 395–408 (1974). https://doi.org/10.1007/BF00648285
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DOI: https://doi.org/10.1007/BF00648285