GLOBAL SOLAR-CYCLE IN THE DISTRIBUTION OF THE GREEN CORONAL EMISSION PERIOD - 1940-1989

We have studied the latitude-time distribution of the green (5303 angstrom) coronal line emission for 1940-1989 from observations by Waldmeier (1957), Kislovodsk, Lomnicky Stit, Norikura, and Pic-du-Midi - Q.B.S.A. (1955-1987). 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-degrees and migrate polewards. The second component representing sunspots shows up at 40-degrees 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.