The fluid mechanics of dark matter formation: Why does Jeans's (1902 & 1929) theory fail?
| dc.creator | Gibson, Carl H. | |
| dc.date | 1999-04-26 | |
| dc.date.accessioned | 2026-07-07T02:31:24Z | |
| dc.date.available | 2026-07-07T02:31:24Z | |
| dc.description | Jeans's (1902 & 1929) linear gravitational instability criterion gives truly spectacular errors in its predictions of cosmological structure formation according to Gibson's (1996) new nonlinear theory. Scales are determined by viscous or turbulent forces, or by diffusivity, at Schwarz length scales L_SV, L_ST, or L_SD, respectively, whichever is larger. By these new criteria, void formation begins in the plasma epoch soon after matter dominates energy, at L approx L_SV = (gamma nu / rho G)^1/2 scales corresponding to protosuperclusters, decreasing to protogalaxies at the plasma-gas transition, where gamma is the rate-of-strain of the expanding universe, nu is the kinematic viscosity, rho is the density, and G is Newton's gravitational constant. Condensation of the primordial gas occurs at mass scales a trillion times less than the Jeans mass to form a `fog' of micro-brown-dwarf (MBD) particles that persist as the galactic baryonic dark matter, as reported by Schild (1996) from quasar-microlensing studies. Nonbaryonic dark matter condensation is prevented by its enormous diffusivity at scales smaller than L_SD = (D^2 /rho G)^1/2, where D is the diffusivity, so it forms outer halos of galaxies, cluster-halos of galaxy clusters, and supercluster-halos. | |
| dc.description | submitted to Astronomy and Astrophysics | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9904365 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9904365 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/14140 | |
| dc.subject | Astrophysics | |
| dc.title | The fluid mechanics of dark matter formation: Why does Jeans's (1902 & 1929) theory fail? | |
| dc.type | text |