Cl III - VERSION 8.0


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

  1. cl_3.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename: cl_3.elvlc
    %observed energies:  Ralchenko, Yu., Kramida, A.E., Reader, J., and NIST ASD Team (2010). 
         NIST Atomic Spectra Database (ver. 4.0.1), [Online]. Available: http://physics.nist.gov/asd 
         [2010, December 1]. National Institute of Standards and Technology, Gaithersburg, MD
    %theoretical energies: Ramsbottom, C.A., Bell, K.L., & Keenan, F.P. 2001, ADNDT, 77, 57
    % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    %   Peter Young, 1-Dec-2010
     
    

  3. cl_3.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: cl_3.wgfa
    %observed energies:  Ralchenko, Yu., Kramida, A.E., Reader, J., and NIST ASD Team (2010).
         NIST Atomic Spectra Database (ver. 4.0.1), [Online]. Available: http://physics.nist.gov/asd
         [2010, December 1]. National Institute of Standards and Technology, Gaithersburg, MD
    %A-values: Mendoza, C., & Zeippen, C.J., MNRAS, 198, 127, 1982
    % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    %   Peter Young, 1-Dec-2010
    

  5. cl_3.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    %filename:  cl_3.splups
    %Theoretical energies: Ramsbottom, C.A., Bell, K.L., & Keenan, F.P. 2001, ADNDT, 77, 57
    %Effective collision strengths: Ramsbottom, C.A., Bell, K.L., & Keenan, F.P. 2001, ADNDT, 77, 57
    %Comment:  Ramsbottom et al. (2001) gave LS energies. For transitions within multiplets, an
    energy splitting of 0.001 Ryd has been assumed.
    The spline fits are accurate to 0.56% or better over the temperature range 7500 to 250,000 K.
    % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    %   Peter Young, 1-Dec-2010
    
    

  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

    cl_3_table.html (html table)

    Page created by Giulio Del Zanna on Fri Sep 18 13:25:38 2015