N II - VERSION 11.0

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

n_2.elvlc (energy levels)

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

 
%filename:  n_2.elvlc
%Theoretical energy levels (1-58):  Tayal, S. S., 2011, ApJS, 195,12
http://adsabs.harvard.edu/abs/2011ApJS..195...12T

%Observed energy levels:  Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/asd [2012, September 14]. National Institute of Standards and Technology, Gaithersburg, MD.

%produced as a part of the  'CHIANTI' atomic database for astrophysical spectroscopy
 K. Dere (GMU) - 2012 October 05

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_2.wgfa.tayal.tachiev.nist5.young

%Theoretical A-values levels (1-58):  Tayal, S. S., 2011, ApJS, 195,12
http://adsabs.harvard.edu/abs/2011ApJS..195...12T

%Theoretical A-values (levels 1-5):  Tachiev, G., Froese Fischer, C., 2001, Canadian Journal of Physics, 79, p.955-976
http://adsabs.harvard.edu/abs/2001CaJPh..79..955T

%Observed wavelengths:  Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/asd [2012, September 14]. National Institute of Standards and Technology, Gaithersburg, MD.

%Observed wavelengths (2-5, 4-5, 2-6):  Young, P.R., Feldman, U., Lobel, A., 2011, ApJS, 196, 23
ADSref:  http://adsabs.harvard.edu/abs/2011ApJS..196...23Y

produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy consortium
K. Dere (GMU) - 2012 March 19
 minimum branching ratio =   1.00e-04
%File processed with wgfa_tidy by pryoung on  6-Mar-2019
%File processed with wgfa_tidy by pryoung on 31-May-2023

n_2.scups (electron collision data)

contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

 
 K. Dere (GMU) - 2012 January 10                                                  
produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
effective collision strengths were provided between 5.0e+2 and 1.e+5 K            
http://adsabs.harvard.edu/abs/2011ApJS..195...12T                                 
%Collision strengths:  Tayal, S. S., 2011, ApJS, 195,12                           
%filename:  n_2.upsdat

n_2.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: n_2.psplups
%rates: Ryans R.S.I., Foster-Woods V.J, Keenan F.P., Reid R.H.G., 1999, ADNDT 73, 1-42
%energies: Wiese W.L., Fuhr J.R., Deters T.M., 1996, J. Phys. Chem. Ref. Data, Monograph 7
%comment: Fits valid for temperatures 8e3 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

n_2_table.html (html table)