Fe VII - VERSION 11.0.1

The CHIANTI database has the following primary ASCII files for this ion:

  1. fe_7.elvlc (energy levels)

    2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies. 

     
%Prepared for the CHIANTI database by Peter Young
%File:  fe_7.elvlc
%Observed energy levels:
   Kramida, A., Ryabtsev, A. N. & Young, P. R., ApJS, 258, 37
%Theoretical energy levels:
   Y. Li et al., 2018, MNRAS, 479, 1260
   S. Tayal & O. Zatsarinny, 2014, ApJ, 788, 24
%Comment
   Not all of the Kramida energies have been added to the model. A separate document
   lists the levels that were omitted - see the CHIANTI 10.1 paper.

   Theoretical energy levels are mostly taken from Li et al. as these are more accurate
   than the values of Tayal & Zatsarinny. Li only provided values for 134 levels,
   however.

   The theoretical energies for levels 25-27 & 29 (5G levels) have been adjusted using
   the new 5G2 energy from Kramida et al. (2022).
%Parent terms for 3p5 3d3 levels
   Terms for the 3p5 3d3 are derived by combining terms from the 3p5 and 3d3 subshells,
   and so the parent terms are written as, e.g., 3p5(2P) 3d3(2G) for the 1H5 level. 
   Since 3p5 only gives rise to one term (2P), then I drop (2P) from the configuration
   description, leaving just 3p5 3d3(2G).

   Parent terms were not provided in the Witthoeft & Badnell (2008), but P.R. Young
   has run AUTOSTRUCTURE for Fe VII to derive the parent terms for all levels. Note
   that there are two 2D parent terms that are distinguished by "a" and "b"; our
   labelling follows that of Ekberg (1981, Phys. Scripta, 23, 7).

   Some of the parent terms were modified to match the Kramida et al. data.

  2. fe_7.wgfa (radiative data)

    3. contains wavelengths, gf and A values of the transitions. The wavelengths are based on the experimental energy levels and should be the best available. Wavelengths calculated from the theoretical energies are of an indeterminate accuracy and their values are presented as negative values of the calculated wavelength. 

     
%Prepared for the CHIANTI database by Peter Young
%File:  fe_7.wgfa
%A-values:
   Tayal & Zatsarinny, 2014, ApJ, 788, 24
   Y. Li et al., 2018, MNRAS, 479, 1260
   Witthoeft & Badnell, 2008, A&A, 481, 543
%Wavelengths:
   Derived from energies in the CHIANTI elvlc file.
%Comment:
   Tayal & Zatsarinny only gave A-values for allowed transitions, so forbidden transitions
   were taken from Li et al. (2018) and, if necessary, Witthoeft & Badnell.
%File processed with wgfa_tidy by pryoung on  3-Apr-2023
%File processed with wgfa_tidy by pryoung on 31-May-2023
%File processed with wgfa_tidy by pryoung on 31-May-2023

  3. fe_7.scups (electron collision data)

    4. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992). 

     
   Tayal & Zatsarinny, 2014, ApJ, 788, 24        
%Oscillator strengths:                           
   Tayal & Zatsarinny, 2014, ApJ, 788, 24        
%Theoretical energies:                           
   Tayal & Zatsarinny, 2014, ApJ, 788, 24        
%Upsilons:                                       
%Prepared for the CHIANTI database by Peter Young
%File:  fe_7.scups

  4. (proton collisional data) Not available in this VERSION.

    5. The html tables below contain the radiative data of the brightest lines sorted in wavelength

    Page created by Giulio Del Zanna on Wed Apr 16 17:43:16 2025