Abstract
Stellar magnetic fields exert torques which, alter the distribution of angular momentum in a star. In the radiative interior of the Sun these torques tend to enforce uniform rotation and the existence of a rapidly rotating core would imply a poloidal field of less than 10–2 G. In the convective envelope magnetic fields generated by dynamo action produce torques which lead to torsional oscillations. A simple nonlinear model allows both multiply periodic and chaotic behaviour. This system demonstrates that both aperiodic magnetic cycles and the irregular modulation responsible for grand minima can be regarded as examples of deterministic chaos. This picture is consistent with the 14C record but implies that the multiply periodic lamination of some Precambrian varves is not associated with the solar cycle.
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Weiss, N.O. (1987). Rotation and Magnetic Fields in the Sun. In: Hillebrandt, W., Meyer-Hofmeister, E., Thomas, HC. (eds) Physical Processes in Comets, Stars and Active Galaxies. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-72640-8_5
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DOI: https://doi.org/10.1007/978-3-642-72640-8_5
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