Other
Scientific paper
Sep 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997acasn..38..250w&link_type=abstract
Acta Astronomica Sinica, vol. 38, p. 250
Other
Accretion Disks, Astronomical Models, Viscosity, Pulses, Radial Flow, Magnetic Effects
Scientific paper
A model of weakly magnetized isothermal accretion disks with diffusion-type viscosity is investigated in this paper. The pulsational instability of the disks, arising from nonaxisymmetric perturbations (including radial, azimuthal, and vertical perturbations) is discussed on the basis of the authors' previous work. It is shown that the radial perturbation is the most important and essential one. There are no pulsational instabilities arising from either azimuthal or vertical perturbations in the absence of the radial perturbation. In contrast, in the presence of the radial perturbation, there exist not only the pure radial pulsational instability, but also those which arise from the coupled radial-vertical perturbations and the coupled radial-azimuthal ones. For the case in which the above perturbations in the three directions coexist, the corresponding nonaxisymmetric pulsational instability will probably exist.
Wang Ding-Xiong
Yang Lan-Tian
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