The Large-Scale Structure of the Universe: Relation to Turbulence Theory and the Stochastic Expansion

Details The Large-Scale Structure of the Universe: Relation to Turbulence Theory and the Stochastic Expansion The Large-Scale Structure of the Universe: Relation to Turbulence Theory and the Stochastic Expansion

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..dfd.kg010m&link_type=abstract

American Physical Society, Division of Fluid Dymanics 55th Annual Meeting, abstract #KG.010

Statistics

Computation

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The large-scale structure and dynamical evolution of the universe is modeled as a fluid, a good approximation for baryonic mass but possibly problematic for collisionless dark matter. The dynamical equations describing this self-gravitating system are scale-free allowing the spatial two-point statistics of galaxies to be a power-law. The observed velocity distribution is nearly Gaussian, which can be exploited methodologically. The cosmological process is statistically homogeneous and isotropic, paralleling turbulence. The inviscid Euler equation for the process has no pressure, but a gravitational potential which mimics the role of pressure and, together with the density, provides the analog of an equation of state. The observed cosmological density correlation defect is a power law, r-1.78, over nine orders of magnitude. For a compressible flow, the velocity correlation is predicted to have a defect like r^0.22, in contrast with the Kolmogorov-Obukhov law for incompressible turbulence of r^2/3. For computation, the system of equations is represented in terms of the Wiener stochastic expansion for the process and exploits Feynman path integrals. The Wiener expansion introduces no adjustable parameters and assures a positive energy spectrum. A computational model is under development.

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