Theory of convection in a deep rotating spherical shell, and its application to the Sun

The theory of convection in a rotating spherical shell, when applied to the Sun should ultimately satisfy at least three broad constraints. The radial heat flux by the convection must not vary significantly with latitude: an equatorial acceleration must be produced, and the convection must give the right dynamo action to produce the gross feature of a solar cycle. Important quantities to look for in the observations with which a convection theory can be compared include evidence of global velocities of giant convection cells, differences in motion features between low latitudes and high, persistance of motion features over successive rotations, evidence of excessive brightness and variations in total solar luminosity, correlations of velocities between northern and southern hemispheres, and between south and east-west motions, and time periodic changes in motion fields. (Auth.)