Turbulent mixing, viscosity, diffusion and gravity in the formation of cosmological structures: the fluid mechanics of dark matter

Details Turbulent mixing, viscosity, diffusion and gravity in the formation of cosmological structures: the fluid mechanics of dark matter Turbulent mixing, viscosity, diffusion and gravity in the formation of cosmological structures: the fluid mechanics of dark matter

2000-03-23

arxiv.org/abs/astro-ph/0003352v5

Journal of Fluids Engineering, Vol. 122, Dec. 2000, 830-835

Astronomy and Astrophysics

Astrophysics

6 pages, no figures, pdf file. See http://www-acs.ucsd.edu/~ir118 for figures and related papers

Scientific paper

Self-gravitational structure formation theory for astrophysics and cosmology is revised using nonlinear fluid mechanics. Gibson's 1996-2000 theory balances fluid mechanical forces with gravitational forces and density diffusion with gravitational diffusion at critical viscous, turbulent, magnetic, and diffusion length scales termed Schwarz scales. Instability occurs for scales larger than the largest Schwarz scale rather than only for scales larger than the acoustic scale introduced by Jeans 1902. From the new theory, the inner-halo-dark-matter of galaxies consists of dark proto-globular-star-cluster (PGC) clumps of small-planetary-mass objects called primordial fog particles (PFPs) formed soon after decoupling at 300,000 years. PFPs explain Schild's 1996 "rogue planets >... likely to be the missing mass" of a quasar lens-galaxy. WIMP dark matter fluid is super-diffusive and fragments at large L_SD scales to form outer-galaxy-halos. In the beginning of structure formation 30,000 years after the Big Bang the viscous Schwarz scale L_SV matched the horizon scale L_H at proto-galaxy-supercluster masses, decreasing to proto-galaxy fragments at 300,000 years. WIMP diffusivities from observed outer-halo (L_SD) scales indicate WIMP particle masses in the neutrino rather than neutralino range.

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