Effect of turbulent viscosity on the isothermal collapse of a rotating protostellar cloud
Abstract
The isothermal collapse of a uniformdensity pure H2 10K protostellar cloud of 1 solar mass rotating rigidly at 3.5 x 10 to the 13th/s is investigated analytically, modifying the twodimensional Eulerianhydrodynamics simulation of Black and Bodenheimer (1975 and 1976) to include turbulentviscosity effects and imposing constantvolume boundary conditions. The results are presented graphically and compared with those for the corresponding inviscid cases and with the phenomenological model of turbulent viscosity of Regev and Shaviv (1980 and 1981). Viscosity is found to retard collapse and increase the density toward the center, but not to suppress the initial ring structure completely (for realistic values of the viscosity force) during the time the collapse could be followed in the simulations.
 Publication:

The Astrophysical Journal
 Pub Date:
 July 1985
 DOI:
 10.1086/163317
 Bibcode:
 1985ApJ...294..502V
 Keywords:

 Angular Momentum;
 Eddy Viscosity;
 Gravitational Collapse;
 Molecular Clouds;
 Protostars;
 Stellar Evolution;
 Computational Astrophysics;
 Density Distribution;
 Hydrodynamic Equations;
 Isothermal Processes;
 Momentum Transfer;
 Ring Structures;
 Astrophysics