Behavior of the angular velocity in the lower part of the solar convection zone

Journal Article · Wed Mar 01 04:00:00 EST 1989 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/167214· OSTI ID:6224965

Durney, B R

The solar angular velocity is expanded in Legendre polynomials. The meridional motions are restricted to one or two cells per hemisphere, and an approximation to the azimuthal equation of motion is integrated with respect to r with the help of the boundary condition at r = Rc, the lower boundary of the solar convection zone (SCZ). The Reynolds stresses appearing in the equation are estimated for the lower SCZ, and approximate expressions are derived for the turbulent viscosity coefficients (which are due to the influence of the mean flow on the turbulent velocities). It is shown that the assumption of isotropic viscosity is always open to criticism. An order-of-magnitude estimate of the different terms in the E(r) and E(theta) equations suggests that the Reynolds and viscous stresses are important only near the boundaries of the SCZ. Away from the boundaries, in the Taylor-Proudman region, the suggested balance is between Coriolis forces, pressure gradients, and buoyancy forces. 47 refs.

• Research Organization: National Solar Observatory, Tucson, AZ
• OSTI ID: 6224965
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 338; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ANGULAR VELOCITY
BOUNDARY CONDITIONS
CONVECTION
CORIOLIS FORCE
DIFFERENTIAL EQUATIONS
ENERGY TRANSFER
EQUATIONS
EQUATIONS OF MOTION
FUNCTIONS
HEAT TRANSFER
LEGENDRE POLYNOMIALS
MAIN SEQUENCE STARS
MASS TRANSFER
MOTION
PARTIAL DIFFERENTIAL EQUATIONS
POLYNOMIALS
PRESSURE GRADIENTS
REYNOLDS NUMBER
ROTATION
STARS
SUN
VELOCITY
VISCOSITY