Abstract
The solar magnetized surface reveals a stable spin period - the Carrington period and a stable oscillation period - the Hale period. The latter is traced by each of the low-order multipole moments, whereby the total magnetic energy (near the surface) is more or less constant. This highly non-stochastic structure is reminiscent of a permanent magnetic flux frozen into the Sun’s radiative core, and dragged out into the heliosphere by the solar wind. The radius-dependent torque exerted by this magnetic flux can restore the observed system of torsional oscillations of the convection zone.
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Kundt, W. (1993). Magnetic Field and Differential Rotation of the Sun. In: Krause, F., Rädler, KH., Rüdiger, G. (eds) The Cosmic Dynamo. International Astronomical Union Symposia / Union Astronomique Internationale, vol 157. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-0772-3_13
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DOI: https://doi.org/10.1007/978-94-011-0772-3_13
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