Zn XXVIII - VERSION 10.0.2


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

  1. zn_28.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename:  zn_28.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(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 energies for n=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
    
    produced as a part of the  'CHIANTI' atomic database for astrophysical spectroscopy
    K. Dere (GMU) - 2018 December 01
    zn_28 IP ev =  2.78345e+03 Ip invcm =    22450000.000 Ip Ryd =     204.57945
    zn_29 IP ev =  1.18648e+04 Ip invcm =    95696100.000 Ip Ryd =     872.04700
     
    

  3. zn_28.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:  zn_28.wgfa
    
    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
    
    
    Autostructure calculation optimized with 'SHFTIC' file using energy corrections from the following sources:
    
    observed(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 energies for n=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
    
    Wavelengths determined from energy levels
    
    Minimum branching ratio =   1.00e-04
    
     allWvl =   1
     minDiff =      0.00010
     outfile = zn_28.wgfa.olg.imp
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2018 December 02
    %File processed with wgfa_tidy by pryoung on  6-Mar-2019
    

  5. zn_28.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) - 2013 January 03
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
    collision strengths provided in the range   1.57e+05 to   1.57e+09 K
    
    ADS ref:  https://ui.adsabs.harvard.edu/abs/2011A%26A...528A..69L/abstract
    DOI:  https://ui.adsabs.harvard.edu/link_gateway/2011A&A...528A..69L/doi:10.1051/0004-6361/201016417
    Astronomy & Astrophysics, Volume 528, id.A69, 15 pp
    including Auger and radiation damping
    R-matrix electron-impact excitation data for the Li-like iso-electronic sequence
    Liang, G. Y.; Badnell, N. R.
    Theoretical collision strengths:
    
    %filename:  zn_28.upsdat  
    

  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

    zn_28_table.html (html table)

    Page created by Giulio Del Zanna on Wed Jun 8 16:15:38 2022