Variations of the coronal brightness in the line 5303 A in an activity cycle and latitude zonal structure of the coronal magnetic field. Period 1944-1974

A comparison of variations of intensity of the corona using the 5303 A line (Pic-du-Midi observations) with the latitude zonal structure of the coronal magnetic field for 1944-1974 is made using Hα charts. It is shown that the global process of solar activity originally shows up in the polar zone after the polarity reversal and lasts for about 11 years up to the next reversal of the magnetic field of the Sun. A second and more intense manifestation of this process takes place at +30 deg to -30 deg in latitude and also lasts for about 11 years. This means that the total duration of the global solar activity cycle at all latitudes attains 17-18 years