Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...378..378d&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 378, Sept. 1, 1991, p. 378-397.
Astronomy and Astrophysics
Astrophysics
19
Angular Velocity, Helioseismology, Magnetohydrodynamic Turbulence, Solar Rotation, Boundary Conditions, Convective Flow, Correlation Coefficients, Eddy Viscosity, Solar Interior
Scientific paper
The dependence of the inner solar angular velocity (ISAV) on the spatial coordinates is examined through helioseismic observation. If the ratios, designated RR, are specified and ISAV is known from the observations, then the azimuthal momentum equation determines the meridional motions. For all realistic values of RR, the stream function of a meridional motion is negative, i.e., the flow rises at the equator and sinks at the poles. Such flows together with the fact that the turbulent convective velocities are negative suggest a natural explanation for the helioseismic observations near the solar surface (with increasing depth, the angular velocity first increases and then decreases). It is proposed that flows with few cells per hemisphere will dominate. Restrictions of this type imposed on the azimuthal momentum equation circumscribe the values of RR. In the simple case under consideration, the eddies take on a slablike appearance elongated along the axis of rotation.
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