Large-scale distribution of magnetic fields, green corona and prominences during an extended activity cycle

Details Large-scale distribution of magnetic fields, green corona and prominences during an extended activity cycle Large-scale distribution of magnetic fields, green corona and prominences during an extended activity cycle

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..128..253b&link_type=abstract

(IAU, The Inside the Sun Colloquium, 121st, Versailles, France, May 22-26, 1989) Solar Physics (ISSN 0038-0938), vol. 128, July

Physics

3

Solar Activity, Solar Corona, Solar Cycles, Solar Magnetic Field, Magnetic Field Configurations, Polar Regions, Solar Prominences, Sunspots

Scientific paper

The interrelations of the latitudinal distribution of the coronal green emission maxima, maximal numbers and areas of prominences, magnetic fields, sunspots, and polar faculae in the 20th and 21st sunspot cycles have been investigated. It is again demonstrated how the behavior of all studied data depends on their heliographic latitude. In the polar zone, well separated from the equatorial, following polarity magnetic fields transported only polewards are observed, while the equatorial zone is occupied mostly by leading polarity fields, developed there, moving equatorwards, and crossing the equator to the other hemisphere with the new cycle during the minimum of sunspot activity. This magnetic field distribution is well emphasized by the places of maximal occurrence of prominences and by the distribution of coronal green emission maxima which also differ in dependence on latitude. The question of identifying the first and last evolutionary stages of an extended cycle of activity is discussed, and the existence of a magnetic activity cycle lasting 15-17 years is suggested.

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