Discrepancies between calculated and observed Fe XVII and NI XIX solar coronal lines

Details Discrepancies between calculated and observed Fe XVII and NI XIX solar coronal lines Discrepancies between calculated and observed Fe XVII and NI XIX solar coronal lines

Dec 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ap%26ss..38..365l&link_type=abstract

(International Astronomical Union, Colloquium on UV and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas, Cambridge, M

Astronomy and Astrophysics

Astrophysics

2

Iron, Nickel, Solar Corona, Solar Spectra, Atomic Energy Levels, Electron Density (Concentration), Line Spectra

Scientific paper

The 36-level model atom Fe(16+) of Loulergue and Nussbaumer (1973) is extended to a 51-level atom including the n 4 configuration. The earlier conclusion still holds that relative intensities among the Fe XV I lines are not sufficiently sensitive to variations in electron density and electron temperature to deduce these parameters from observed intensity ratios. Discrepancies between calculated and observed relative intensities in Fe XVII and Ni XIX are attributed to blends or misidentifications.

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