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

ne_3.elvlc (energy levels)

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

 
%observed energy levels: Fuhr, J.R., et al., 1999, "NIST Atomic Spectra Database" ver. 2.0 
    March 1999. NIST Physical Reference Data
%theoretical energy levels (ground levels): McLaughlin, B.M., Bell K.L., 2000, J.Phys.B, 33, 597
%theoretical energy levels (2s.2p5 and n=3 levels): Bhatia, A.K., Thomas, R.J., Landi, E., 2002, ADNDT, in press
%theoretical energy levels (2p6 1S0 - level 58): Bhatia, A.K., private communications
%comment: McLaughlin & Bell energies are in LS coupling. For this reason levels 2 and 3 theoretical energies
          are identical to the experimental ones.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi Mar 2001
 

ne_3.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: Fuhr, J.R., et al., "NIST Atomic Spectra Database" ver. 2.0
    March 1999. NIST Physical Reference Data
%theoretical energy levels (ground levels): McLaughlin, B.M., Bell K.L., 2000, J.Phys.B, 33, 597
%theoretical energy levels (2s.2p5 and n=3 levels): Bhatia, A.K., Thomas, R.J., Landi, E., 2002, ADNDT, in press
%comment: McLaughlin & Bell energies are in LS coupling. For this reason levels 2 and 3 theoretical energies
          are identical to the experimental ones.
%Oscillator strengths (n=3): Bhatia, A.K., Thomas, R.J., Landi, E., 2002, ADNDT, in press
%oscillator strengths (level 58 - 2p6 1S0): Bhatia A.K. (private communications)
%A-values (levels 1 to 5): Galavis M., Mendoza C., Zeippen C.J., 1997, A&AS, 123, 159
%A-values (transitions 2-5, 4-5): Daw A., Parkinson W.H., Smith P.L., Calamai A.G., 2000, ApJ, 533, 179
%comment:
    The A-values from Daw et al. are experimentally determined and have
    accuracies of +/- 9% (2-5) and +/- 7% (4-5).
%comment: added radiative data for transitions originating from level 11, missing in 4.02. This allows CHIANTI
          to predict a few new lines in the EUV. Effects on level populations are minimal at all densities 
          (Nov 2003).
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi Sep 2003, P.R.Young (n=2 transition probabilities) Mar 2000

ne_3.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: ne_3.splups
%oscillator strengths: Bhatia, A.K., Landi, E., 2002, ADNDT, in press
%effective collision strengths ground configuration: McLaughlin B.M., Bell K.L., 2000, J.Phys.B, 33, 597
%collision strengths all other transitions: Bhatia, A.K., Landi, E., 2002, ADNDT, in press
%collision strengths for level 58: Bhatia A.K. (private communications)
%comment: energies for the ground configuration transitions are from the observed values in the .elvlc file
%comment: effective collision strengths are provided in the temperature range 3.0 < Log T < 6.0
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi and P.R.Young - Aug 2001

ne_3.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: ne_3.psplups
%rates: Ryans R.S.I., Keenan F.P., Reid R.H.G., unpublished.
%energies: Observed values, from .elvlc file
%comment: Fits valid for temperatures 2e4 to 1e6 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   15-May-2001

---

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

ne_3_table.html (html table)


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