Benchmarking atomic data for astrophysics: Fe XXIII

Details Benchmarking atomic data for astrophysics: Fe XXIII Benchmarking atomic data for astrophysics: Fe XXIII

Mar 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...432.1137d&link_type=abstract

Astronomy and Astrophysics, Volume 432, Issue 3, March IV 2005, pp.1137-1150

Astronomy and Astrophysics

Astrophysics

11

Atomic Data, Line: Identification, Sun: Corona, Techniques: Spectroscopic

Scientific paper

Recent scattering calculations for Fe XXIII are benchmarked against laboratory and astrophysical observations. The collisional data are supplemented by radiative data obtained with empirical adjustments that take into account observed wavelengths. All previous line identifications and energy levels are reviewed and assessed in light of these new calculations. Most of the previous identifications, in particular of the astrophysically-important spectral lines are confirmed. However, some identification are rejected or questioned, and new ones proposed. The agreement between theoretical and experimental data in terms of wavelengths, line intensities and level lifetimes is very good. Observations of Fe XXIII L-shell emission lines provide a great opportunity to directly measure electron temperatures for a wide range of astrophysical sources. Examples from solar (SMM, SOLEX) and stellar (Chandra, EUVE) observations are provided.
The full set of energies (cf. Table 2), wavelengths and A-values (cf. Table 3) are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/432/1137 .

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