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The CHIANTI database consists of the following primary ASCII files for this ion:
contains the energy levels in cm^(-1) It includes both experimental and theoretical values of the levels energies.
%observed energy levels (2): Smitt et al. 1976, Phys. Scripta, 13, 293 %observed energy levels (3): Combination of Smitt et al. (1976) and Shirai et al. 2000, J. Phys. Chem. Ref. Data, Mmonograph 8 %observed energy levels (4): Feldman & Doschek 2007, ADNDT, 93, 779 %observed energy levels (5): Combination of Smitt et al. (1976) and Feldman & Doschek (2007) %observed energy levels (6): Combination of Fawcett & Hayes (1972) and Borges et al. (2007) %observed energy levels (7,9,11): Combination of Fawcett & Hayes (1972), Borges et al. (2007), and Shirai et al. (2000) %observed energy levels (8): Borges et al 2007, Brazilian J. Phys., 37, 335 %observed energy levels (10,12): Combination of Borges et al. (2007) and Shirai et al. (2000) %observed energy levels (27-31): Fawcett & Hayes 1972, J. Phys. B, 5, 366 %observed energy levels (32,34,39): Combination of Fawcett & Hayes (1972) and ground configuration observed energies %observed energy levels (36): Combination of Fawcett & Hayes (1972) and Smitt et al. (1976) %Theoretical energy levels: Landi & Bhatia 2009, ADNDT, in press %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Enrico Landi - Nov 2008
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: ni_14.wgfa %observed energy levels (2): Smitt et al. 1976, Phys. Scripta, 13, 293 %observed energy levels (3): Combination of Smitt et al. (1976) and Shirai et al. 2000, J. Phys. Chem. Ref. Data, Mmonograph 8 %observed energy levels (4): Feldman & Doschek 2007, ADNDT, 93, 779 %observed energy levels (5): Combination of Smitt et al. (1976) and Feldman & Doschek (2007) %observed energy levels (6): Combination of Fawcett & Hayes (1972) and Borges et al. (2007) %observed energy levels (7,9,11): Combination of Fawcett & Hayes (1972), Borges et al. (2007), and Shirai et al. (2000) %observed energy levels (8): Borges et al 2007, Brazilian J. Phys., 37, 335 %observed energy levels (10,12): Combination of Borges et al. (2007) and Shirai et al. (2000) %observed energy levels (27-31): Fawcett & Hayes 1972, J. Phys. B, 5, 366 %observed energy levels (32,34,39): Combination of Fawcett & Hayes (1972) and ground configuration observed energies %observed energy levels (36): Combination of Fawcett & Hayes (1972) and Smitt et al. (1976) %Theoretical energy levels: Landi & Bhatia 2009, ADNDT, in press %A and gf values: Landi & Bhatia 2009, ADNDT, in press %Comment: A and gf values computed with the Flexible Atomic Code - Gu, M.F., 2003, ApJ, 582, 1241 %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Enrico Landi - Nov 2008
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_14.splups %gf values: Landi & Bhatia, 2009, in press %Collision strengths: Landi & Bhatia, 2009, in press %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Enrico Landi - Nov 2008