The latitude of filament bands at the sunspot minimum and the activity level in the two following 11-year solar cycles

Details The latitude of filament bands at the sunspot minimum and the activity level in the two following 11-year solar cycles The latitude of filament bands at the sunspot minimum and the activity level in the two following 11-year solar cycles

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..137..385m&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 137, Feb. 1992, p. 385-394.

Physics

13

Solar Cycles, Solar Prominences, Sunspots, Magnetic Field Configurations, Solar Magnetic Field

Scientific paper

The zonal structure of the distribution of filaments is considered. The mean latitudes of two filament bands are calculated in each solar hemisphere at the minima of the sunspot cycle in the period 1924-1986: middle latitude phi2,m and low latitude phi1,m. It is shown that the mean latitude of the filament band phi2,m at the minimum - m of the cycle correlates, with rho = 0.94, with the maximum - M sunspot area S(M) and maximum Wolf number W(M) in the succeeding solar cycle M. It is shown that the mean latitude of the low-latitude filament band phi1,m is linearly dependent on the mean latitude filament band phi2,m + 1 at the succeeding minimum. A correlation of the latitude of the low-latitude filament band phi1,m with the maximum sunspot area in the M + 1 cycle is found. The power of two succeeding 11-year solar cycles can then be predicted on the basis of the latitude of filament bands at the minimum of activity.

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