Baroclinic waves in a vertically stratified thin accretion disk

Details Baroclinic waves in a vertically stratified thin accretion disk Baroclinic waves in a vertically stratified thin accretion disk

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...166..359k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 166, no. 1-2, Sept. 1986, p. 359-367. Research supported by the Max-Planck-Ins

Astronomy and Astrophysics

Astrophysics

17

Accretion Disks, Baroclinic Waves, Stratification, Baroclinic Instability, Buoyancy, Linear Equations, Resonance, Turbulence

Scientific paper

The conditions for steady equilibrium and energy transport in general require a thin accretion disk to be baroclinic, i.e. the rotation speed to vary with height in the disk. A necessary condition for baroclinic instability is derived which is analogous to that encountered in geophysics. The instabilty can occur only if the radial scale length is locally comparable to the vertical scale height H, or if the vertical stratification is close to adiabatic. The maximum level of turbulence expected is limited by the dominant effect of the shear in the Kepler flow. The role of the thermal wind and of meridional circulations in establishing the mean state is elucidated. Attention is drawn to the role of buoyancy resonances which may play an important role in many wave phenomena in disks.

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