Fe VIII - VERSION 5.1

The CHIANTI database consists of 4 primary ASCII files for each ion in the database.

• fe_8.elvlc (energy levels)

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

  References:

  %Experimental energy levels: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1999,
      NIST Database for Atomic Spectroscopy, Version 2.0, NIST Standard Reference Database 61
  %Experimental energy levels (3p6.4d levels - 51,52): Ekberg, J.O. & Feldman U., 2003, ApJ, 595, 517
  %theoretical energy levels: Griffin, D.C., Pindzola, M.S., Badnell, N.R., 2000, A&ASS, 142, 317
  %theoretical energy levels n=5,6,7: Czyzak,S.J., Krueger,T.K., 1966, ApJ, 144, 381
  %Comment: Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8 report
            an inversion of energies between levels 70 and 72 (same J). For consistency with Griffin 
            et al 2000, who adapted their atomic structure calculation to a set of observed energies
            identical to the NIST one, we use the NIST v.2 level ordering.
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % E.Landi - Nov 2004
  

  
  

• fe_8.wgfa (radiative data)

  contains wavelengths, gf and A values for each transition. Wavelengths are based on experimental level energies where available; wavelengths calculated from theoretical energies are less accurate and are given as negative values.

  References:

  %Experimental energy levels: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1999,
        NIST Database for Atomic Spectroscopy, Version 2.0, NIST Standard Reference Database 61.
  %Experimental energy levels (3p6.4d levels - 51,52): Ekberg, J.O. & Feldman U., 2003, ApJ, 595, 517
  %theoretical energy levels: Griffin, D.C., Pindzola, M.S., Badnell, N.R., 2000, A&ASS, 142, 317
  %Comment: Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8 report
            an inversion of energies between levels 70 and 72 (ssame J). For consistency with Griffin 
            et al 2000, who adapted their atomic structure calculation to a set of observed energies
            identical to the NIST v.2 one, we use the NIST v.2 level ordering.
  %Radiative data: Griffin, D.C., Pindzola, M.S., Badnell, N.R., 2000, A&ASS, 142, 317
  %Radiative data n=5,6,7: Czyzak,S.J., Krueger,T.K., 1966, ApJ, 144, 381
  %Radiative data 1 - 2 transition: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1999,
        NIST Database for Atomic Spectroscopy, Version 2.0, NIST Standard Reference Database 61
  %Radiative data for levels with J=9/2, 11/2: calculated using SUPERSTRUCTURE, with the configurations
                 3s2.3p6.3d, 3s2.3p5.3d2, 3s2.3p5.3d.4s, 3s2.3p6.4s, 3s2.3p6.4p, 3s2.3p6.4d, 3s2.3p6.4f,
                 3s2.3p4.3d3, 3s2.3p3.3d4
  %comment: SUPERSTRUCTURE radiative data have been corrected for the differences between experimental
            and SUPERSTRUCTURE transition wavelength differences, where experimental values were available.
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % E.Landi - Nov 2004
  

  
  

• fe_8.splups (electron collision data)

  contains the spline fits to the electron collision strengths scaled according to 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.

  References:

  
  %filename: fe_8.splups
  %Oscillator strengths: Griffin, D.C., Pindzola, M.S., Badnell, N.R., 2000, A&ASS, 142, 317
  %Effective collision strengths: Griffin, D.C., Pindzola, M.S., Badnell, N.R., 2000, A&ASS, 142, 317
  %collision strengths and gf values n=5,6,7:  Czyzak,S.J., Krueger,T.K., 1966, ApJ, 144, 381
  %comment: effective collision strengths were provided in the temperature range 4.5 < Log T < 6.5
  %comment: added collisional data for transitions involving levels 21,25,28,29,39. They affect
            level populations at electron densities larger than 10^9 cm^-3 (June 2003).
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  % 
  % Enrico Landi - June 2003
  

  
  

• fe_8.psplups (electron collision data) - Not Present in CHIANTI 5.1

  contains the spline fits to the scaled proton collision strengths.
  

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

  
  

• fe_8_table.html (html table)