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)

S IX - VERSION 4.2

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

  1. s_9.elvlc (energy levels)

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

     
%observed energy levels (n=2,3 levels): Fuhr, J.R., et al., "NIST Atomic Spectra Database" ver. 2.0
    March 1999. NIST Physical Reference Data
%observed energy levels (levels 11,12,71,77): Kelly,R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
%observed energy levels (levels 23,24,38->40,46,57,59-60,63,75): Jupen, C., Engstrom, L., 1997, Phys.Scr., 56, 592
%observed energy levels (levels 17->21,28-29,31-34,41-42,61-62): Kink, I., Jupen, C., Engstrom, L., 
    Feldman, U., Laming, M.J., Schuhle, U., 1997, ApJ, 487, 956
%theoretical energy levels (n=2,3 levels): Bhatia, A.K., Landi, E., 2002, ADNDT, in press
%Comment: The energies of levels 81 and 84 (2p3.(2P).3d 1D2 and 3D2 respectively) have been
           exchanged to correctly match theoretical energies.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%E. Landi - Sep 2001

  2. s_9.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. 

     
%observed energy levels (n=2,3 levels): Fuhr, J.R., et al., "NIST Atomic Spectra Database" ver. 2.0
     March 1999. NIST Physical Reference Data
%observed energy levels (levels 11,12,71,77): Kelly,R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
%observed energy levels (levels 17->21,23,24,28,29,31->34,38->42,46,57,59->63,75): Jupen, C.,
     Engstrom, L., 1997, Phys.Scr., 56, 592
%theoretical energy levels (n=2,3 levels): Bhatia, A.K., Landi, E., 2002, ADNDT, in press
%Radiative data: Bhatia, A.K., Landi, E., 2002, ADNDT, in press
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Oct 2001

  3. s_9.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: s_9.omdat
%oscillator strengths: Bhatia, A.K., Landi, E., 2002, ADNDT, in press
%collision strengths: Bhatia, A.K., Landi, E., 2002, ADNDT, in press
%produced as part of the Arcetri/Cambridge/NRL "CHIANTI" atomic database collaboration
%
% E. Landi - Sep 2001

  4. s_9.psplups (proton collision data)

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

     

%file: s_9.psplups
%rates: Ryans R.S.I., Keenan F.P., Reid R.H.G., unpublished.
%energies: Observed values, from .elvlc file
%comment: Fits valid for temperatures 3e5 to 1e7 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

    s_9_table.html (html table)


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