Resonant Oscillatory Modes in Hydrodynamic Simulations of Accretion Disks

Details Resonant Oscillatory Modes in Hydrodynamic Simulations of Accretion Disks Resonant Oscillatory Modes in Hydrodynamic Simulations of Accretion Disks

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0151c&link_type=abstract

American Astronomical Society, HEAD meeting #9, #1.51; Bulletin of the American Astronomical Society, Vol. 38, p.337

Computer Science

Sound

Scientific paper

We use a pseudo-spectral algorithm to perform a detailed study of the properties of the inner regions of two-dimensional, viscous accretion disks. We find that stable solutions do not exist for most combinations of parameters. When the disks are unstable, their regions near the maximum of the radial epicyclic frequency oscillate, generating outward axisymmetric waves. Besides these strong axisymmetric waves, the flows inside those regions of the disks are sometimes also unstable to non-axisymmetric perturbations, forming one-armed or two-armed spiral waves. The frequencies of the axisymmetric sound waves and the spiral waves are in ratios of small integers, providing a plausible explanation of the high-frequency QPOs observed from accreting black holes.

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