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

n_3.elvlc (energy levels)

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

 
%energy levels (n=2): Fuhr, J.R., et al., "NIST Atomic Spectra Database" Ver. 2.0, March 1999, NIST Physical Reference Data
%energy levels (n=3): Kelly,R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
%Theoretical energy levels: Zhang,H.L., Graziani,M., Pradhan,A.K., 1994, A&A, 283, 319
%theoretical energy levels (N III):  Stafford,R.P., Bell,K.L., Hibbert,A., 1992, J. Phys. B, 25, 5449
%comment:  energy levels renumbered
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E.Landi and P.R.Young - 8-Dec-2003
 

n_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.

 
%filename: n_3.wgfa
%energy levels (n=2): Fuhr, J.R., et al., "NIST Atomic Spectra Database" Ver. 2.0, March 1999, NIST Physical Reference Data
%energy levels (n=3): Kelly,R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
%A-values (ground transition): Nussbaumer H., Storey, 1979, A&A, 71, L5
%Allowed transitions for decays from 2s.2p2, 2s2.3s and 2s2.3d to the ground 2s2.2p configuration:
   Correge, G., Hibbert, A., 2002, J.Phys.B, 35, 1211
%Allowed transitions for all other transitions: Tachiev, G., & Froese Fischer, C., 2000, J.Phys.B, 33, 2419
%comment: The table below compares A-values from the previous CHIANTI model (A_1),
   with the new model (A_2), where differences are greater than 30%. Significant
   differences are seen for the intercombination lines, and for some of the n=3
   levels.
   Also, two new (weak) transitions are present in the new model (8-12, 5-13).

  i  j       wvl       A_1       A_2   %diff
  1  3  1748.652 2.52e+002 3.49e+002   38.61
  1  4  1746.820 4.47e+000 8.90e+000   99.02
  2  3  1753.989 2.54e+002 3.63e+002   42.76
  2  4  1752.145 4.36e+001 6.17e+001   41.49
  2  5  1749.662 1.76e+002 2.72e+002   54.32
  9 18  1001.752 7.21e+005 2.82e+005  -60.87
  9 17  1002.112 2.64e+006 9.52e+005  -63.94
 10 17  1003.218 1.40e+006 5.22e+005  -62.71
 10 18  1002.857 3.41e+006 1.25e+006  -63.37
 14 19  2714.711 1.41e+006 6.26e+005  -55.61
 15 19  2715.227 2.82e+005 1.25e+005  -55.82
 15 20  2714.814 1.70e+006 7.52e+005  -55.75

% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%   P.R.Young - 12-Dec-03

n_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: n_3.splups
%oscillator strengths: Stafford, R.P., Hibbert, A., Bell, K.L., 1993, MNRAS, 260, L11
%effective collision strengths: Stafford, R.P., Bell, K.L., Hibbert, A., 1994, MNRAS, 266, 715
%comment: effective collision strengths were provided in the temperature range 4.0 < Log T < 5.2
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% K.P. Dere 1994

n_3.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: n_3.psplups
%rates: Foster VJ, Keenan FP, Reid RHG, ADNDT 67, 99, 1997
%energies: From .elvlc file, experimental energies
%comment: The rate coefficients are in units cm^3/s.
%comment: Fits valid for temperatures 8e3 to 1e5 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   15-May-2001

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

n_3_table.html (html table)


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