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

fe_13.elvlc (energy levels)

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

 
% filename: fe_13.elvlc
%observed energy levels(1-3): Penn & Kuhn, 1994, ApJ, 434, 807
%observed energy levels(6,9- 11,13,15,16,22): Jupen et al., MNRAS, 264, 627, 1993
%observed energy levels(4-5,7-8,12,14,17-21,23-27): NIST Database for Atomic
   Spectroscopy, Version 1.0, NIST Standard Reference Database 61, 1995.
%Theoretical energy levels: Gupta, G.P., Tayal, S.S., 1998, ApJ, 506, 464
%Theoretical energy for level 6: Fawcett & Mason, 1989, ADNDT, 43, 245
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data collaboration
%
% E. Landi 2000
 

fe_13.wgfa (radiative data)

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.

 
%observed energy levels(1-3): Penn & Kuhn, 1994, ApJ, 434, 807
%observed energy levels(6,9- 11,13,15,16,22): Jupen et al., MNRAS, 264, 627, 1993
%observed energy levels(4-5,7-8,12,14,17-21,23-27): NIST Database for Atomic
   Spectroscopy, Version 1.0, NIST Standard Reference Database 61, 1995.
%Theoretical energy levels: Gupta, G.P., Tayal, S.S., 1998, ApJ, 506, 464
% A values: computed from 'superstructure' using a 24 configuration model of Fe XIII.
% comment: the 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: level 18 is metastable, and can decay down to levels
    in the 3s3p^3 and 3s^23p3d configurations via electric quadrupole
    and magnetic dipole transitions. However, the strongest
    transitions are down to the ground configuration via two magnetic
    QUADRUPOLE transitions. These transitions are accurately known
    since the line strength hardly changes when extra configurations
    are added to the model.

% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%   P.R.Young 1999

fe_13.splups (electron collision data)

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_13.splups
%oscillator strengths: SUPERSTRUCTURE calculation (see file fe_13.wgfa for details)
% effective collision strengths: Gupta, G.P., Tayal, S.S., 1998, ApJ, 506, 464
%comment: effective collision strengths were given in the temperature range 5.7 < Log T < 6.7
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Apr 1999

fe_13.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: fe_13.psplups
%rates: Landman D.A., A&A 43, 285, 1975
%energies: Landman D.A., A&A 43, 285, 1975
%comment: Landman tabulates rates between the individual magnetic sublevels of 
    the ground configuration levels. For CHIANTI we sum over these 
    sublevels using Eq. 8 of Landman.
%comment: These fits reproduce the original data to within 2%. The original 
    data cover the temperature range 1e-6 to 3e-6.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   12-Jun-2001

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

fe_13_table.html (html table)


Last revised by G. Del Zanna on 4-Sep-2009