Fe XII - VERSION 10.1


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

  1. fe_12.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
     
     Experimental energies:
    
    Del Zanna, G. & Mason, H. E. 2005, A&A, 433, 731
    Del Zanna, G. 2012, A&A, 546, A97
    
    Changes in v.9 have been introduced after Wang et al. 2018,  ApJSS 235, 27.
     
    level 21: from the suggestion in Wang et al.,  the 3-21 line being at 248.5 Angstroms
    level 37: the energy 579630, from the 200.356 Ansgstrom line identified by Bromage et al. (1978)
    has been reinstated, following Wang et al.
    
    Note: in v.9 the energies of levels 37,38 were incorrect as the indexing was switched.
    
    
    The identifications of the 3s 3p3 3d levels were uncertain. 
    According to the discussion in Wang et al., the main decay from level 84, to level 6
    is the previously unidentified weak line  at 187.0 Angstroms. The energy 
    of level 84 is then only 522 Kaysers below the predicted energy.  809132.
    Wang et al. suggested that the main transition from level 87, 7-87, is the 
    blended line at 189.12   Angstroms. 
    The 27-50 transition was identified as blending the Fe XII line at 592.6
    
    
    Theoretical energies:
    
    Del Zanna, G., Storey, P. J., Badnell, N. R., & Mason, H. E. 2012, A&A, 543,A139
    Note: the theoretical energies are the 'best energies', i.e. 
    are the empirically-adjusted theoretical energies.
    
    Following Wang et al., 2020, the following 3s2 3p2 4d levels have been modified:
    383 (4D 7/2), 489(4F 7/2),  491(2F 5/2), 503 (2F 7/2), 
    545(2F 5/2), 554 (2D 5/2), 587 (2S 1/2)
    
    Produced for the CHIANTI database v.10 by Giulio Del Zanna  May 2020
    
    
     -1
     
    

  3. fe_12.wgfa (radiative data)
  4. 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.

     
    
    Theoretical energies, gf and A-values:
    
    Del Zanna, G., Storey, P. J., Badnell, N. R., & Mason, H. E. 2012, A&A, 543,A139
    Note: the theoretical energies are the 'best energies', i.e. 
    are the empirically-adjusted theoretical energies.
    
    Experimental energies:
    
    Del Zanna, G. & Mason, H. E. 2005, A&A, 433, 731
    Del Zanna, G. 2012, A&A, 546, A97
    
    Changes in v.9 have been introduced after Wang et al. 2018,  ApJSS 235, 27.
     
    level 21: from the suggestion in Wang et al.,  the 3-21 line being at 248.5 Angstroms
    level 37: the energy 579630, from the 200.356 Ansgstrom line identified by Bromage et al. (1978)
    has been reinstated, following Wang et al.
    
    Note: in v.9 the energies of levels 37,38 were incorrect as the indexing was switched.
    
    
    The identifications of the 3s 3p3 3d levels were uncertain. 
    According to the discussion in Wang et al., the main decay from level 84, to level 6
    is the previously unidentified weak line  at 187.0 Angstroms. The energy 
    of level 84 is then only 522 Kaysers below the predicted energy.  809132.
    Wang et al. suggested that the main transition from level 87, 7-87, is the 
    blended line at 189.12   Angstroms. 
    The 27-50 transition was identified as blending the Fe XII line at 592.6
    
    
    Following Wang et al., 2020, the following 3s2 3p2 4d levels have been modified:
    383 (4D 7/2), 489(4F 7/2),  491(2F 5/2), 503 (2F 7/2), 
    545(2F 5/2), 554 (2D 5/2), 587 (2S 1/2)
    
    Produced for the CHIANTI database v.10 by Giulio Del Zanna  May 2020
    
    
     
    %File processed with wgfa_tidy by pryoung on 31-May-2023
    %File processed with wgfa_tidy by pryoung on 31-May-2023
    

  5. fe_12.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    
    
    Produced for the CHIANTI database v.8 by Giulio Del Zanna  Dec 2013
    
    Del Zanna, G., Storey, P. J., Badnell, N. R., & Mason, H. E. 2012, A&A, 543,A139
    Data from:
    
    

  7. fe_12.psplups (proton collision data)
  8. contains the spline fits to the scaled proton collision strengths.

     
    
    %filename: fe_12.psplups
    %rates: Landman, D.A., 1978, ApJ 220, 366
    %energies: Landman, D.A., 1978, ApJ 220, 366
    %comment: Errors (comparing original rates with those derived from the above 
        splines) are at most 2\% for individual points. For transition 3-4, 
        a good fit could not be found, likely implying errors in the original 
        data values. Errors of up to 4.5\% are found for this transition.
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % Peter Young   7-Jun-2001
    


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

    Page created by Giulio Del Zanna on Mon Jun 26 11:16:41 2023