The magnetic fields of active regions. II - Rotation

Details The magnetic fields of active regions. II - Rotation The magnetic fields of active regions. II - Rotation

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..126..299h&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 126, April 1990, p. 299-309.

Physics

20

Solar Activity, Solar Magnetic Field, Solar Rotation, Faculae, Helioseismology, Polarity

Scientific paper

The Mount Wilson coarse array data set is used to define active regions in the interval 1967 to August 1988. From the positions of these active regions on consecutive days, rotation rates are derived. The differential rotation of the active regions is calculated and compared with previous magnetic field and plage rates. A correlation is found between rotation rate and region size in the sense that larger regions rotate more slowly. A correlation between rotation rate and cycle phase is suggested which is in agreement with earlier sunspot results. The regions with polarity orientations nearest the normal configuration tend to show rotation rates that are nearest the average values. Most of these results generally support the conclusion that old, weaker magnetic fields have evolved different subsurface connections from the time they were a part of sunspots or plages. It seems possible that they are connected at a shallower layer than are sunspot or plage fields.

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