Fe XIII d - VERSION 8.0


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

  1. fe_13d.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename: fe_13d.elvlc
    %observed energy levels (1-3): Penn & Kuhn, 1994, ApJ, 434, 807
    %observed energy levels (6,9- 11,13,15): Jupen et al., MNRAS, 264, 627, 1993
    %observed energy levels (4-5,7-8,12,14): NIST Database for Atomic Spectroscopy, Version 1.0, 
         NIST Standard Reference Database 61, 1995.
    %observed energy levels (16-58): Mendoza, C., Kallman, T.R., Bautista, M.A., Palmeri, P., 2004, A&A, 414, 377
    %Theoretical energy levels (1- 15): Gupta, G.P., Tayal, S.S., 1998, ApJ, 506, 464
    %Theoretical energy for level 6: Fawcett & Mason, 1989, ADNDT, 43, 245
    %Theoretical energy levels (16- 58): Mendoza, C., Kallman, T.R., Bautista, M.A., Palmeri, P., 2004, A&A, 414, 377
    %Comment: the theoretical energies from Mendoza et al have been used as experimental ones
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data collaboration
    %
    % E. Landi - Jan 2005
     
    

  3. fe_13d.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_13d.wgfa
    %observed energy levels (1-3): Penn & Kuhn, 1994, ApJ, 434, 807
    %observed energy levels (6,9- 11,13,15): Jupen et al., MNRAS, 264, 627, 1993
    %observed energy levels (4-5,7-8,12,14): NIST Database for Atomic Spectroscopy, Version 1.0,
         NIST Standard Reference Database 61, 1995.
    %observed energy levels (16-58): Mendoza, C., Kallman, T.R., Bautista, M.A., Palmeri, P., 2004, A&A, 414, 377
    % A values (levels 1- 15): computed from 'superstructure' using a 24 configuration model for Fe XIII.
    % A values (levels above ionization): Mendoza, C., Kallman, T.R., Bautista, M.A., Palmeri, P., 2004, A&A, 414, 377
    %Autoionization rates: Mendoza, C., Kallman, T.R., Bautista, M.A., Palmeri, P., 2004, A&A, 414, 377
    % comment: the superstructure model of Fe XIII included the following configurations:
        3s2 {3p2 3p3d 3d2}
        3s23p {4s 4p 4d 4f}
        3s3p2 {3d 4s 4p 4d 4f}
        3p3 {3d 4s 4p 4d}
        3s3d {4s 4p 4d 4f}
        3p4
        3s {3p3 3d3 3p3d2}
    %comment: A values for levels 16 to 48 are a fix
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data collaboration
    %
    % E. Landi - Jan 2005
    

  5. fe_13d.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    %filename: fe_13d.splups
    %Effective collision strengths and autoionization rates: Mendoza, C., Kallman, T.R., Bautista, M.A., Palmeri, P., 2004, A&A, 414, 377
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    %  E. Landi - Sep 2005
    
    


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

    fe_13d_table.html (html table)

    Page created by Giulio Del Zanna on Fri Sep 18 13:26:46 2015