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 XI - VERSION 6.0

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

  1. s_11.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 (n=2): Edlen, B., 1985, Phys. Scr., 31, 345
%Observed energy levels (22-24,37,39-43,45,46,67,72): Ralchenko Y., 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
%Observed energy levels (35,36,44): Bromage, G.E., Fawcett, B.C., 1977, MNRAS, 178, 605
%Observed energy levels (28,31,32,64,68): Lepson et al, 2005, ApJ, 625, 1045
%Theoretical energy levels: from the 24-configuration model by Landi & Bhatia 2003, ApJ, 149, 251
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
% 
%  E. Landi - March 2005

  2. s_11.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_11.wgfa
%Observed energy levels (n=2): Edlen, B., 1985, Phys. Scr., 31, 345
%Observed energy levels (22-24,37,39-43,45,46,67,72): Ralchenko Y., 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
%Observed energy levels (35,36,44): Bromage, G.E., Fawcett, B.C., 1977, MNRAS, 178, 605
%Observed energy levels (28,31,32,64,68): Lepson et al, 2005, ApJ, 625, 1045
%Theoretical energy levels: from the 24-configuration model by Landi & Bhatia 2003, ApJ, 149, 251
%oscillator strengths and A values: from the 24-configuration model by Landi & Bhatia 2003, ApJ, 149, 251
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%  E. Landi - March 2005

  3. s_11.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_11.splups
%Oscillator strengths: from the 9-conf model of Landi & Bhatia 2003, ApJ, 149, 251
%Effective collision strengths levels 1-6: Conlon, Keenan & Aggarwal, 1992, Phys. Scripta, 45,309
%Collision strengths levels 7-72: from the 9-conf model of Landi & Bhatia 2003, ApJ, 149, 251
%comment: effective collision strengths are provided in the range 5.45 < log T < 7.05
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Apr 2003

  4. s_11.psplups (proton collision data)

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

     

%filename: s_11.psplups
%rates: Ryans R.S.I., Foster-Woods V.J, Keenan F.P., Reid R.H.G., 1999, ADNDT 73, 1-42
%energies: CHIANTI database, ver.1, Dere et al., A&AS 125, 149, 1997
%comment: Fits valid for temperatures 4e5 to 3e7 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   10-Sep-2002

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

    s_11_table.html (html table)


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