Common evolution of adjacent sunspot groups

Details Common evolution of adjacent sunspot groups Common evolution of adjacent sunspot groups

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..145...77v&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 145, no. 1, p. 77-94.

Physics

10

Magnetic Flux, Polarity, Solar Activity, Solar Magnetic Field, Sunspots, Chromosphere, H Alpha Line, Magnetic Signatures, Photosphere, Umbras

Scientific paper

Debrecen full-disk, white-light photoheliograms and H-alpha filtergrams as well as Meudon magnetograms are used to trace the evolution of two adjacent bipolar sunspots. The proper motions of the principal preceding spots of both groups exhibit quite similar patterns; the spots move along almost parallel tracks and change the direction of their motion on the same day at almost the same heliographic longitude. Three simultaneous emergences of magnetic flux were observed in both groups as well. The hypothesis that these adjacent sunspot groups were magnetically linked below the photosphere is confirmed. Matching the extrapolated magnetic field lines with the chromospheric fibril structure appears to be different in the two groups since they indicate quite different model solutions for each group, i.e., a near-potential magnetic field configuration in the older group and a twisted force-free field configuration in the younger group.

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