Fe XVIII - VERSION 8.0


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

  1. fe_18.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename: fe_18.elvlc
    %Observed energies (levels up to n=4):D el Zanna,G . 2006, Astron. Astroph. 459, 307
    %Observed energies (n=5 levels): Landi &P hillips 2005, ApJS, 160, 286 
    %Observed energy level above ionization:P almeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175
    %Theoretical energies (levels up to n=4): Witthoeft, M.C., Badnell, N.R.,D el Zanna,G ., Berrington, K.A., andP elan, J.C. 2006, Astron. Astroph. 446, 361
    %Theoretical energies (n=5 levels): Landi &G u, 2006, ApJ, 640, 1171
    % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    %    G. Del Zanna and Enrico Landi -  Oct 2008 
     
    

  3. fe_18.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_18.wgfa
    %Observed energies (levels up to n=4): Del Zanna, G. 2006, Astron. Astroph. 459, 307
    %Observed energies (n=5 levels): Landi & Phillips 2005, ApJS, 160, 286
    %Theoretical energies (levels up to n=4): Witthoeft, M.C., Badnell, N.R., Del Zanna, G., Berrington, K.A., and Pelan, J.C. 2006, Astron. Astroph. 446, 361
    %Theoretical energies (n=5 levels): Landi & Gu, 2006, ApJ, 640, 1171
    %observed energy level above ionization: Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175
    %A-values (levels up to n=4): Del Zanna, G.: 2006, Astron. Astroph. 459, 307
    %A-values (n=5 levels): Landi & Gu, 2006, ApJ, 640, 1171
    %Autoionization rate: 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  -  Oct 2008
    

  5. fe_18.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    %filename: fe_18.splups
    %oscillator strengths (levels up to n=4): Witthoeft, M.C., Badnell, N.R., Del Zanna, G., Berrington, K.A., and Pelan, J.C., 2006, Astron. Astroph. 446, 361
    %oscillator strengths (n=5 levels): Landi & Gu, 2006, ApJ, 640, 1171
    %oscillator strengths (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171
    %effective collision strengths (levels up to n=4): Witthoeft, M.C., Badnell, N.R., Del Zanna, G., Berrington, K.A., and Pelan, J.C. 2006, Astron. Astroph. 446, 361.
    %collision strengths (n=5 levels): Landi & Gu, 2006, ApJ, 640, 1171
    %effective collision strengths (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171
    %comment: only excitations from the lowest three levels to the n=4 states are retained.
    %comment: effective collision strengths for levels above ionization are given in the range 6.46e4 < T < 1.62e7
    % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    %   G. Del Zanna  -  Oct 2008
    
    

  7. fe_18.psplups (proton collision data)
  8. contains the spline fits to the scaled proton collision strengths.

     
    
    %filename: fe_18.psplups
    %rates: Foster V.J, Keenan F.P., Reid R.H.G., 1994, Phys. Rev. A 49, 3092-3095
    %energies: Reader J., Sugar J., 1975, J.Phys.Chem.Ref.Data 4, 353
    %comment: Fit valid for temperatures 2e6 to 2.5e8 K.
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % Peter Young   16-May-2001
    

  9. fe_18.reclvl (total recombination population rates)
  10.  
    %filename: fe_18.rec
    %Total recombination population rate: Gu, M.F., 2003, ApJ, 582, 1241
    %comment: level indexing was modified on 10 Dec 2007
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % Enrico Landi and Giulio Del Zanna - 10 Dec 2007
    

  11. fe_18.cilvl (collisional ionization population rates)
  12.  
    %filename: fe_18.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
    


    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 13:27:00 2015