Astronomy and Astrophysics – Astrophysics
Scientific paper
1999-04-21
Gibson, C. H., The Identification of Dark Matter, Neil J. C. Spooner, Ed., World Scientific, Singapore, 1997, 114-119
Astronomy and Astrophysics
Astrophysics
6 page original for 1996 U. Sheffield Conference Proceedings, 3 figures, PDF file
Scientific paper
Dark matter appears in two forms as a consequence of the fluid mechanics of self-gravitational condensation. Condensation occurs primarily on non-acoustic nuclei rather than on the acoustic nuclei of the Jeans (1902) criterion, leading to a very different scenario for structure formation. Viscous forces at 10^12 s (30,000 y) after the big bang permit decelerations of 10^47 kg protosupercluster plasma masses, and 10^42 kg protogalaxy masses at 10^13 s (300,000 y). Then gas formed, and all the baryonic universe became a "primordial fog" of 10^23 kg particles at the viscous Schwarz scale: 100% dark matter. Some of these H-He objects have collected to form stars, but most persist as dark dwarfs in galaxy halos. They manifest themselves in quasar microlensing observations as "rogue planets", Schild (1996), "dark galaxies", Hawkins (1996), and as comets "brought out of cold storage", O'Dell and Handron (1996). Non-baryonic WIMP fluids are superviscous, with large viscous Schwarz scales, and condense slowly to form most of the dark matter of galaxy superclusterhalos and clusterhalos.
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