C VI - VERSION 10.1


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

  1. c_6.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename: c_6.elvlc
    %observed energy levels: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995, 
       NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61.
    %comment:     3952061.52    Limit
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration CHIANTI
    %
    % K.P.Dere 1999
    -1
     
    

  3. c_6.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.

     
    %filename:  /data2/svn/chianti/dbase/trunk/c/c_6/c_6.wgfa
    %filename: c_6.wgfa
    %observed energy levels: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995,
    NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61.
    %A values (transition 1-2): Parpia, F.A., Johnson, W.R., 1982, Phys.Rev.A, 26, 1142.
    %Radiative data: SUPERSTRUCTURE calculation including all levels up to n=5.
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    %  Giulio Del Zanna  -  May 2006
    % edited wavelengths at line 68 to provide a space between the wavelength and the level2 numbers
    % K Dere 7 oct 2015
    
     minimum branching ratio =   1.00e-05
    K. Dere  2017 December 06
    %File processed with wgfa_tidy by pryoung on  6-Mar-2019
    %File processed with wgfa_tidy by pryoung on 31-May-2023
    

  5. c_6.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    %   G. Del Zanna  -  Nov  2007
    %
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %comment: Only excitations from the 1s and 2s levels are retained from the original dataset.
              to statistical weights.
    %comment: The fine structure collision strengths have been obtained assuming a distribution according 
    %comment: fine-structure values for electron impact-excitation within the n=2 levels from Zygelman & Dalgarno (1987) Phys. Rev. A, 35, 4085 
    %effective collision strengths: Ballance, Badnell, & Smith 2003, J. Phys. B, 36, 3707
    %oscillator strengths: SUPERSTRUCTURE calculation including all levels up to n=5.
    %filename: c_6.splups
    

  7. c_6.psplups (proton collision data)
  8. contains the spline fits to the scaled proton collision strengths.

     
    
    %file: c_6.psplups
    %prepared for the CHIANTI database by Peter Young on 28-Feb-2023
    %Energies:
       Zygelman, B. & Dalgarno, A., 1987, Phys. Rev. A, 35, 4085
    %Proton rate coefficients:
       Zygelman, B. & Dalgarno, A., 1987, Phys. Rev. A, 35, 4085
    

  9. c_6.reclvl (total recombination population rates)
  10.  
    %filename: c_6.reclvl
    %Radiative recombination rates: Mewe, R, Gronenschild, E.H.B.M, and van den Oord, G.H.J, 1982, A&AS, 62, 197
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % E. Landi - Aug 2006
    


    The html table below contains the radiative data of the brightest lines sorted in wavelength

    c_6_table.html (html table)

    Page created by Giulio Del Zanna on Mon Jun 26 11:14:40 2023