Relation between "solar magnetic dipole" and filament bands

Details Relation between "solar magnetic dipole" and filament bands Relation between "solar magnetic dipole" and filament bands

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003esasp.535..749c&link_type=abstract

In: Solar variability as an input to the Earth's environment. International Solar Cycle Studies (ISCS) Symposium, 23 - 28 June 2

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Filaments, Unipolar Regions, Polar Reversal, Solar Cycle

Scientific paper

The "solar magnet" consists of several components: (a) the large-scale unipolar magnetic field regions and their boundaries, the filament bands; (b) a variable dipole yielding polar plumes; (c) other effects. The filament bands have a poleward motion (speeds up to 50 m/s) except for a "recoil" after polar reversal (when the upper unipolar zone disappears at a pole) and the subsequenc "rest" during the minimum of solar activity. The filament bands carry huge currents, which repulse/attract each other. Numerical estimates yield large accelerations which are roughly compensated by the friction of the "skin layer" constituting the unipolar regions slipping over the solar surface as a connected sheet as it is pervaded by a magnetic field and does not mix with the solar surface. When new large-scale unipolar zones originate near the equator the additional repulsion of the filament bands causes the pole-ward motion of the previous filaments; moreover the upper one interacts with the dipole of the polar plumes. The surprising "recoil" of the remaining filament bands may be partially explained by the variation of this dipole and by a recoil of the "skin layer".

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