On some statistical and morphological characteristics of the quiescent prominences of solar activity cycle N 21

  • M. Sh. Gigolashvili
  • I. S. Iluridze
Conference paper
Part of the Lecture Notes in Physics book series (LNP, volume 363)


The observational data obtained at Abastumani Astrophysical Observatory of Georgian SSR Academy of Sciences, the data published in Monthly Bulletins “Solar Data” and Rome Astronomical Observatory Bulletin “Photographic Journal of the Sun” have been used. Long life-time objects maintaining their form and structural peculiarities were chosen for investigation. The filaments observed during less than 3 days were not considered.

The latitude distribution of quiescent prominences in time is studied both for each year of the solar activity cycle N 21 and for the whole one in 1975–1985. It was found that during the whole cycle the latitude distribution of quiescent prominences is of the pattern specific to both quiescent and active prominences at the moment of the solar activity minimum according to Waldmaier in 1933–1943. It should be noted that there is not such a similarity in yearly distribution during the whole solar activity cycle.

For revealing the sizes specific to quiescent prominences observed just on the solar limb, the differences {ie291-1} between the heliographic latitudes of the extremely northern and southern points were measured. The dependence of {ie291-2} on the prominence number is studied. It is seen that most frequently there are prominences with {ie291-3} 3°. Then, there is a large group with a wide interval of {ie291-4}, the average of which {ie291-5} 15°, though two subgroups can be distinguished with their {ie291-6} about 10° and 19°. There is a small numer of prominences with {ie291-7} 25°.

It can be suggested that the prominences nearly parallel to the solar equator, belong to the first group. The prominences of the second group form a comparatively wide angle to the equator. The prominences almost meridional to the solar surface belong to the most scanty third group. The above dependence, reflects and includes both the lifetime of filaments and the effect of the solar differential rotation on the location on the solar surface.

Copyright information

© Springer-Verlag 1990

Authors and Affiliations

  • M. Sh. Gigolashvili
    • 1
  • I. S. Iluridze
    • 1
  1. 1.Abastumani Astrophysical ObservatoryGeorgian SSR Academy of SciencesGeorgiaUSSR

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