Ar XVI - VERSION 10.1


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

  1. ar_16.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    
    %filename:  ar_16.elvlc
    
    Theoretical energy levels:  Autostructure calculation with energy levels optimized to match to the observed energies
    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.
    
    theoretical energies for n=2 above IP
    Yerokhin, V. A.; Surzhykov, A., Physical Review A, vol. 86, Issue 4, id. 042507
    Relativistic configuration-interaction calculation of energy levels
    of core-excited states in lithiumlike ions: Argon through krypton
    ADSref:  http://adsabs.harvard.edu/abs/2012PhRvA..86d2507Y
    DOI:  http://dx.doi.org/10.1103/PhysRevA.86.042507
    
    theoretical energy levels (n=3,4,5 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
    
    produced as a part of the  'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2017 June 03
     ar_16 IP ev =  9.18385e+02 Ip invcm =     7407274.000 Ip Ryd =      67.50005
     ar_17 IP ev =  4.12084e+03 Ip invcm =    33236829.000 Ip Ryd =     302.87626
    
    
     
    

  3. ar_16.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:  ar_16.wgfa
    
    Theoretical wavelengths, gf and A-values:  
    Autostructure calculation with energy levels optimized to match to the observed energies
    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
    
    Energy corrections to AS calculation way of 'SHFTIC' file constructed from 
    the following energies
    
    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.
    
    theoretical energies for n=2, level 67 above IP
    Yerokhin, V. A.; Surzhykov, A., Physical Review A, vol. 86, Issue 4, id. 042507
    Relativistic configuration-interaction calculation of energy levels
    of core-excited states in lithiumlike ions: Argon through krypton
    ADSref:  http://adsabs.harvard.edu/abs/2012PhRvA..86d2507Y
    DOI:  http://dx.doi.org/10.1103/PhysRevA.86.042507
    
    theoretical energy levels (n=2,3,4,5 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
    
     wavelengths determined from energy levels
    
    elvlcName = ar_16.elvlc
     wgfaName = ar_16.wgfa.olg
     allWvl =   1
     minDiff =      0.00010
     outfile = ar_16.wgfa.olg.imp
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2017 June 03
     minimum branching ratio =   1.00e-04
    %File processed with wgfa_tidy by pryoung on  6-Mar-2019
    %File processed with wgfa_tidy by pryoung on 31-May-2023
    

  5. ar_16.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) - 2017 June 17
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
    
    collision strengths provided in the range   5.12e+04 to   5.12e+08 K
    
    adsRef:  http://adsabs.harvard.edu/abs/2011A%26A...528A..69L
    DOI:  http://dx.doi.org/10.1051/0004-6361/201016417
    BibCode:  2011A&A...528A..69L
    R-matrix electron-impact excitation data for the Li-like iso-electronic sequence including Auger and radiation damping
    Liang, G. Y.; Badnell, N. R.
    theoretical collision strenghs:
    
    %filename: ar_16.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

    ar_16_table.html (html table)

    Page created by Giulio Del Zanna on Mon Jun 26 11:14:06 2023