The variation of the coronal intensity in the 5303 A line in the activity cycle and the latitudinal zonal structure of the coronal magnetic field - The period 1944-1974

Details The variation of the coronal intensity in the 5303 A line in the activity cycle and the latitudinal zonal structure of the coronal magnetic field - The period 1944-1974 The variation of the coronal intensity in the 5303 A line in the activity cycle and the latitudinal zonal structure of the coronal magnetic field - The period 1944-1974

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987azh....64.1072m&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 64, Sept.-Oct. 1987, p. 1072-1078. In Russian.

Astronomy and Astrophysics

Astronomy

4

Latitude, Line Spectra, Solar Activity, Solar Corona, Solar Magnetic Field, Annual Variations, Spectrum Analysis, Time Dependence

Scientific paper

A comparison of variations of intensity of the corona using the 5303 Å 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 is to be seen 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° to -30° 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.

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