Turbulent viscosity in a gravitating gaseous disk

Details Turbulent viscosity in a gravitating gaseous disk Turbulent viscosity in a gravitating gaseous disk

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985pazh...11..231m&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 11, Mar. 1985, p. 231-238) Soviet Astronomy Letters (ISSN 0360-0327), vol. 11, Mar.-Apr

Statistics

Computation

3

Accretion Disks, Computational Astrophysics, Rotating Disks, Turbulence, Viscosity, Dissipation, Gravitational Effects

Scientific paper

It is shown that turbulent viscosity in a gravitating gaseous disk may exceed the molecular viscosity, when the disk contains a region which is only marginally stable. The difference in the viscosities is estimated to be a factor of at least h/l exp. 2/3, where h is the disk thickness and l is the mean free path of particles in the disk. The onset of turbulent diffusion in the disk due to a buildup of negative waves of energy in the dissipative medium, is described within the framework of conventional accretion disk theory.

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