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

ca_15.elvlc (energy levels)

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

 
%energy levels (n=2): Edlen, B., 1985, Phys.Scripta, 31, 345
%energy levels (n=3): Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995,
   NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61.
%Theoretical energy levels (1-15) : 3 conf model of SSTRUCT
%Theoretical energy levels (16-46) : Bhatia, A.K., Doschek, G.A., 1993, ADNDT, 53, 195
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%  E.Landi and P.R.Young 2000
 

ca_15.wgfa (radiative data)

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 (n=2): Edlen, B., 1985, Physica Scripta, 31, 345
%observed energy levels (n=3): Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995,
   NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61.
%oscillator strengths (6-46 transitions) : Bhatia, A.K., Doschek, G.A., 1993, ADNDT, 53, 195
%A values: Froese Fischer & Saha, 1985, Phys. Scripta 32, 181 
%comment: Theoretical energies were used by Froese Fischer & Saha to derive
	 the transition probabilities, but as the theoretical energies
	 tabulated in the above paper did not differ from the observed
	 values by more than 0.5%, it was not deemed necessary to re-scale
	 the A values to account for this.
%comment: negative wavelengths have been computed using theoretical energy levels
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
% 
% E.Landi and P.R.Young 2000

ca_15.splups (electron collision data)

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_15.splups
%oscillator strengths: are taken from "superstructure" using a 3
   configuration model of the ion, which was shown to closely match the
   'HF+2p4' oscillator strengths found in Aggarwal, 1983, J.Phys.B, 16, 2231
%collision strengths transitions 6-46 : Bhatia, A.K., Doschek, G.A., 1993, ADNDT, 53, 195
%effective collision strengths (transitions 1 - 15): Aggarwal, Berrington & Keenan, 1991, ApJS, 77, 441
%comment: the authors regard their collisional model to be accurate to ~10%. 
%comment: effective collision strengths were given in the temperature range 5.0 < Log T < 7.0.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%  E.Landi and P.R.Young 2000

ca_15.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: ca_15.psplups
%rates: Ryans R.S.I., Foster-Woods V.J, Keenan F.P., Reid R.H.G., 1999, ADNDT 73, 1-42
%energies: Cheng K.T., Kim Y.K., Desclaux J.P., 1979, ADNDT 24, 111
%comment: Fits valid for temperatures 7e5 to 6e7 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   15-May-2001

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

ca_15_table.html (html table)


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