Fe XI - VERSION 8.0


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

  1. fe_11.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. 2010, A&A, 514, A41
    Del Zanna, G. 2012, A&A, 546, A97
    
    Theoretical energies:
    Del Zanna, G., Storey, P.J., 2013,  A&A, 549, A42
    
    Note: the theoretical energies are the 'best energies', i.e. 
    are the empirically-adjusted theoretical energies.
    
    
    
     -1
     
    

  3. fe_11.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.

     
    
    Experimental energies:
    Del Zanna, G. 2010, A&A, 514, A41+
    Del Zanna, G. 2012, A&A, 546, A97
    
    
    Theoretical energies, gf and A-values:
    Del Zanna, G., Storey, P.J., 2013,  A&A, 549, A42
    
    Note: the theoretical energies are the 'best energies', i.e. 
    are the empirically-adjusted theoretical energies.
    
    Only transitions with a branching ratio of 10^-5 have been retained.
    
    For transitions from levels 37,41,43:
    Del Zanna, G., Storey, P. J., & Mason, H. E. 2010, A&A, 514, A40+
    
    Produced for the CHIANTI database v.8 by Giulio Del Zanna  26 Jun 2013
     
    
    

  5. fe_11.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    
    Data from:
    Del Zanna, G., Storey, P.J., 2013,  A&A, 549, A42
    
    For transitions from levels 37,39,41:
    Del Zanna, G., Storey, P. J., & Mason, H. E. 2010, A&A, 514, A40+
    
    
    
    

  7. fe_11.psplups (proton collision data)
  8. contains the spline fits to the scaled proton collision strengths.

     
    
    %filename: fe_11.psplups
    %rates: Landman, D.A., ApJ 240, 709, 1980
    %energies: Observed energies from CHIANTI .elvlc file
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % Peter Young   13-Jun-2001
    


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

    Page created by Giulio Del Zanna on Fri Sep 18 13:26:19 2015