CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.

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Naval Research Laboratory (USA) - Rutherford Appleton Laboratory (UK)
University of Cambridge (UK) - George Mason University (USA) - Universita' degli Studi di Firenze (Italy)

Ni XII - VERSION 4.2

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

  1. ni_12.elvlc (energy levels)

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

     
% Experimental 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:
         3s2 3p5, 3s 3p6,
         3s2 3p4 3d,  3s 3p5 3d,  3p6 3d,
         3s2 3p3 3d2, 3s 3p4 3d2, 3p5 3d2,
         3s2 3p2 3d3, 3s 3p3 3d3, 3p4 3d3,
         3s2 3p4 4s,  3s2 3p4 4d, 3s2 3p4 4f
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data collaboration
%
% E. Landi 1998

  2. ni_12.wgfa (radiative data)

    3. 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. 

     
% Experimental 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 and radiative transition probabilities: SUPERSTRUCTURE calculations
%comment: the SUPERSTRUCTURE has been carried out with the following configurations:

         3s2.3p5, 3s.3p6,
         3s2.3p4.3d,  3s.3p5.3d,  3p6.3d,
         3s2.3p3.3d2, 3s.3p4.3d2, 3p5.3d2,
         3s2.3p2.3d3, 3s.3p3.3d3, 3p4.3d3,
         3s2.3p4.4s,  3s2.3p4.4d, 3s2.3p4.4f

% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data collaboration
%
% E. Landi 1998

  3. ni_12.splups (electron collision data)

    4. 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: ni_12.splups
%Oscillator strengths: calculated using SUPERSTRUCTURE, see file ni_12.wgfa
%effective collision strengths: Matthew, Ramsbottom, Bell, Keenan, ApJ, 491, 415
%comment: effective collision strengths were provided in the temperature range 3.2 < Log T < 6.6
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Enrico Landi 1998

  4. ni_12.psplups (proton collision data)

    5. contains the spline fits to the scaled proton collision strengths. 

     

%filename: ni_12.psplups
%rates: Bely, O., Faucher, P., 1970, A&A 6, 88
%energies: Observed energies from .elvlc file.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   11-Jun-2001

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

    ni_12_table.html (html table)


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