Ca XVII - VERSION 10.1


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

  1. ca_17.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
     
     Theoretical energies:
    Fernandez-Menchero, Del Zanna and Badnell, A&A, 2014, 566, A104
    doi = {10.1051/0004-6361/201423864}
    
    Note: only the bound levels up to n=5 have been retained
    
    
    observed energy levels (1-5,9,10): Edlen, B. 1983, Physica Scripta, 28, 51
    observed energy levels (6-8): Edlen, B. 1985, Physica Scripta, 32, 86
    observed energy levels (13,15): Fawcett, B.C, Hayes, R.W. 1975, MNRAS, 170, 185
    observed energy levels (27,28,39,41,45): Fawcett, B.C, Hayes, R.W. 1975, MNRAS, 170, 185 and Edlen, B., 1983, Physica Scripta, 28, 51
    observed energy levels (11,18,19,20): McKenzie, D.L., Landecker, P.B. 1982, ApJ, 254, 309 and Edlen, B., 1983, Physica Scripta, 28, 51
    
    Produced as part of the 'CHIANTI' atomic data base collaboration by
    Giulio Del Zanna, May 2020
    
     
     -1
     
    

  3. ca_17.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.

     
    
    gf-values, A-values and theoretical energies:
    Fernandez-Menchero, Del Zanna and Badnell, A&A, 2014, 566, A104
    doi = {10.1051/0004-6361/201423864}
    Only transition probabilities with a branching ratio
    greater than 10^(-5) have been retained.
    
    Note: only the bound levels up to n=5 have been retained
    
    gf-values, A-values for the n=2,3 (lowest 20 levels):
    MBPT calculations by  Wang, K. et al., 2015, ApJS,  218, 16
    doi = {10.1088/0067-0049/218/2/16}
    
    observed energy levels (1-5,9,10): Edlen, B. 1983, Physica Scripta, 28, 51
    observed energy levels (6-8): Edlen, B. 1985, Physica Scripta, 32, 86
    observed energy levels (13,15): Fawcett, B.C, Hayes, R.W. 1975, MNRAS, 170, 185
    observed energy levels (27,28,39,41,45): Fawcett, B.C, Hayes, R.W. 1975, MNRAS, 170, 185 and Edlen, B., 1983, Physica Scripta, 28, 51
    observed energy levels (11,18,19,20): McKenzie, D.L., Landecker, P.B. 1982, ApJ, 254, 309 and Edlen, B., 1983, Physica Scripta, 28, 51
    
    
    Produced as part of the 'CHIANTI' atomic data base collaboration by
    Giulio Del Zanna, May 2020
    
    
    %File processed with wgfa_tidy by pryoung on 31-May-2023
    

  5. ca_17.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    
    
    
    Giulio Del Zanna, May 2020
    Produced as part of the 'CHIANTI' atomic data base collaboration by
    
    Note: only the bound levels up to n=5 have been retained.
    
    doi = {10.1051/0004-6361/201423864}
    Fernandez-Menchero, Del Zanna and Badnell, A&A, 2014, 566, A104
    oscillator strengths and effective collision strengths:
    
    
    

  7. ca_17.psplups (proton collision data)
  8. contains the spline fits to the scaled proton collision strengths.

     
    
    %filename: ca_17.psplups
    %rates: Ryans R.S.I., Foster-Woods V.J, Copeland F., Keenan F.P., Matthews A., Reid R.H.G., 1998, ADNDT 70, 179-229
    %energies: Bhatia A.K., Feldman U., Seely J.F., 1986, ADNDT 35, 449-472
    %comment: Fits valid for temperatures 1e6 to 2e8 K.
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % Peter Young  24-Oct-00
    


    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 11:14:41 2023