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

n_4.elvlc (energy levels)

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

 
%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: Ramsbottom, C.A., Berrington, K.A., Hibbert, A., Bell, K.L.,
   Pyhs.Scripta, 1994, 50, 246
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Enrico Landi 1996
 

n_4.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_4.elvlc
%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.
%A-values: Tachiev, G. & Froese Fischer, C., 1999, J.Phys.B, 32, 5805
%A-values (transition 1-9): Kingston, A.E., Hibbert, A., 2001, J.Phys.B, 34, 81
%A-values (transitions 5-13, 8-13, 4-14, 3-15, 4-15, 2-16, 3-16, 4-16): P.R. Young, 9-Jun-2006, calculation with SSTRUCT.
%comment: The Tachiev & Froese Fischer calculation did not cover all transtions
   for N IV, and so they have been supplemented with data from Kingston & Hibbert 
   and P.R. Young.  
   The SSTRUCT calculation used a 17 configuration model of the ion, and
   term energy corrections were applied. Observed energies were used in the
   calculation of the A-values.
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young - 12-Jun-2006

n_4.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_4.splups
%oscillator strengths: SUPERSTRUCTURE calculations by P.R.Young
%effective collision strengths: Ramsbottom, C.A., Berrington, K.A., Hibbert, A., Bell, K.L., Pyhs.Scripta, 1994, 50, 246
%comment: The transitions between levels 1-4 and levels 2-10 have been re-fit
   using 9 point splines to better reproduce the low temperature behaviour.
   These fits are accurate to < 1.22 % over the range 3.1 < log T < 5.6
   All remaining fits are valid over the range 4.0 < Log T < 6.0.
% Comment: updated with 9 point spline fits (PRY 12-Jun 2006)
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young and Enrico Landi - 12-Jun-2006

n_4.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: n_4.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: Wiese W.L., Fuhr J.R., Deters T.M., 1996, J. Phys. Chem. Ref. Data, Monograph #7
%comment: Fits valid for temperatures 4e4 to 3e6 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young  23-Mar-01

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

n_4_table.html (html table)


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