The rotation of active regions with differing magnetic polarity separations

Details The rotation of active regions with differing magnetic polarity separations The rotation of active regions with differing magnetic polarity separations

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..142..233h&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 142, no. 2, p. 233-248.

Physics

23

Magnetic Flux, Polarity, Solar Activity Effects, Solar Magnetic Field, Solar Rotation, Sunspots, Dynamic Characteristics, Magnetic Signatures, Solar Physics

Scientific paper

The separation of the leading and following portions of plages and sunspot groups, here called polarity separation (PS), is examined as a parameter in the analysis of plage and spot group rotation. A clear and significant dependence of the total magnetic flux of a region on its PS is shown. The average residual rotation rates of regions depend on the PS in that larger separations correspond to slower rotation rates. For sunspots, it is confirmed that smaller and individual sunspots rotate faster than larger spots, and that smaller spot groups rotate faster than larger groups. Groups with larger PSs rotate faster than those with smaller separations, an anomalous effect that may be related to the evolution of plages and spot groups or to connections with subsurface toroidal flux tubes.

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