S X - VERSION 11.0

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

s_10.elvlc (energy levels)

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

 
%filename: s_10.elvlc
%Observed energy levels (1 - 15): Edlen, 1984, Phys.Scripta, 30, 135
%Observed energy levels (16 - 22): Fuhr, J.R., Kelleher, D.E., Martin, W.C., Musgrove, A., Sugar, J., Wiese, W.L.,
        Dalton, G.R., Dragoset, R.A., Mohr, P.J., Olsen, K., Reader, J., Saloman, E.B., Sansonetti, C.J.,
        Wiersma, G., "NIST Atomic Spectra Database" Ver. 2.0, March 1999, NIST Physical Reference Data
%Observed energy levels (n=3): Kink, I, Engstroem, L., 1999, Physica Scripta, 59, 355
%Theoretical energy levels: from the 24-conf model of Bhatia & Landi, 2003, ApJS, 147, 409
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic database collaboration
%
% E. Landi - Aug 2002

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_10.wgfa
Observed energy levels (1-15): Edlen, 1984, Phys.Scripta, 30, 135
%Observed energy levels (16-22): Fuhr, J.R., Kelleher, D.E., Martin, W.C., Musgrove, A., Sugar, J., Wiese, W.L.,
Dalton, G.R., Dragoset, R.A., Mohr, P.J., Olsen, K., Reader, J., Saloman, E.B., Sansonetti, C.J.,
Wiersma, G., "NIST Atomic Spectra Database" Ver. 2.0, March 1999, NIST Physical Reference Data
%Observed energy levels (n=3): Kink, I, Engstroem, L., 1999, Physica Scripta, 59, 355
%A values and oscillator strengths: from the 24-conf model of Bhatia & Landi, 2003, ApJS, 147, 409
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic database collaboration
%
% E. Landi - Aug 2002

 K. Dere - minimum branching ratio =   1.00e-05  :  2017 December 06
%File processed with wgfa_tidy by pryoung on  6-Mar-2019
%File processed with wgfa_tidy by pryoung on 31-May-2023

s_10.scups (electron collision data)

contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

 
% E. Landi and G. Del Zanna - Aug 2002                                                                     
%                                                                                                          
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic database collaboration                     
     with the collision strengths                                                                          
%Comment: the oscillator strengths have been taken from the 6-configuration calculation for consistency    
%Comment: the effective collision strength at Log T=4.6 of transition 12 - 18 has been omitted from the fit
%Comment: effective collision strengths are provided in the temperature range 4.6 < Log T < 6.7            
%Comment: Corrected errors in the transitions: 1 - 12, 2 - 22, 8 - 22, 12 - 19                             
%Oscillator strengths (levels 23-72): Bhatia & Landi, 2003, ApJS, 147, 409                                 
%Collision strengths (levels 23-72): Bhatia & Landi, 2003, ApJS, 147, 409                                  
%effective collision strengths (levels 1-22): Bell and Ramsbottom, 2000, ADNDT, 76, 176                    
%oscillator strengths (16-22): from the 6-conf model of Bhatia & Landi, 2003, ApJS, 147, 409               
%oscillator strengths (1-15):  Zhang, Sampson, 1999, ADNDT, 72, 153                                        
%filename: s_10.splups

s_10.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: s_10.psplups
%energies: Bhatia, A.K. Landi, E., 2003, ApJS, 147, 409
%rates: Bhatia, A.K. Landi, E., 2003, ApJS, 147, 409
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Feb 2003

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

s_10_table.html (html table)