Thin Accretion Disks are Unstable via Hydrodynamic Viscosity

Details Thin Accretion Disks are Unstable via Hydrodynamic Viscosity Thin Accretion Disks are Unstable via Hydrodynamic Viscosity

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0153w&link_type=abstract

American Astronomical Society, HEAD meeting #9, #1.53; Bulletin of the American Astronomical Society, Vol. 38, p.337

Astronomy and Astrophysics

Astronomy

Scientific paper

We have studied the effects of ordinary hydrodynamic viscosity on the linear stability of thin accretion disks, including the induced equilibrium meridional flow to lowest consistent order in disk thickness/radius. Perturbing the Navier-Stokes equations produces a set of coupled parabolic equations in which the time derivative and undifferentiated term are uncoupled. This structure allows the formulation of a sufficient condition for instability, which we relate to the viscosity and the accretion rate. It also depends upon the axial mode number. These results complement those of Ortega-Rodriguez and Wagoner (2000), who found that many normal modes grow exponentially at a rate proportional to the viscosity parameter (alpha). We comment on why these results are so different than those in slowly rotating stars, and possible effects of magnetic fields on this instability.

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