Fe XXII - VERSION 10.0.2


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

  1. fe_22.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename:  fe_22.elvlc
    
    Theoretical energy levels:  Autostructure calculation
    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.
    
    
    %experimental energies 518, 519:
    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
    
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2017 December 29
    
    %comment: Fixed text problem in comments. No change to data.  Peter Young, 25-Jul-2019
     
    

  3. fe_22.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_22.wgfa.e1e2.imp5
    Theoretical wavelengths, gf, A-values:  Autostructure calculation
    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.
    
    %experimental energies 518, 519:
    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 Lóopez-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
    
    Observed wavelength 1-2:
    Feldman, U.; Curdt, W.; Landi, E.; Wilhelm, K.
    Identification of Spectral Lines in the 500-1600 Å Wavelength Range of Highly Ionized Ne, Na, Mg, Ar, K, Ca, Ti, Cr, Mn, Fe, Co, and Ni
    Emitted by Flares (Te>=3×106 K) and Their Potential Use in Plasma Diagnostics
    2000ApJ...544..508F
    adsRef:  http://adsabs.harvard.edu/abs/2000ApJ...544..508F
    DOI:  	10.1086/317203
    
    sorted by lvl12
    
     elvlcName = fe_22.elvlc
     wgfaName = fe22.wgfa.e1e2.sorted
     allWvl =   1
     minDiff =      0.00010
     wavelengths determined from energy levels
    
     produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2019 February 07
     minimum branching ratio =   1.00e-04
    2019 February 07
    %File processed with wgfa_tidy by pryoung on  6-Mar-2019
    
    %comment: Fixed text problem in comments. No change to data.  Peter Young, 25-Jul-2019
    

  5. fe_22.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    %comment: Fixed text problem in comments. No change to data.  Peter Young, 25-Jul-2019
    
    fe_23 IP ev =  1.95858e+03 Ip invcm =    15797000.000 Ip Ryd =     143.95285
    fe_22 IP ev =  1.79901e+03 Ip invcm =    14510000.000 Ip Ryd =     132.22485
    K. Dere (GMU) - 2017 December 29
    adsRef:  http://adsabs.harvard.edu/abs/2013PhRvL.111j3002R
    
    DOI:  10.1103/PhysRevLett.111.103002
    Physical Review Letters, vol. 111, Issue 10, id. 103002
    X-Ray Resonant Photoexcitation: Linewidths and Energies of K-alpha Transitions in Highly Charged Fe Ions
    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 Lóopez-Urrutia, J. R.
    %experimental energies 518, 519:
    
    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.
    
    Autostructure calculation optimized with 'SHFTIC' file using energy corrections from the following sources:
    
    ADSref:  http://adsabs.harvard.edu/abs/2011CoPhC.182.1528B
    Badnell, N.R., 2011, Computer Physics Communications, 182, 1528
    A Breit-Pauli distorted wave implementation for AUTOSTRUCTURE
    Theoretical energy levels:  Autostructure calculation
    2018 December 10
     levels renumbered by K. Dere
    
    % Enrico Landi - Mar 2005
    %
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %comment: data from Badnell & Griffin have been adapted to the level ordering given by the Flexible Atomic Code
    %comment: effective collision strengths from Badnell et al. (2001) are used in the temperature range 6.4 < Log T < 8.0
    %collisional data (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171
    %Collision strengths (205-513): Landi & Gu, 2006, ApJ, 640, 1171
    %effective collision strengths (1-204): Badnell, N.R., Griffin, D.C., Mitnik, D.M., 2001, J.Phys.B, 34, 5071
    %oscillator strengths (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171
    %oscillator strengths (205-513): Landi & Gu, 2006, ApJ, 640, 1171
    %oscillator strengths (1-204): Badnell, N.R., Griffin, D.C., Mitnik, D.M., 2001, J.Phys.B, 34, 5071
    %filename: fe_22.splups
    filename fe_22.scups_rnmbr 
    

  7. fe_22.psplups (proton collision data)
  8. contains the spline fits to the scaled proton collision strengths.

     
    
    %filename: fe_22.psplups
    %rates: Foster VJ, Keenan FP, Reid RHG, ADNDT 67, 99, 1997
    %energies: From .elvlc file, experimental energies
    %comment: The rate coefficients are in units cm^3/s.
    %comment: Fits valid for temperatures 2e6 to 6e7 K.
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % Peter Young   15-May-2001
    

  9. fe_22.cilvl (collisional ionization population rates)
  10.  
    %filename: fe_22.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 Wed Jun 8 16:05:19 2022