Numerical Simulation of Viscous Accretion Disks

Details Numerical Simulation of Viscous Accretion Disks Numerical Simulation of Viscous Accretion Disks

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...187.2501d&link_type=abstract

American Astronomical Society, 187th AAS Meeting, #25.01; Bulletin of the American Astronomical Society, Vol. 27, p.1322

Astronomy and Astrophysics

Astronomy

Scientific paper

A two-dimensional numerical hydrodynamics code is developed to model viscous accretion discs, employing the method of smoothed particle hydrodynamics. The effective shear viscosity present in the code is evaluated. Using a polytropic equation of state, models of self-gravitating accretion disks are evolved with a range of physical parameters, including viscosity. From these models it is found that a characteristic mass accretion rate, constant with time, tends to be maintained by the accretion disks, and that mass accretion is inversely proportional to the strength of the local shear viscous force. This is a consequence of the damping effect of local viscous forces upon the global non-axisymmetric modes that primarily drive accretion in these disks. In addition, the formation of satellites is observed in models which also develop a dominating m=1 tidal mode. The relevance of these satellites to planet formation is speculated.

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