Surface magnetic fields during the solar activity cycle

Details Surface magnetic fields during the solar activity cycle Surface magnetic fields during the solar activity cycle

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981soph...74..131h&link_type=abstract

(ESA and European Physical Society, ESLAB Symposium on Physics of Solar Variations, 14th, Scheveningen, Netherlands, Sept. 16-19

Physics

223

Magnetic Flux, Nonuniform Magnetic Fields, Solar Activity, Solar Cycles, Solar Magnetic Field, Data Reduction, Latitude, Solar Rotation, Sunspots

Scientific paper

The behavior of the magnetic field of the sun as measured in the Fe I 5250 A line is summarized. A latitudinal distribution of the fields observed over 13.5 yr is presented, and episodic formation of the polar fields (about 6 gauss) from a poleward drift originating at the sunspots is noted. Weak magnetic fields (-2 to +2) reach a maximum two years before the maximum in the average field. The total flux remains constant from minimum to maximum, with strong magnetic flux exhibiting an equatorward drift; both strong and new flux appear mostly around sunspots. The appearance of new flux implies the decay of flux elsewhere on the sun, because of the measured constancy of total flux; total replacement of the surface flux can occur within ten days. Field annihilation is concentrated in the active latitudes, where strong opposite polarity fields occur close together.

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