Cr XXIII - VERSION 10.0.2


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

  1. cr_23.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename:  cr_23.elvlc.nist
    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 (theoretical) energy levels (1s2s, 1s2p):  Artemyev, A. N.; Shabaev, V. M.; Yerokhin, V. A.; Plunien, G.; Soff, G., 2005, Phys. Rev. A, 72, 2104
    ADSref:  http://adsabs.harvard.edu/abs/2005PhRvA..71f2104A
    
    Observed energy levels:  Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2018).
     NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/asd [Tue Feb 20 2018]. 
    National Institute of Standards and Technology, Gaithersburg, MD.
    
    Observed wavelengths, energies: 1s^2 - 1s2p 1P1, 1s4p 1P1, 1s5p 1P1:
    
    Beiersdorfer, P.; Bitter, M.; von Goeler, S.; Hill, K. W.
    Physical Review A (General Physics), Volume 40, Issue 1, July 1, 1989, pp.150-157
    DOI:  https://ui.adsabs.harvard.edu/link_gateway/1989PhRvA..40..150B/doi:10.1103/PhysRevA.40.150
    ADSref:  https://ui.adsabs.harvard.edu/abs/1989PhRvA..40..150B/abstract
    
    Theoretical energies for n=2, 3 above IP
    Goryaev, F. F.; Vainshtein, L. A.; Urnov, A. M.
    Atomic data for doubly-excited states 2lnl‧ of He-like ions and 1s2lnl‧ of Li-like ions with Z = 6-36 and n = 2 , 3
    2017, ADNDT, 113, 117-257
    adsRef:  http://adsabs.harvard.edu/abs/2017ADNDT.113..117G
    DOI:  10.1016/j.adt.2016.04.002
    
    Theoretical energy levels (n=4,5 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 adjusted by SHFTIC file derived from 
    Artemyev, nterpolated bnd energies, Goryaev (n=2, 3 above IP) and Safronova (n= 4,5,6 above IP energies
    
    
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
    K. Dere (GMU) - 2020 October 07
     
    

  3. cr_23.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_23.wgfa.olg.imp
    Theoretical 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
    
    Observed (theoretical) energy levels (1s2s, 1s2p):  Artemyev, A. N.; Shabaev, V. M.; Yerokhin, V. A.; Plunien, G.; Soff, G., 2005, Phys. Rev. A, 72, 2104
    ADSref:  http://adsabs.harvard.edu/abs/2005PhRvA..71f2104A
    
    Observed energy levels:  Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2018).
     NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/asd [Tue Feb 20 2018]. 
    National Institute of Standards and Technology, Gaithersburg, MD.
    
    Observed wavelengths, energies: 1s^2 - 1s2p 1P1, 1s4p 1P1, 1s5p 1P1:
    
    Beiersdorfer, P.; Bitter, M.; von Goeler, S.; Hill, K. W.
    Physical Review A (General Physics), Volume 40, Issue 1, July 1, 1989, pp.150-157
    DOI:  https://ui.adsabs.harvard.edu/link_gateway/1989PhRvA..40..150B/doi:10.1103/PhysRevA.40.150
    ADSref:  https://ui.adsabs.harvard.edu/abs/1989PhRvA..40..150B/abstract
    
    Theoretical energies for n=2, 3 above IP
    Goryaev, F. F.; Vainshtein, L. A.; Urnov, A. M.
    Atomic data for doubly-excited states 2lnl‧ of He-like ions and 1s2lnl‧ of Li-like ions with Z = 6-36 and n = 2 , 3
    2017, ADNDT, 113, 117-257
    adsRef:  http://adsabs.harvard.edu/abs/2017ADNDT.113..117G
    DOI:  10.1016/j.adt.2016.04.002
    
    Theoretical energy levels (n=4,5 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 adjusted by SHFTIC file derived from 
    Artemyev, Goryaev (n=2, 3 above IP) and Safronova (n= 4,5,6 above IP energies
    
    two-photon A-value:  Derevianko, A.; Johnson, W. R., 1997, Phys Rev A, 56, 1288 
     Two-photon decay of 2 1S0 and 2 3S1 states of heliumlike ions  
     ADSref:  https://ui.adsabs.harvard.edu/abs/1997PhRvA..56.1288D/abstract 
     sorted by lvl12
     
    elvlcName = cr_23.elvlc.nist
     wgfaName = cr_23.wgfa-srt
     allWvl =   1
     minDiff =      0.00010
     outfile = cr_23.wgfa.olg.imp
     wavelengths determined from energy levels
     
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2020 October 07
    

  5. cr_23.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    
    K. Dere (GMU) - 2020 February 09
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
    collision strengths provided in the range   1.06e+05 to   1.06e+09 K
    DOI:  http://dx.doi.org/10.1088/0953-4075/34/15/320
    adsRef:  http://adsabs.harvard.edu/abs/2001JPhB...34.3179W
    A radiation-damped R-matrix approach to the electron-impact excitation of helium-like ions for diagnostic application to fusion and astrophysical plasmas
    Whiteford, A. D.; Badnell, N. R.; Ballance, C. P.; O'Mullane, M. G.; Summers, H. P.; Thomas, A. L.
    
    filename: cr_23.scups
    
    

  7. (proton collisional data) Not available in this VERSION.

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

    cr_23_table.html (html table)

    Page created by Giulio Del Zanna on Wed Jun 8 16:03:30 2022