Cr XXII - VERSION 8.0


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

  1. cr_22.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename:  cr_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
    
    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 (above IP):  calculations of U. Safronova reported in Kato et al., 1997, ADNDT, 67, 225.
    ADS http://adsabs.harvard.edu/abs/1997ADNDT..67..225K
     updated by U. Safronova, 2001, private communication
     theoretical energy levels corrected by Safronova data on an inner term basis
     energies of Safronova have been treated as "observed energies" 
     
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2014 November 19
     -1
     
    

  3. cr_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:  cr_22.wgfa
    
    Observed wavelengths:  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.
    
    Theoretical energies, gf and 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
    
    wavelengths determined from energy levels
    
    wavelengths:  calculations of U. Safronova reported in Kato et al., 1997, ADNDT, 67, 225.
    ADS http://adsabs.harvard.edu/abs/1997ADNDT..67..225K
    updated by U. Safronova, 2001, private communication
     theoretical energy levels corrected by Safronova data on an inner term basis
     wavelengths of Safronova have been treated as "observed wavelengths" 
    
     minimum branching ratio =   1.00e-05
    
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2014 November 19
    

  5. cr_22.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    %filename:  cr_22.scups
    
    Theoretical gf A values:  Whiteford, A. D., Badnell, N. R., Ballance, C. P., O'Mullane, M. G., Summers, H. P., Thomas, A. L., 2001, J. Phys. B, 34, 3179
    
    Theoretical collision strengths:  Whiteford, A. D., Badnell, N. R., Ballance, C. P., O'Mullane, M. G., Summers, H. P., Thomas, A. L., 2001, J. Phys. B, 34, 3179
    collision strengths provided in the range   9.68e+04 to   9.68e+08 K
    
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
    K. Dere (GMU) - 2013 January 16
    
    

  7. (proton collisional data) Not available in this VERSION.
  8. cr_22.reclvl (total recombination population rates)
  9.  
    filename:  cr_22.reclvl
    
    %Radiative recombination rates for recombination onto Cr XXIII to form Cr  XXII
    Badnell, N. R., 2006, ApJS, 167, 334
    Radiative Recombination Data for Modeling Dynamic Finite-Density Plasmas
    adsLink:  http://adsabs.harvard.edu/abs/2006ApJS..167..334B
    
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2014 September 15
    


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

    cr_22_table.html (html table)

    Page created by Giulio Del Zanna on Fri Sep 18 13:25:51 2015