Mg X - VERSION 10.0.2


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

  1. mg_10.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename:  mg_10.elvlc.olg.nist
    
    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
    
    Autostructure calculation optimized with 'SHFTIC' file using energy corrections from the following sources:
    
    Observed bound energy levels and for n=2,3 above IP:
    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, 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
    physics.nist.gov/asd [2012, September 14]. National Institute of Standards and Technology, Gaithersburg, MD.
    
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2017 August 03
    
    
     
    

  3. mg_10.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:  mg_10.wgfa.olg.imp
    
    Theoretical radiative data:
    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
    
    Autostructure calculation optimized with 'SHFTIC' file using energy corrections from the following sources:
    
    Observed bound energy levels and n=2,3 above IP:
    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, 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
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2017 August 03
    %File processed with wgfa_tidy by pryoung on  6-Mar-2019
    

  5. mg_10.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 23
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
    
    collision strengths provided in the range   2.00e+04 to   2.00e+08 K
    BibCode:  2011A&A...528A..69L
    DOI:  http://dx.doi.org/10.1051/0004-6361/201016417
    adsRef:  http://adsabs.harvard.edu/abs/2011A%26A...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: mg_10.ups
    

  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

    mg_10_table.html (html table)

    Page created by Giulio Del Zanna on Wed Jun 8 16:08:03 2022