Fe XXIV d - VERSION 8.0


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

  1. fe_24d.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename: fe_24d.elvlc
    %observed energy levels (below ionization): Sugar, J., Corliss, C., 1979, J.Phys.Chem.Ref.Data, 8, 865
    %observed energy levels (below ionization): Kelly, R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
    %comment: 5s from Kelly
    %Theoretical energy levels: Zhang, H.L., Sampson, D.H., Fontes, C.J., 1990, ADNDT, 44, 31
    %observed energy levels (n=2 above ionization): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175
    %theoretical energy levels (n=2 above ionization): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175
    %theoretical energy levels (n>2 above ionization): calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225
    %Comment: the theoretical energies from Palmeri et al. have been used as experimental ones when the latter were unavailable
    % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    %  E. Landi - Feb 2005
     
    

  3. fe_24d.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: fe_24d.wgfa
    %observed energy levels (below ionization): Sugar, J., Corliss, C., 1979, J.Phys.Chem.Ref.Data, 8, 865
    %observed energy levels (below ionization): Kelly, R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
    %observed energy levels (above ionization, n=2): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175
    %theoretical energy levels (n>2 above ionization): calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225
    %oscillator strengths (below ionization): H.L.Zhang, D.H.Sampson, C.J.Fontes, 1990, ADNDT, 44, 31
    %oscillator strengths (below ionization): Martin,I., Karwowski,J., Diercksen,G.H.F., Barrientos, C., 1993, A&AS, 100, 595
    %A and gf values (above ionization, n=2): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175
    %Autoionization rates (above ionization, n=2): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175
    %A and gf values (above IP, n>2): calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225
    %A and gf values (Transitions between n=2 to 1s2l3l): calculations of Cornille reported in Kato et al., 1997, ADNDT, 67, 225
    %Autoionization rates (above ionization, n>2): calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225
    %comment: Cornille's data for levels 74, 88 have been exchanged with those for levels 88, 153 respectively,
              due to changes in LS coupling notation. The exchange has been based on comparison with autoionization
              and radiative decay rates between Cornille and Safronova's calculations for n=3 to 1s2l3l satellite
              lines (E. Landi, 24 Aug 2004).
    %comment: theoretical energies have been used as experimental values for the dielectronic transitions
    %comment: corrected the wavelengths of dielectronic lines from n=6 levels (Sep 2004)
    % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    %  E. Landi - Sep 2005
    

  5. fe_24d.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    %filename: fe_24d.splups
    %Effective collision strengths and autoionization rates (n=2): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175
    %Effective collision strengths and autoionization rates (n>2): calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    %  E. Landi - Oct 2004
    
    


    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 13:27:18 2015