Fe XIX - VERSION 10.0.2


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

  1. fe_19.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename:  fe_19.elvlc
    
    Observed energies: 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 [2013, May 3]. National Institute of Standards and Technology, Gaithersburg, MD.
    
    Theoretical energies:
    Butler, K. & Badnell, N. R. 2008, A&A, 489, 1369
    
    Levels 343-630 are from  CHIANTI v.7.1:
    Theoretical energy levels (below ionization): Landi & Gu, 2006, ApJ, 640, 1171
    
    Produced for the CHIANTI database v.8 by G. Del Zanna Mar 2014
    
    revised in Feb 2018 by K. Dere
    
    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
    
    optimized through an ISHFTIC file with the observed energies of:
    
    NIST for levels 1-10 and , for levels 631 and 632:
    
    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) - 2018 February 19
    
    %comment: Fixed text problems in comments. No change to data.  Peter Young, 25-Jul-2019
    
     
    

  3. fe_19.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_19.wgfa
    
    Observed energies: 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 [2013, May 3]. National Institute of Standards and Technology, Gaithersburg, MD.
    
    Theoretical energies:
    Butler, K. & Badnell, N. R. 2008, A&A, 489, 1369
    
    Levels 343-630 are from  CHIANTI v.7.1:
    observed energy levels (above ionization): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175
    Theoretical energy levels (below ionization): Landi & Gu, 2006, ApJ, 640, 1171
    Radiative data (below ionization): Landi & Gu, 2006, ApJ, 640, 1171
    
    Produced for the CHIANTI database v.8 by G. Del Zanna Mar 2014
    
    Revised in Feb 2018 by K. Dere
    
    Theoretical energy levels, oscillator strengths and A values for transitions from autoionizing 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
    
    optimized through an ISHFTIC file with the observed energies of:
    
    NIST for levels 1-10 and , for levels 631 and 632
    
    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) - 2018 February 19
    
    
    minimum branching ratio =   1.00e-05
    %File processed with wgfa_tidy by pryoung on  6-Mar-2019
    
    %comment: Fixed text problems in comments. No change to data.  Peter Young, 25-Jul-2019
    

  5. fe_19.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    
    
    
    Modified by G. Del Zanna on 2018 Oct 30 to fix the high-energy extrapolation of the Butler & Badnell data.
    
    Produced for the CHIANTI database v.8 by G. Del Zanna Mar 2014
    
    Collisional data (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171
    Collision strengths (343-630) computed with the Flexible Atomic Code - Gu, M.F., 2003, ApJ, 582, 1241
    oscillator strengths (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171
    The data for levels 343-636 are from CHIANTI v.7.1:
    
    Levels 1-342: data from Butler & Badnell A&A v489, 1369 (2008).
    
    

  7. fe_19.psplups (proton collision data)
  8. contains the spline fits to the scaled proton collision strengths.

     
    
    %filename: fe_19.psplups
    %rates: Ryans R.S.I., Keenan F.P., Reid R.H.G., unpublished.
    %energies: Observed values, from .elvlc file
    %comment: Fits valid for temperatures 2e6 to 4e7 K.
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % Peter Young   15-May-2001
    

  9. fe_19.cilvl (collisional ionization population rates)
  10.  
    %filename: fe_19.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 Wed Jun 8 16:04:16 2022