The CHIANTI database has the following primary ASCII files for this ion:
contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.
%filename: ar_10.elvlc
%Observed energy levels (n=2 levels): Edlen, B., 1983, Physica Scripta, 28, 51
%Observed energy levels (n=3,4 levels): Lepson, J.K., Beiersdorfer, P., Behar, E., & Kahn, S.M. 2003, ApJ, 590, 604
%Observed energy levels (4,6,23,64,65,79): Fawcett, B.C., Gabriel, A.H., & Paget, T.M. 1971, J.Phys.B, 4, 986
%Observed energy level (10): Average from measurements of Lepson et al. (2003) and Fawcett et al. (1971)
%Observed energy levels (96,97): Connerade, J.P., Peacock, N.J., Speer, R.J., 1971, Solar Physics, 18, 63
%Observed energy levels (11-17,19,21,22,25-28,31-34,37,38,42,4350,51,54): Bengtsson, P., Engstroem, L., Jupen, C., 1994, Physica Scripta, 49, 297
%Comment: The energies from Bengtsson et al 1994 have been calculated using their observed wavelengths and
the energies of levels 4 to 10 (2s2.2p4.3s configuration) from the sources listed above.
%Theoretical energy levels: Witthoeft, M.C., Whiteford, A.D., & Badnell, N.R. 2007, J.Phys.B, 40, 2969
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Feb 2007
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: ar_10.wgfa
%Observed energy levels (n=2 levels): Edlen, B., 1983, Physica Scripta, 28, 51
%Observed energy levels (n=3,4 levels): Lepson, J.K., Beiersdorfer, P., Behar, E., & Kahn, S.M. 2003, ApJ, 590, 604
%Observed energy level (10): Average from measurements of Lepson et al. (2003) and Fawcett et al. (1971)
%Observed energy levels (4,6,23,64,65,79): Fawcett, B.C., Gabriel, A.H., & Paget, T.M. 1971, J.Phys.B, 4, 986
%Observed energy levels (96,97): Connerade, J.P., Peacock, N.J., Speer, R.J., 1971, Solar Physics, 18, 63
%Observed energy levels (11-17,19,21,22,25-28,31-34,37,38,42,4350,51,54): Bengtsson, P., Engstroem, L., Jupen, C., 1994, Physica Scripta, 49, 297
%Comment: The energies from Bengtsson et al 1994 have been calculated using their observed wavelengths and
the energies of levels 4 to 10 (2s2.2p4.3s configuration) from the sources listed above.
%Theoretical energy levels: Witthoeft, M.C., Whiteford, A.D., & Badnell, N.R. 2007, J.Phys.B, 40, 2969
%Radiative data: Witthoeft, M.C., Whiteford, A.D., & Badnell, N.R. 2007, J.Phys.B, 40, 2969
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Feb 2007
%File processed with wgfa_tidy by pryoung on 6-Mar-2019
%File processed with wgfa_tidy by pryoung on 31-May-2023
contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).
% E. Landi - Jan 2007
%
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
temperatures the Ar X abundance is negligible under equilibrium.
%comment: data at very high or very low temperatures were sometimes discarded to improve the fit. At these
%comment: effective collision strengths are USED for temperatures in the range 4.9 < Log T < 7.0
%comment: effective collision strengths are published for temperatures in the range 4.3 < Log T < 8.3
%Effective collision strengths: Witthoeft, M.C., Whiteford, A.D., & Badnell, N.R. 2007, J.Phys.B, 40, 2969
%Oscillator strengths: Witthoeft, M.C., Whiteford, A.D., & Badnell, N.R. 2007, J.Phys.B, 40, 2969
%filename: ar_10.splups
contains the spline fits to the scaled proton collision strengths.
%filename: ar_10.psplups %rates: Bely, O., Faucher, P., 1970, A&A 6, 88 %energies: Observed energies from .elvlc file. %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Peter Young 8-Jun-2001
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