Causally limited viscosity and the stability properties of isothermal accretion disks

Details Causally limited viscosity and the stability properties of isothermal accretion disks Causally limited viscosity and the stability properties of isothermal accretion disks

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...432..672w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 432, no. 2, p. 672-679

Other

9

Accretion Disks, Acoustic Propagation, Flow Stability, Hydrodynamics, Isothermal Flow, Viscosity, Active Galactic Nuclei, Stellar Oscillations, X Ray Binaries

Scientific paper

An analytical study is performed to examine the influence of causally limited viscosity on the stability properties of an isothermal accretion disk. We find that the stability and propagating properties of three kinds of oscillation mode in the disk are different from those in the conventional viscosity case, if the viscosity is modified to follow causality. The viscous mode is still stable throughout the disk, but it is no longer a standing wave. It propagates inward with a damping rate proportional to the viscosity parameter alpha. The two inertial-acoustic modes are no longer complex conjugates of one another. Their stability and propagating properties are different. The outward-moving mode is unstable throughout the disk, while the inward-moving mode is unstable in the outer disk but stable in the inner disk when the Mach number of accretion flow is larger than a critical value. We estimate that this critical Mach number is approximately 0.4 if a revised diffusion-type viscosity is adopted and approximately 0.25 if a revised alpha-viscosity is adopted.

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