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

mg_9.elvlc (energy levels)

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

 
%observed 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 (1-10): Zhang, Sampson, ADNDT, 1992, 52, 143
%theoretical energy levels (11-46): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125.
%comment:  NIST values for levels 28 (E4) and 31 (F3) are uncertain
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%   K.P. Dere, Jan. 1996
 

mg_9.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.

 
%observed 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 (1-10): Zhang, Sampson, ADNDT, 1992, 52, 143
%theoretical energy levels (11-46): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125
%A-values: computed using a SSTRUCT model by P.R.Young
%comment: A-values computed using a 15 configuration model of the ion. 
    The following configs were included:

        2s2, 2s 2p, 2p2
        2s 3s, 2s 3p, 2s 3d
        2p 3s, 2p 3p, 2p 3d
        3s2, 3p2, 3d2
        3s 3p, 3s 3d, 3p 3d

    For the levels with no observed energies, `best-guess' SSTRUCT energies were 
    used, which are more accurate than those derived from the theoretical 
    energies in the .elvlc file.

    A crucial aspect of this new data is the availability of allowed transitions 
    to de-populate the 3p.3p 3F4 level (level 26) which was previously metastable.

%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%   P.R.Young  Jul 1998

mg_9.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: mg_9.splups
%oscillator strengths: SUPERSTRUCTURE calculations from P.R> Young (see mg_9.wgfa for details)
%effective collision strengths (levels 1 to 10): Keenan et al., Physica Scripta 34, 216, 1986
%collision strengths (levels 11 to 46): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125
%comment: the upsilons were calculated in the temperature range  5.2 < Log T < 6.8
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%   Peter Young, Apr 1999

mg_9.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: mg_9.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: CHIANTI database, ver.1, Dere et al., A&AS 125, 149, 1997
%comment: Fit valid for temp. range 1e5 to 3e7 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young  19-Oct-00

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

mg_9_table.html (html table)


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