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The CHIANTI database consists of the following primary ASCII files for this ion:
contains the energy levels in cm^(-1) It includes both experimental and theoretical values of the levels energies.
%observed energy levels (1-24): Del Zanna, 2006, A&A, 447, 761 %Theoretical energy levels (1-24): Whiteford et al., 2002, J.Phys.B, 35, 3729 %observed energy levels (above ionization: 25,26,29,30,32,36,38-40): Shirai,T. et al., 2000, J.Phys.Chem.Ref.Data, Monograph 8 %Theoretical energy levels (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2003, A&A, 403, 339 %comment: theoretical energies for levels 27,28,31,33-35,37 have been used as experimental energies %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % G. Del Zanna and E. Landi - Jun 27, 2005
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_24.wgfa %observed energy levels (1-24): Del Zanna, 2006, A&A, 447, 761 %Theoretical energy levels (1-24): Whiteford et al., 2002, J.Phys.B, 35, 3729 %observed energy levels (25,26,29,30,32,36,38-40): Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8 %Theoretical energy levels (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2003, A&A, 403, 339 %comment: theoretical energies for levels 27,28,31,33-35,37 have been used as experimental energies %Radiative data (1-24): Whiteford et al., 2002, J.Phys.B, 35, 3729 %Radiative data (above ionization): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175 %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % G. Del Zanna and E. Landi - Jun 27, 2005
contains the spline fits to the electron collision strengths scaled according the rules formulated by Burgess and Tully (1992). Accurate replication of the temperature averaged collision strength over a wide range of temperatures can be accomplished with the data in this file.
% filename: fe_24.splups
%Oscillator strengths (1-15): Berrington and Tully 1997, A&AS, 126, 105
%Oscillator strengths (16-24): Whiteford et al., 2002, J.Phys.B, 35, 3729
%gf values (above ionization): Palmeri, P., Mendoza, C., Kallman, T.R., Bautista, M.A., 2003, A&A, 403, 1175
%Effective collision strengths (1-15): Berrington and Tully 1997, A&AS, 126, 105
%Effective collision strengths (16-24): Whiteford et al., 2002, J.Phys.B, 35, 3729
%collisional data (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171
%comment: rate coefficients are to be considered valid in the 1.6x10^6 -- 10^8 K temperature range.
%comment: Only the excitations from the first 3 levels are retained here.
These are sufficient up to high (10^{19} cm-3) electron densities, since these are the levels mostly populated
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% G. Del Zanna and E. Landi - Jun 27, 2005
%filename: fe_24.rec %Total recombination population rate: Gu, M.F., 2003, ApJ, 582, 1241 %produced as part of the Arcetri/Cambridge/NRL CHIANTI atomic data base collaboration % % Enrico Landi - Feb 2004
%filename: fe_24.ci %Collisional ionization population rate: Gu, M.F., 2003, ApJ, 582, 1241 %produced as part of the Arcetri/Cambridge/NRL CHIANTI atomic data base collaboration % % Enrico Landi - Feb 2004