Fe XIV - VERSION 10.1

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

  1. fe_14.elvlc (energy levels)

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

     
%filename: fe_14.elvlc
%Observed energies (1-197): reassessed from original measurements -- see comments below
%Observed energies (122, 125, 136): Del Zanna 2012, A&A, in press
%Theoretical energy levels (1-197): Liang et al. 2010, ApJS, 190, 322
%Theoretical energy levels (198-739): Landi & Dere 2012. ADNDT, submitted
%Comment: the wavelengths from  Churilov,S.S. Levashov,V.E., 1993 Physica Scripta 48, 425  
          were adopted for most transitions. A few added wavelengths are from
          Shirai, T., Sugar, J., Musgrove, A., & Wiese, W. L. 2000, J. Phys. Chem. Ref. Data, Monograph 8
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Enrico Landi and Giulio del Zanna - Sep 25, 2012

  2. fe_14.wgfa (radiative data)

    3. 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_14.wgfa
%Observed energies (1-197): reassessed from original measurements -- see comments below
%Observed energies (122, 125, 136): Del Zanna 2012, A&A, in press
%Theoretical energy levels (1-197): Liang et al. 2010, ApJS, 190, 322
%Theoretical energy levels (198-739): Landi & Dere 2012
%A and gf values (1-197): Liang et al. 2010, ApJS, 190, 322
%A and gf values (198-739): Landi & Dere 2012
%Comment: the wavelengths from  Churilov,S.S. Levashov,V.E., 1993 Physica Scripta 48, 425
          were adopted for most transitions. A few added wavelengths are from
          Shirai, T., Sugar, J., Musgrove, A., & Wiese, W. L. 2000, J. Phys. Chem. Ref. Data, Monograph 8
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%   Enrico Landi and Giulio Del Zanna, Sep 25, 2012
%File processed with wgfa_tidy by pryoung on  6-Mar-2019
%File processed with wgfa_tidy by pryoung on  6-Mar-2019
%File processed with wgfa_tidy by pryoung on 31-May-2023
%File processed with wgfa_tidy by pryoung on 31-May-2023

  3. fe_14.scups (electron collision data)

    4. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992). 

     
%   Enrico Landi and Giulio Del Zanna, Jan 2011
%
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
          the data was such that only the data between 10$^5$ and 10$^7$ K could be fitted.
%comment: The Liang et al. (2010) were fitted with 9-point splines, however the structure of 
%Collision strengths (levels 198-739): Landi & Dere, 2012, ADNDT, submitted
%Oscillator strengths (levels 198-739): Landi & Dere, 2012, ADNDT, submitted
%Effective collision strengths (levels 1-197): Liang et al. 2010, ApJS, 190, 322
%Oscillator strengths (levels 1-197): Liang et al. 2010, ApJS, 190, 322
%filename: fe_14.splups

  4. fe_14.psplups (proton collision data)

    5. contains the spline fits to the scaled proton collision strengths. 

     

%filename: fe_14.psplups
%rates: J. Tully, private communication, Nov. 2001
%energies: Observed value from .elvlc file.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   17-Jan-2002

    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 11:16:25 2023