Evolution of latitude zonal structure of the large-scale magnetic field in solar cycles

Details Evolution of latitude zonal structure of the large-scale magnetic field in solar cycles Evolution of latitude zonal structure of the large-scale magnetic field in solar cycles

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989soph..119...35m&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 119, no. 1, 1989, p. 35-44.

Physics

75

Solar Cycles, Solar Magnetic Field, H Alpha Line, Lines Of Force, Migration, Polarity, Solar Prominences

Scientific paper

The latitude zonal component of the large-scale solar magnetic field is analyzed using H-alpha charts for the 1905-1982 period, and the poleward migration of prominences is used to calculate the time of reversal of the polar magnetic field for the 1970-1982 period. It is found that in each hemisphere, the polar, middle latitude, and equatorial zones of the predominant polarity of the large-scale magnetic field can be detected by determining the average latitude of prominence samples referred to one boundary of the large-scale magnetic field. Such prominence samples do not have any regular equatorward drift, and they manifest a poleward migration with a variable velocity of up to 30 m/s, depending on the phase of the cycle.

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