The equation of state of a cosmological self-gravitating fluid influenced by thermal or turbulent motion and the primeval background radiation

Details The equation of state of a cosmological self-gravitating fluid influenced by thermal or turbulent motion and the primeval background radiation The equation of state of a cosmological self-gravitating fluid influenced by thermal or turbulent motion and the primeval background radiation

Oct 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981ap%26ss..79..443n&link_type=abstract

Astrophysics and Space Science, vol. 79, no. 2, Oct. 1981, p. 443-461.

Physics

Fluid Dynamics

2

Background Radiation, Cosmology, Equations Of State, Fluid Dynamics, Thermodynamic Properties, Adiabatic Conditions, Fluctuation Theory, Gravitational Effects, Radiation Pressure, Statistical Analysis, Turbulent Flow

Scientific paper

The usual dispersion relation of a self-gravitating cosmological fluid w2 = k2v~ - 4irGp is analyzed within thermodynamical theory. Restricting to a static universe (Einstein Universe with cosmological A- term) an equation of state for the substratum is found including gravitational_pressure. A pure thermal monatomic gas (C~/C~ = ~) shows adiabatic fluctuations of the order \/AN2/N N -1/4, if the non- Newtonian part of the gravitational pressure is included. Non-thermal influences (turbulence) on the equation of state are also discussed. Taking into account the radiation pressure with modification due to the mean free path of the photons in the recombination era, we find critical isothermal fluctuations analogous to the van der Waals gas. The corresponding critical masses are in the range of cluster masses of galaxies (~.` 1O'~M®)

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