CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.

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Naval Research Laboratory (USA) - Rutherford Appleton Laboratory (UK)
University of Cambridge (UK) - George Mason University (USA) - Universita' degli Studi di Firenze (Italy)

Ca XIII - VERSION 5.1

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

  1. ca_13.elvlc (energy levels)

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

     
%Observed energy levels (1 - 10): Edlen, 1983, Ph. Scr., 28, 51
%Observed energy levels (4,5): Feldman, Curdt, Landi, Wilhelm, 2000, ApJ, 544, 508
%Observed energy levels (11): from the spectrum of Acton et al 1985, ApJ, 291, 865
%Observed energy levels (12 - 16,25 - 26): Doschek et al 1973, J.Opt.Soc.Am, 63, 1463
%Observed energy levels (2s2.2p3.3d configuration): Fawcett & Hayes, 1975, MNRAS, 170, 185
%theoretical energy levels: Landi, E., Bhatia, A.K., 2005, A&A, in press
%comment: theoretical energy levels come from the 24-configuration calculation in Landi & Bhatia (2005)
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Mar 2005

  2. ca_13.wgfa (radiative data)

    3. 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. 

     
%Observed energy levels (1-10): Edlen, 1983, Ph. Scr., 28, 51
%Observed energy levels (4,5): Feldman, Curdt, Landi, Wilhelm, 2000, ApJ, 544, 508
%Observed energy levels (11): from the spectrum of Acton et al 1985, ApJ, 291, 865
%Observed energy levels (12-16,25-26): Doschek et al 1973, J.Opt.Soc.Am, 63, 1463
%Observed energy levels (2s2.2p3.3d configuration): Fawcett & Hayes, 1975, MNRAS, 170, 185
%theoretical energy levels: Landi, E., Bhatia, A.K., 2005, A&A, in press
%comment: theoretical energies and radiative data come from the 24-configuration calculation in Landi & Bhatia (2005)
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Apr 2005

  3. ca_13.splups (electron collision data)

    4. contains the spline fits to the electron collision strengths scaled according the rules formulated by Burgess and Tully (1992). Accurate replication of the temperature averaged collision strength over a wide range of temperatures can be accomplished with the data in this file. 

     

%filename: ca_13.splups
%Collision strengths: Landi & Bhatia 2005, A&A, in press
%Oscillator strengths: Landi & Bhatia 2005, A&A, in press
%comment: oscillator strengths have been taken from the 6-configuration model of Landi & Bhatia
    (2005) for consistency with the collisional calculation
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Mar 2005

  4. ca_13.psplups (proton collision data)

    5. contains the spline fits to the scaled proton collision strengths. 

     

%filename: ca_13.psplups
%rates: Ryans R.S.I., Keenan F.P., Reid R.H.G., unpublished.
%energies: Observed values, from .elvlc file
%comment: Fits valid for temperatures 7e5 to 1.2e7 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   15-May-2001

    The html tables below contain the radiative data of the brightest lines sorted in wavelength


    Last revised by G. Del Zanna on 4-Sep-2009