The monthly number of polar faculae of the Sun were determined from white-light images at spectral band A(eff) = (4100 -4-200) A obtained at the Kislovodsk Solar Station during 1960-1994. Corrected monthly numbers were obtained with the help of the visibility function. The level of polar activity larger than lcr above the monthly running mean was calculated, and the relation between the polar faculae and sunspot cycle was studied. We confirmed earlier results (Makarov and Makarova, 1987) that the monthly number of polar faculae, NPF~ (t) correlates with the monthly sunspot area A,~ (Sp)(t + T) with a time shift T ~-, 6 yr. The new polar faculae cycle began in the middle of 1991. Peculiarities of the first part of sunspot cycle 23 are discussed.
The paper reports the results of the analysis of the data on polar faculae for three solar cycles at the Kislovodsk Station of the Pulk0vo Observatory and on polar bright points in Ca II K line for two solar cycles (1940)(1941)(1942)(1943)(1944)(1945)(1946)(1947)(1948)(1949)(1950)(1951)(1952)(1953)(1954)(1955)(1956)(1957) at the Kodaikanal Station of the Indian Institute of Astrophysics. We have noticed that the monthly numbers of polar faculae and polar bright points in Ca II K line and monthly sunspot areas in each hemisphere of the following solar cycle have a correlation with each other. A new cycle of polar faculae and polar bright points in the Ca II K line begins after the polar magnetic field reversal. We find that the smaller the period between the ending of the polar field reversal and the beginning of a new sunspot cycle is, the more intense is the cycle itself. The intensity of the forthcoming solar cycle (cycle 22) and the periods of strong fluctuations in activity expected in this cycle are also discussed.
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