Abstract
Observations of the Ca ii H, K, and infrared triplet lines are compared with theoretical predictions from the slab models of Heasley and Milkey (1976). While the theoretical models describe the hydrogen and helium emission spectra of quiescent prominences satisfactorily the predicted Ca ii lines are systematically too bright. The most likely reason for the discrepancy is the inapplicability of the symmetric slab prominence model for lines which become even moderately optically thick in prominences.
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Operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.
Visiting scientist at Kitt Peak National Observatory.
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Heasley, J.N., Milkey, R.W. & Engvold, O. The Ca ii emission lines in quiescent prominences. Sol Phys 51, 315–320 (1977). https://doi.org/10.1007/BF00216369
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DOI: https://doi.org/10.1007/BF00216369