Fossils of turbulence and non-turbulence in the primordial universe: the   fluid mechanics of dark matter
  Was the primordial universe turbulent or non-turbulent soon after the Big Bang? How did the hydrodynamic state of the early universe affect the formation of structure from gravitational forces, and how did the formation of structure by gravity affect the hydrodynamic state of the flow? What can be said about the dark matter that comprises 99.9 % of the mass of the universe according to most cosmological models? Space telescope measurements show answers to these questions persist literally frozen as fossils of the primordial turbulence and nonturbulence that controlled structure formation, contrary to standard cosmology which relies on the erroneous Jeans 1902 linear-inviscid-acoustic theory and a variety of associated misconceptions (e. g., cold dark matter). When effects of viscosity, turbulence, and diffusion are included, vastly different structure scenarios and a clear explanation for the dark matter emerge. From Gibson's 1996 theory the baryonic (ordinary) dark matter is comprised of proto-globular-star-cluster (PGC) clumps of hydrogenous planetoids termed ``primordial fog particles''(PFPs), observed by Schild 1996 as ``rogue planets ... likely to be the missing mass'' of a quasar lensing galaxy. The weakly collisional non-baryonic dark matter diffuses to form outer halos of galaxies and galaxy clusters. 
Carl H. Gibson (Univ. of Cal. San Diego)