Cooling Flows of Selfgravitating, Rotating, Viscous Systems
Abstract
We obtain selfsimilar solutions that describe the dynamics of a selfgravitating, rotating, viscous systems. We use simplifying assumptions but explicitly include viscosity and the cooling due to the dissipation of energy. By assuming that the turbulent dissipation of energy is a power law of the density and the speed v_{rms} and for a powerlaw dependence of viscosity on the density, pressure, and rotational velocity, we investigate turbulent cooling flows. It has been shown that for cylindrical and spherical cooling flows the similarity indices are the same, and they depend only on the exponents of the dissipation rate and the viscosity model. Depending on the values of the exponents, which the mechanisms of the dissipation and viscosity determine, we may have solutions with different general physical properties. The conservation of the total mass and the angular momentum of the system strongly depend on the mechanism of energy dissipation and the viscosity model.
 Publication:

The Astrophysical Journal
 Pub Date:
 July 2002
 DOI:
 10.1086/340894
 arXiv:
 arXiv:astroph/0108021
 Bibcode:
 2002ApJ...574..198S
 Keywords:

 Hydrodynamics;
 Instabilities;
 Stars: Formation;
 Turbulence;
 Astrophysics
 EPrint:
 19 pages, 5 figures, To appear in ApJ (scheduled for the v574, July 20, 2002)