Baroclinic instability in stars

Details Baroclinic instability in stars Baroclinic instability in stars

Mar 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...132...89s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 132, no. 1, March 1984, p. 89-96. Research supported by the Alfred P. Sloan Fo

Astronomy and Astrophysics

Astrophysics

18

Astrophysics, Baroclinic Instability, Red Giant Stars, Stellar Rotation, Adiabatic Conditions, Angular Velocity, Flow Stability, Lithium, Vorticity Equations

Scientific paper

The conditions for the occurrence of adiabatic baroclinic instability in differentially rotating stars are studied using the quasi-geostrophic approximation on a β-plane. In rapidly rotating stars (near breakup) the instability can occur throughout the star. In slowly rotating stars, it can only occur in very narrow regions located near (1) the center of the star, (2) the boundary of a convection zone, (3) a jump in the molecular weight or in the buoyancy frequency, or (4) a jump in the gradient of the rotation rate. It is concluded that the instability cannot be responsible for the mixing needed to explain the Li abundance anomalies in main sequence stars or the low neutrino flux of the Sun. It could however, be important for mixing near the cores of red giants.

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