Abstract
The Ca+ K line of the quiescent prominence of 15 October 1969 observed at the Abastumani Astrophysical Observatory of the Academy of Sciences of Georgia, U.S.S.R. is studied in detail. The behaviour of various fragments of the prominence with the line-of-sight Doppler velocities is investigated for different places of the prominence along the spectrum height. Due to superposition of the fragments and the radial velocities a complex non-gaussian profile of the spectral line is formed. Decomposition of the non-gaussian profile into suitable gaussian ones is made with a computer yielding objectivity and high accuracy. The rms error for the intensities in the decomposition is about 5%.
It is found that the components into which the Ca+ K line decomposes at each level, are traced while proceeding from one photometric section to another throughout the spectral height.
A hypothesis on the preferably filamentary structure of the prominence is put forward.
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References
Dunn, R. B.: 1960, Thesis, Harvard University.
Engvold, O.: 1976, Solar Phys. 49, 283.
Gigolashvili, M. Sh.: 1976, Observational Problems of Astronomy, Ed. ‘Nauka’, Leningrad, pp. 8–9.
Gigolashvili, M. Sh.: 1978, Solar Phys. 60, 296.
Hirayama, T., Nakagomi, Y., and Okamoto, T.: 1979, ‘Physics of Solar Prominences’, IAU Colloq. 44, 48.
Khetsuriani, Ts. S. and Gigolashvili, M. Sh.: 1975, Bull. Abast. Astrophys. Obs. 46, 189.
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Gigolashvili, M.S., Zhugzhda, Y.D. Fine structure of motions in a quiescent prominence. Sol Phys 77, 95–108 (1982). https://doi.org/10.1007/BF00156098
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DOI: https://doi.org/10.1007/BF00156098