Ca XVIII - VERSION 8.0


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

  1. ca_18.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename:  ca_18.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
    
    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.
    
    Energy values (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 corrected by Safronova data on an inner term basis
     energies of Safronova have been treated as "observed energies" 
    
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2014 November 21
     -1
     
    

  3. ca_18.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:  ca_18.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
    
    wavelengths determined from energy levels
    
    A values and wavelengths (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
    
     minimum branching ratio =   1.00e-05
    
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2014 November 21
    

  5. ca_18.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    %filename:  ca_18.scups
    
    Theoretical gf A values:  Whiteford, A. D., Badnell, N. R., Ballance, C. P., O'Mullane, M. G., Summers, H. P., Thomas, A. L., 2001, J. Phys. B, 34, 3179
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
    
    Theoretical collision strengths:  Whiteford, A. D., Badnell, N. R., Ballance, C. P., O'Mullane, M. G., Summers, H. P., Thomas, A. L., 2001, J. Phys. B, 34, 3179
    collision strengths provided in the range   6.48e+04 to   6.48e+08 K
    
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
    K. Dere (GMU) - 2012 December 31
    
    

  7. (proton collisional data) Not available in this VERSION.
  8. ca_18.reclvl (total recombination population rates)
  9.  
    filename:  ca_18.reclvl
    
    %Radiative recombination rates for recombination onto Ca XIX to form Ca XVIII
    Badnell, N. R., 2006, ApJS, 167, 334
    Radiative Recombination Data for Modeling Dynamic Finite-Density Plasmas
    adsLink:  http://adsabs.harvard.edu/abs/2006ApJS..167..334B
    
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2014 September 15
    


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

    ca_18_table.html (html table)

    Page created by Giulio Del Zanna on Fri Sep 18 13:25:31 2015