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

si_11.elvlc (energy levels)

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

 
%observed energy levels (1-10): Edlen, B. 1983, Phys. Scr., 28, 51
%observed energy levels (13,17-19): Acton, L.W., Bruner, M.E., Brown, W.A., Fawcett, B.C., Schweizer, W., & 
     Speer, R.J. 1985, ApJ, 291, 865
%observed energy levels (16,20,21,27-29,31,39,40,42,43,46-48,53,54,59,90,91): Hoory, S., Feldman, U., Goldsmith, S., 
     Behring, W., & Cohen, L. 1970, J.Opt.Soc.Am., 60, 1449
%observed energy levels (35,37,41,45,92): 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 (52): Tondello, G. 1969, J.Phys. B, 2, 727
%observed energy levels (11,32,55) average of measurements from NIST and Hoory et al. 1970
%observed energy levels (12,80,81): average of measurements from Tondello 1969 and Hoory et al. 1970
%observed energy levels (56): average of measurements from Tondello 1969, Hoory et al. 1970 and NIST
%observed energy levels (76,77): average of measurements from Hoory et al. 1970 and Fawcett, B.C., Hardcastle, R.A., 
     & Tondello, G 1970, J. Phys. B, 3, 564
%observed energy levels (15,49,50): Brandt, B., Trabert, E., Heckmann, P.H., Fawcett, B.C. 1988, Zeit. Phys. D, 9, 279
%observed energy levels (51,87): Khardi, S., Buchet-Poulizac, M.C., Buchet, J.P., Carre', M., Denis, A., 
     Desesquelles, J., Livingstone, A.E., Martin, S., & Ouerdane, Y. 1994, Phys. Scr., 49, 571
%Theoretical energy levels: 27-conf model from Bhatia & Landi, 2007, ADNDT, 93, 275
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%  E. Landi - Oct. 2005
 

si_11.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.

 
%filename: si_11.wgfa
%observed energy levels (1-10): Edlen, B. 1983, Phys. Scr., 28, 51
%observed energy levels (13,17-19): Acton, L.W., Bruner, M.E., Brown, W.A., Fawcett, B.C., Schweizer, W., &
     Speer, R.J. 1985, ApJ, 291, 865
%observed energy levels (16,20,21,27-29,31,39,40,42,43,46-48,53,54,5,9,90,91): Hoory, S., Feldman, U., Goldsmith, S.,
     Behring, W., & Cohen, L. 1970, J.Opt.Soc.Am., 60, 1449
%observed energy levels (35,37,41,45,92): 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 (52): Tondello, G. 1969, J.Phys. B, 2, 727
%observed energy levels (11,32,55) average of measurements from NIST and Hoory et al. 1970
%observed energy levels (12,80,81): average of measurements from Tondello 1969 and Hoory et al. 1970
%observed energy levels (56): average of measurements from Tondello 1969, Hoory et al. 1970 and NIST
%observed energy levels (76,77): average of measurements from Hoory et al. 1970 and Fawcett, B.C., Hardcastle, R.A.,
     & Tondello, G 1970, J. Phys. B, 3, 564
%observed energy levels (15,49,50): Brandt, B., Trabert, E., Heckmann, P.H., Fawcett, B.C. 1988, Zeit. Phys. D, 9, 279
%observed energy levels (51,87): Khardi, S., Buchet-Poulizac, M.C., Buchet, J.P., Carre', M., Denis, A.,
     Desesquelles, J., Livingstone, A.E., Martin, S., & Ouerdane, Y. 1994, Phys. Scr., 49, 571
%Theoretical energy levels: 27-conf model from Bhatia & Landi 2007, ADNDT, 93, 275
%A values and oscillator strengths: 27-conf model from Bhatia & Landi 2007, ADNDT, 93, 275
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
% 
%  E. Landi - Oct. 2005

si_11.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: si_11.splups
%Oscillator strengths: Bhatia & Landi 2007, ADNDT, 93, 275
%Effective collision strengths (among levels 1-10): Berrington,K.A., Burke,P.G., Dufton,P.L., Kingston,A.E., 1985, ADNDT, 33, 195
%Collision strengths (all other transitions): Bhatia & Landi 2007, ADNDT, 93, 275
%comment: Temperature range of validity of the effective collision strengths: 5.40 < LogT < 7.00
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Feb 2006

si_11.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: si_11.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: CHIANTI database, ver.1, Dere et al., A&AS 125, 149, 1997
%comment: Fits valid for temperatures 4e5 to 8d7 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young  19-Oct-00

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

si_11_table.html (html table)


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