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 ~b2, m and low latitude ~bl.,,. It is shown that the mean latitude of the filament band ~P2,,,, at the minimum -m of the cycle correlates, with p = 0.94, with the maximum -M sunspot area S(M) and maximum Wolf number W(M) ilz the succeeding solar cycle M. It is shown that the mean latitude of the low-latitude filament band q~,,~ is linearly dependent on the mean latitude filament band q~z, m + 1 at the succeeding minimum. We found a correlation of the latitude of the low-latitude filament band q)~, ,, with the maximum sunspot area in the M + 1 cycle. This enables us to predict the power of two succeeding 11-year solar cycles on the basis of the latitude of filament bands at the minimum of activity, 1985-1986: W(22)-~ 205 • 10, W(23)-210 • 10. The importance of the relationships found for theory and applied aspects is emphasized. An attempt is made to interpret the relationships physically.
We have studied the latitude-time distribution of the green (5303 A) coronal line emission for 1940-1989 from observations by Waldmeier (1957), Kislovodsk, Lomnickj~ Stlt, Norikura, and Pic-du-Midi -Q.B.S.A. (1955. We have compared these data with the distributions of the weak magnetic field (Stenflo, 1988), of polar faculae and sunspots, and have given our interpretation of the results. We have found that a new cycle of coronal activity commences after the polar field reversal in the form of two components in each hemisphere. We identify the first component with the polar faculae that appear at latitude 40 o and migrate polewards. The second component representing sunspots shows up at 40 ~ latitude 5-6 years after and drifts equatorward. Thus the global coronal activity cycle has a duration of 16-17 years and is described by two components that reflect the activity of polar faculae and sunspots.
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