The CA II emission lines in quiescent prominences

Details The CA II emission lines in quiescent prominences The CA II emission lines in quiescent prominences

Mar 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977soph...51..315h&link_type=abstract

Solar Physics, vol. 51, Mar. 1977, p. 315-320.

Physics

9

Calcium, Emission Spectra, Solar Prominences, Solar Spectra, Metal Ions, Optical Thickness, Stellar Models

Scientific paper

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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