The space-time distribution of brightness of the Fe XIV, 530.3 nm coronal green line and its cyclic variations are analysed for a long time interval of more than five cycles (1943–2001). For this purpose a special movie has been made. It is shown that a substantial spatial reorganization of the coronal green-line brightness (CGLB) takes a relatively short time and occurs close to the so-called reference points of the cycle, as derived from the series of various solar activity indices. The ‘active longitudes' lasting for 1.5–3.0 years are found to exist in the CGLB. The antipodal and ‘intermittent' active longitudes are identified. For the time interval 1977–2001, it has been corroborated that the CGLB is strongly influenced by the magnetic field strength. An agreement is shown to exist between the spatial structure on the CGLB synoptic charts and those of the magnetic field strength. It is shown that the nature of the relationship between the CGLB and the magnetic field strengths in the corona inside and outside the sunspot formation zone differ significantly.
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coronal green line;
coronal magnetic field;
Document Type: Research Article
Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, 142190, Troitsk, Russia
Astronomical Institute of the Slovak Academy of Sciences, 05960, Tatranská Lomnica, Slovak Republic
Publication date: 2004-12-01
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