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)

S XIII - VERSION 6.0

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

  1. s_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 (1-5,9,10): Edlen, B., 1983, Phys. Scr., 28, 51
%observed energy levels (6-8): Edlen, B., 1985, Phys. Scr., 32, 86
%observed energy levels (15,16,31,37,44,47,53-55,76,77,81): Fawcett & Hayes 1987, Phys. Scr., 36, 80
%observed energy levels (38-42,45): Goldsmith, S., Oren, L., Cohen, L., 1974, ApJ, 188, 197
%observed energy levels (52,88): Lepson, J.K., Beiersdorfer, P., Behar, E., & Kahn, S.M., 2005, ApJ, 625, 1045
%observed energy levels (25): Ralchenko, Yu., Jou, F.-C., Kelleher, D.E., Kramida, A.E., Musgrove, A.,
     Reader, J., Wiese, W.L., & Olsen, K. 2005, NIST Atomic Spectra Database (version 3.0.2), National Institute
     of Standards and Technology, Gaithersburg, MD
%observed energy levels (91): average from Fawcett, B.C., Hardcastle, R.A., & Tondello, G. 1970, J. Phys. B., 3, 564
       and Fawcett & Hayes 1987
%observed energy levels (11,13,17,18,20,27-29,32,46): Average from Fawcett & Hayes 1987 and Goldsmith et al 1974
%observed energy levels (19): Average from Fawcett & Hayes 1987, Goldsmith et al 1974 and Lepson et al. 2005
%observed energy levels (84): Average from Fawcett & Hayes 1987 and Lepson et al. 2005
%observed energy levels (48): Average from Goldsmith et al 1974, Lepson et al. 2005 and 
       Kardi, S., et al., 1994, Phys. Scr., 49, 571
%observed energy levels (56): Average from Fawcett & Hayes 1987, Goldsmith et al 1974, Khardi et al 1994 and
       Lepson et al. 2005
%Theoretical energy levels: 27-conf model from Landi & Bhatia 2008, ADNDT, 94, 1
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%  E. Landi - Sep 2006

  2. s_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. 

     
%filename: s_13.wgfa
%observed energy levels (1-5,9,10): Edlen, B., 1983, Phys. Scr., 28, 51
%observed energy levels (6-8): Edlen, B., 1985, Phys. Scr., 32, 86
%observed energy levels (15,16,31,37,44,47,53,54,55,76,77,81): Fawcett & Hayes 1987, Phys. Scr., 36, 80
%observed energy levels (38-42,45): Goldsmith, S., Oren, L., Cohen, L., 1974, ApJ, 188, 197
%observed energy levels (52,88): Lepson, J.K., Beiersdorfer, P., Behar, E., & Kahn, S.M., 2005, ApJ, 625, 1045
%observed energy levels (25): Ralchenko, Yu., Jou, F.-C., Kelleher, D.E., Kramida, A.E., Musgrove, A.,
     Reader, J., Wiese, W.L., & Olsen, K. 2005, NIST Atomic Spectra Database (version 3.0.2), National Institute
     of Standards and Technology, Gaithersburg, MD
%observed energy levels (91): average from Fawcett, B.C., Hardcastle, R.A., & Tondello, G. 1970, J. Phys. B., 3, 564
       and Fawcett & Hayes 1987
%observed energy levels (11,13,17,18,20,27-29,32,46): Average from Fawcett & Hayes 1987 and Goldsmith et al 1974
%observed energy levels (19): Average from Fawcett & Hayes 1987, Goldsmith et al 1974 and Lepson et al. 2005
%observed energy levels (84): Average from Fawcett & Hayes 1987 and Lepson et al. 2005
%observed energy levels (48): Average from Goldsmith et al 1974, Lepson et al. 2005 and
       Kardi, S., et al., 1994, Phys. Scr., 49, 571
%observed energy levels (56): Average from Fawcett & Hayes 1987, Goldsmith et al 1974, Khardi et al 1994 and
       Lepson et al. 2005
%Theoretical energy levels: 27-conf model from Landi & Bhatia 2008, ADNDT, 94, 1
%A values and oscillator strengths: 27-conf model from Landi & Bhatia 2008, ADNDT, 94, 1
%% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%  E. Landi - Sep 2006

  3. s_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: s_13.splups
%Oscillator strengths: 27-conf model from Landi & Bhatia 2008, ADNDT, 94, 1
%Effective collision strengths (levels 1-10): Keenan, 1988, Physica Scripta, 37, 57
%Collision strengths (levels 11-92): 27-conf model from Landi & Bhatia 2008, ADNDT, 94, 1
%Comment: effective collision strengths were provided in the 5.6 < Log T < 7.2 temperature range
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Aug 2006

  4. s_13.psplups (proton collision data)

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

     

%filename: s_13.psplups
%rates: Ryans R.S.I., Foster-Woods V.J, Copeland F., Keenan F.P., Matthews A., Reid R.H.G., 1998, ADNDT 70, 179-229
%energies: Martin W.C., Sugar J., Musgrove A., Dalton G.R., 1995, NIST Database for Atomic Spectroscopy, 
    Version 1.0, NIST Standard Reference Database 61.
%comment: Fits valid for temperatures 5e5 to 7.5e7 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young  24-Oct-00

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

    s_13_table.html (html table)


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