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: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995, 
   NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61
%Theoretical energy levels (1-10): Zhang, Sampson, ADNDT, 1992, 52, 143
%theoretical energy levels (11-46): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%  K.P. Dere Jan. 1996 (levels 11-46), E. Landi 1995 (n=2 levels)
 

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.

 
%observed energy levels: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995,
   NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61
%theoretical energy levels (11-46): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125
%A values(1 - 10 levels): Calculated using SSTRUCT
%A values(11 - 46 levels): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125.
%comment: Have re-calculated the A values for the first 10 levels using 
  SSTRUCT. The major addition is the 3-4 transition probability 
  which has a considerable effect on the level balance at low 
  densities. The SSTRUCT model included the following 15 
  configurations:

	2s2, 2s 2p, 2p2
	2s 3s, 2s 3p, 2s 3d
	2p 3s, 2p 3p, 2p 3d
	3s2, 3p2, 3d2
	3s 3p, 3s 3d, 3p 3d

%comment:  gf values for transitions 19-26 and 23-26 were simply taken to be
   equal to the O V gf values reported by Hibbert, 1980, J. Phys. B, 13, 1721.
   The A values were obtained from the gf values by using the wavelengths listed.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% P.R. Young - Nov 1996

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: Zhang, Sampson, 1992, ADNDT, 52, 143
%Effective collision strengths (levels 1 - 10): Berrington, K.A., Burke, P.G., Dufton, P.L., 
   Kingston, A.E., 1985, ADNDT, 33, 195
%collision strengths (levels 11 - 46): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125
%comment: The Delta-E's for transitions between levels 1 - 10 have been taken from the observed values 
   in the .elvlc file. The gf values are from the .wgfa file.
%comment: effective collision strengths were provided in the temperature range 5.40 < LogT < 7.00
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% K.P. Dere (levels 11-46) and E. Landi (levels 1-10)  Mar 2001

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