Maunder convection mode on the sun and long solar activity minima

Details Maunder convection mode on the sun and long solar activity minima Maunder convection mode on the sun and long solar activity minima

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...82..427d&link_type=abstract

(International Astronomical Union and Akademiia Nauk SSSR, Colloquium on Problems of Solar and Stellar Oscillations, 66th, Nauch

Physics

2

Convection, Solar Activity, Solar Rotation, Angular Velocity, Solar Magnetic Field, Velocity Distribution

Scientific paper

A model is proposed for velocity field oscillations in the solar convective zone. The system of convective equations is investigated for a thin rotating spherical envelope when the rotation velocity is a function of the coordinates. It is demonstrated that two different structures of convective cells (longitudinal or latitudinal) can exist in the envelope depending on gradient values of the rotation velocity and Prandtl number. The supposition is made that two different regimes of convection (stationary and autofluctuating) are possible in the envelope when the angular velocity gradients are determined by the convection itself. For the case of autofluctuating regime, the alternation of longitudinal and latitudinal structure of convection is effected. With the assumption that on the sun there exists an autooscillating convection regime, the periods of the existence of latitudinal convection structure may be associated with long periods of activity minima. This is so because, according to Cowling's (1951) theorem, the action of the axisymmetric magnetic field generation mechanism is impossible under conditions of axisymmetric velocity structures.

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