Meridional circulation in the surface layers of rotating stars

Details Meridional circulation in the surface layers of rotating stars Meridional circulation in the surface layers of rotating stars

Dec 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....61..747s&link_type=abstract

Astronomy and Astrophysics, vol. 61, no. 5, Dec. 1977, p. 747-754.

Astronomy and Astrophysics

Astrophysics

13

Early Stars, Meridional Flow, Stellar Envelopes, Stellar Rotation, Surface Layers, Angular Velocity, Astrophysics, Boundary Layers, Inertia, Partial Differential Equations

Scientific paper

The influence of self-inertia on the meridional circulation in the radiative envelopes of rotating early-type stars is examined. It is found that the inertia of the circulation becomes important in a shallow subsurface boundary layer having a relative depth determined by the approximate ratio of centrifugal to gravitational force, and by the ratio of the free-fall time to the Kelvin-Helmholtz contraction time. The structure equations appropriate to the boundary layer are derived using stretched variable techniques, and qualitative features of the flow discussed. There is found to be minimal deviation from the Von Zeipel gravity darkening law through the boundary layer for all rotation speeds.

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