The optically thick C III spectrum. I - Term populations and multiplet intensities at lower optical depths

Details The optically thick C III spectrum. I - Term populations and multiplet intensities at lower optical depths The optically thick C III spectrum. I - Term populations and multiplet intensities at lower optical depths

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apjs...79..139b&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 79, March 1992, p. 139-156.

Mathematics

Probability

14

Carbon, Electron Density (Concentration), Fine Structure, Line Spectra, Optical Thickness, Solar Spectra, Stellar Spectra, Energy Levels, Forbidden Bands, Iue

Scientific paper

The C III spectrum is studied quantitatively under both optically thin and optically thick conditions, yielding term populations and line/multiplet intensities for column lengths from zero to 10 exp 18/sq cm. The roles of escape probabilities and line profiles in the calculation are discussed in some detail. It is shown that use of the fully integrated escape factor, rather than the more appropriate monodirectional escape probability, can lead to appreciable errors in calculated intensities. The results for populations and intensities make it possible to identify two unassigned features in the solar EUV spectrum of Vernazza and Reeves (1978) as C III multiplets, and to establish that an unidentified infrared solar feature at 8500.32 A, seen in both absorption (Fraunhofer) and emission (chromospheric) spectra, is the C III transition 2s3s(1S)-2s3p(1P). Voigt parameters for the C III lines and multiplets, obtained by a modified semiclassical method are tabulated. A new, unambiguous notation for the numerous line ratios present in a typical spectrum, which is argued to be an improvement over present arbitrary notations, is proposed and used.

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