Fe XXI - VERSION 10.1


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

  1. fe_21.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    
    Observed energy levels as in CHIANTI v.9:
    
    levels (2,4): Feldman, U., Curdt, W., Landi, E., Wilhelm, K., 2000, ApJ, 544, 508
    
    levels (3,5 to 21): Feldman, U., Curdt, W., Landi, E., Wilhelm, K., 2000, ApJ, 544, 508 and
      Fuhr, J.R., et al., "NIST Atomic Spectra Database" Ver. 2.0, March 1999, NIST Physical Reference Data
    
    levels (28,37,38,39,40,42,46,49,58,60, 84,144,149): Brown et al., 2002, ApJS, 140, 589
    
    levels (56,74,81,461): Fuhr, J.R., et al., "NIST Atomic Spectra Database" Ver. 2.0,
               March 1999, NIST Physical Reference Data
    
    levels (246,247,248,261,266,410,462): Fawcett et al, 1987, MNRAS, 225, 1013
    
    levels (22,35,73, 87, 276,297, 385, 408,409,457):
    From  Landi & Phillips, 2005, ApJS, 160, 286
    
    
    levels (above ionization): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175
    
    Theoretical energy levels (below ionization):
    Mao, J. , Badnell, N. R., Del Zanna, G., 2020, A&A, 634, A7
    DOI:  10.1051/0004-6361/201936931 
    
    
    Theoretical energy levels and A-values for auto-ionizing states
    as in v.9 (K. Dere January 2018) 
    A Breit-Pauli distorted wave implementation for AUTOSTRUCTURE
    Badnell, N.R., 2011, Computer Physics Communications, 182, 1528
    ADSref:  http://adsabs.harvard.edu/abs/2011CoPhC.182.1528B
    
    Autostructure calculation optimized with 'SHFTIC' file using energy corrections from the following sources:
    
    Observed energy levels:  Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/asd [2012, September 14]. National Institute of Standards and Technology, Gaithersburg, MD.
    
    energy levels 592 and 595
    Rudolph, J. K.; Bernitt, S.; Epp, S. W.; Steinbrugge, R.; Beilmann, C.; Brown, G. V.; Eberle, S.; Graf, A.; Harman, Z.; Hell, N.; Leutenegger, M.; Mueller, A.; Schlage, K.; Wille, H.-C.; Yavas, H.; Ullrich, J.; Crespo Lopez-Urrutia, J. R.
    X-Ray Resonant Photoexcitation: Linewidths and Energies of K-alpha Transitions in Highly Charged Fe Ions
    Physical Review Letters, vol. 111, Issue 10, id. 103002
    DOI:  10.1103/PhysRevLett.111.103002
    adsRef:  http://adsabs.harvard.edu/abs/2013PhRvL.111j3002R
    
    levels 596 and 597 switched to agree with V8 data
    
    
    Produced as part of the 'CHIANTI' atomic data base collaboration by
    Giulio Del Zanna, Aug 2020
    
    
     
     -1
     
    

  3. fe_21.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.

     
    
    
    gf-values, A-values and theoretical energies:
    
    Mao, J. , Badnell, N. R., Del Zanna, G., 2020, A&A, 634, A7
    DOI:  10.1051/0004-6361/201936931 
    
    Only transition probabilities with a branching ratio
    greater than 10^(-5) have been retained.
    
    
    %Radiative data (above ionization) as in v.9:
    Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175
    
    
    Observed energies: see energy file.
    
    
    Produced as part of the 'CHIANTI' atomic data base collaboration by
    Giulio Del Zanna, Aug 2020
    
    
    %File processed with wgfa_tidy by pryoung on 31-May-2023
    

  5. fe_21.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    
    
    
    Giulio Del Zanna, Aug 2020
    Produced as part of the 'CHIANTI' atomic data base collaboration by
    
    
    Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171
    collisional data (above ionization) as in v.9:
    
    DOI:  10.1051/0004-6361/201936931 
    Mao, J. , Badnell, N. R., Del Zanna, G., 2020, A&A, 634, A7
    
    oscillator strengths and effective collision strengths:
    
    

  7. fe_21.psplups (proton collision data)
  8. contains the spline fits to the scaled proton collision strengths.

     
    
    %filename: fe_21.psplups
    %rates: Ryans R.S.I., Foster-Woods V.J, Keenan F.P., Reid R.H.G., 1999, ADNDT 73, 1-42
    %energies: CHIANTI database, ver.1, Dere et al., A&AS 125, 149, 1997
    %comment: Fits valid for temperatures 1.5e6 to 1.5e8 K.
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % Peter Young   10-Sep-2002
    

  9. fe_21.cilvl (collisional ionization population rates)
  10.  
    %filename: fe_21.cilvl
    %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 Mon Jun 26 11:16:04 2023