Abstract
A total eclipse offers a rare opportunity for ground based observers within the shadow path to study the less luminous solar corona at the moment when the intensely bright photosphere is occulted by the Moon’s disk. The free electrons that scatter photospheric radiation producing the K corona are concentrated usually in the regions with strong magnetic fields forming such coronal features as streamers, helmets, plumes, and polar rays. The coronal spectrograms reveal a great number of coronal emission lines (see for example [1]) over the whole range of the spectrum from λ6900 to λ3100 Å. Their existence is attributed to forbidden transitions of very highly ionized atoms of iron, nickel, and calcium, which have lost from 9 to 14 of their electrons under extremely low pressure and high kinetic temperature. Besides the usual features of the corona some observers report about unexpected, usually faint, low excitation emissions at the wavelength of the K and H Ca H, D3 He, Hα and others, registered higher in the solar corona.
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Dermendjiev, V.N. (1997). Faint “Chromospheric” Emission in the Solar Corona: Observational and Theoretical Problems. In: Mouradian, Z., Stavinschi, M. (eds) Theoretical and Observational Problems Related to Solar Eclipses. NATO ASI Series, vol 494. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-5492-5_23
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DOI: https://doi.org/10.1007/978-94-011-5492-5_23
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