Meridional circulation in rotating stars. II. Mean steady motions in rotationally and tidally distorted stars

Journal Article · Fri Oct 01 04:00:00 EDT 1982 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/160337· OSTI ID:6424485

Tasoul, J; Tassoul, M

This paper deals with the problem of circulatory currents in the radiative envelope of a nonmagnetic star, which is a synchronously rotating, detached component of a double star. Uniformly valid solutions are found when departure from spherical symmetry is not too large. To the lowest possible order in the ratio of the centrifugal force to gravity at the equator, the velocity field has three nonvanishing components. Actually, the mean steady flow is the superposition of (i) rotationally driven currents (which are symmetrical with respect to both the rotation axis and the equator), (ii) tidally driven currents (which are symmetrical with respect to the tidal axis only), and (iii) motions having no particular symmetry that result from the continuous interaction (via the Coriolis force) between these two meridional circulations and overall rotation.

• Research Organization: Departement de Physique, Universite de Montreal
• OSTI ID: 6424485
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 261:1; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BINARY STARS
CORIOLIS FORCE
FLUID MECHANICS
HYDRODYNAMICS
MAIN SEQUENCE STARS
MATHEMATICAL MODELS
MECHANICS
MOTION
NUMERICAL SOLUTION
ROTATION
STAR MODELS
STARS
TURBULENCE