Convective instability in differentially rotating disks

Details Convective instability in differentially rotating disks Convective instability in differentially rotating disks

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...388..438r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 388, April 1, 1992, p. 438-450. Research supported by NASA.

Other

112

Accretion Disks, Convective Flow, Magnetohydrodynamic Stability, Mass Flow, Rotating Plasmas, Active Galactic Nuclei, Angular Momentum, Angular Velocity, Momentum Transfer, Quasars

Scientific paper

A normal mode analysis for nonaxisymmetric perturbations in a thin, differentially rotating disk with a vertical structure that is isothermal and convectively unstable is performed. The vertical gravity is assumed to be external and constant. The perturbation scale is assumed to be much shorter than the radius of the disk but comparable to or less than the thickness. The initial value problem is formulated in shearing coordinates. Dispersion relations are obtained for the three limiting cases of zero shear, axisymmetric perturbations, and small radial wavelengths. The full effects of shear are studied by integrating numerically the initial value problem. Nonaxisymmetric local Fourier modes are found to have a radial wavenumber that increases linearly with time in proportion to the shear times the azimuthal wavenumber. While Coriolis forces exert stabilizing effects on the convective modes, reducing their growth rate and the range of unstable wavelengths, shear has destablizing effects inasmuch as it reduces the epicyclic frequency at a given angular velocity. In a Keplerian disk, perturbations with azimuthal wavelengths about 2 times smaller than vertical wavelengths grow exponentially.

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