The Fe XIV spectrum: Predicted line intensities and solar identifications

Details The Fe XIV spectrum: Predicted line intensities and solar identifications The Fe XIV spectrum: Predicted line intensities and solar identifications

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...427..497b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 427, no. 1, p. 497-510

Other

13

Data Processing, Photoluminescent Bands, Resonance Lines, Solar Corona, Solar Spectra, Ultraviolet Radiation, Electron Density (Concentration), Emission Spectra, High Dispersion Spectrographs, Luminous Intensity, Skylab Program, Wavelengths

Scientific paper

Level populations and line intensities have been calculated in a 40-level model of Fe XIV which includes the configuations 3p3 and 3s3p3d. The results have been compared against intensities of weaker, unidentified, or tentatively classified lines in published solar line lists including a recent Goddard Space Flight Center/Solar Extreme Ultraviolet Telescope and Spectrograph (GSFC/SERTS) high-resolution list, and in presently measured archival Naval Research Laboratory (NRL)/S082A active region spectra. Seven new lines are identified as Fe XIV transitions; five other observed, unidentified lines are considered to be Fe XIV transitions on the basis of wavelength coincidence, but require further observations to obtain photometric intensities for verification; one line at 216.93 A is shown to be due to some other ion than Fe XIV. In addition, a unique forbidden infrared (approx. equal to 1.25 micrometer(s)) line originating in the high metastable level 3s3p3d(F9/2-4) is found to have an unusual intensity dependence on electron density.

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