Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...277..806c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 277, Feb. 15, 1984, p. 806-812.
Astronomy and Astrophysics
Astrophysics
11
Accretion Disks, Baroclinic Instability, Reynolds Stress, Stellar Mass Accretion, Stellar Rotation, Variable Stars, Baroclinic Waves, Boundary Value Problems, Eigenvalues, Perturbation, Stellar Radiation
Scientific paper
The instability of linear, nonaxisymmetric baroclinic waves in the radiative regions of a thin accretion disk is investigated with simplifying assumptions used in the representation of the structure of the basic state. As in stars with rotation laws deviating from rotation on cylinders, the departure from barotropy ("baroclinicity") resulting from such rotation feeds potential energy from the basic state into the kinetic energy of the baroclinic motions. The baroclinic instability is considered as a possible mechanism for driving turbulence in disks. Estimates of the Reynolds stress from baroclinic waves indicate that the degree of baroclinicity in stationary disk models is insufficient to account for the large viscosity inferred from observations of, e.g., cataclysmic variables.
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