The radial-azimuthal stability of accretion disks - Gas pressure contributions

Details The radial-azimuthal stability of accretion disks - Gas pressure contributions The radial-azimuthal stability of accretion disks - Gas pressure contributions

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...251..689m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 251, no. 2, Nov. 1991, p. 689-692.

Computer Science

Numerical Analysis

6

Accretion Disks, Perturbation Theory, Radiation Pressure, Stellar Mass Accretion, Gas Pressure, Numerical Analysis, Radial Distribution

Scientific paper

A radial-azimuthal stability analysis of a thin, alpha disk accretion flow is presented. The proportion of radiation pressure, Pr, of the unperturbed flow is allowed to vary according to the parameter beta = Pr/P, where P is the total pressure. As is the case for a purely radial analysis, the disk is stable for beta equal to or less than 0.6. However, the coupling of radial and azimuthal perturbations eliminates the viscous instability for such nonradial modes for all values of beta. The group velocity of the retrograde thermal mode is calculated as a function of beta.

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