Abstract
The dynamically-driven adiabatic motions inside an obliquely rotating magnetic star are studied in detail for three distributions of magnetic flux through the star. Ohmic dissipation of the currents induced by the motions yields an upper limit to the time in which the obliquity angle achieves its asymptotic value. This time is sensitive to the rotation of the star and its total magnetic flux. Some tentative conclusions are drawn concerning the distribution of flux through a star, and the likelihood of limited, magnetically-driven mixing during stellar evolution.
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