In view of the uncertainty in the angular velocity (r, 0) in the solar interior, we have worked out the general behavior of the solar dynamo for horizontal shear (() /aO) for comparison with the earlier models based on vertical shear (a /ar). The horizontal shear produces greater complexity, with the fields at the surface migrating toward the equator (for a uniform distribution of shear and cyclonic convection) and a layer of counter migrating fields at the bottom of the dynamo. More important, perhaps, the horizontal shear excites the even and odd modes equally, whereas vertical shear excites the odd mode before the even mode.
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Lerche et al. (1972) studied this question.