Abstract
The intensity of the green coronal Fe XIV λ530.3-nm line is correlated with sunspot areas and the magnetic field strength calculated for a distance of 1.1R ⊙. The relation of the green line emission to large-scale and local magnetic fields is shown to change differently with cycle phase. Large-scale coronal magnetic fields play a decisive role at the ascending phase, while a slightly higher correlation of the green line intensity with the local magnetic fields of sunspots is observed at the descending phase. Our results can be used to construct and test various solar coronal heating models.
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Original Russian Text © N.G. Bludova, O.G. Badalyan, 2006, published in Pis’ma v Astronomicheskiĭ Zhurnal, 2006, Vol. 32, No. 10, pp. 777–786.
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Bludova, N.G., Badalyan, O.G. Relation of the coronal green line intensity to magnetic fields and sunspot areas in the solar cycle. Astron. Lett. 32, 698–706 (2006). https://doi.org/10.1134/S1063773706100057
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DOI: https://doi.org/10.1134/S1063773706100057