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

mg_6.elvlc (energy levels)

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

 
%Observed energy levels (1-15): Edlen, 1984, Phys.Scripta, 30, 135 
%Observed energy levels (16-23): Martin,W.C., Sugar,J., Musgrove,A., Dalton,G.R., 1995,  
   NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Data base 61.
%Theoretical energy levels (1-15): Zhang, Sampson, ADNDT, 1999, 72, 153
%Theoretical energy levels (16-23): Bhatia AK, Young PR, 1998, ADNDT, 68, 219
%comment: NIST v.2 has the same values as v.1, and does not provide a an 
 observed energy for level 21 so will use 
 a "best guess" for this energy in column 3 (P.R. Young June 1997)
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
% 
% G. Del Zanna, 2001.
 

mg_6.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.

 
% Experimental energy levels (1- 15): Edlen, 1984, Phys.Scripta, 30, 135
% Theoretical energy levels: Bhatia A.K., Young P.R., 1998, ADNDT, 68, 219
% gf values for transitions between the (1- 15) levels: Zhang, Sampson, ADNDT, 1999, 72, 153
% A values for transitions with 2s.2p4 and 2p5: Zhang, Sampson, ADNDT, 1999, 72, 153
% A values for transitions within the ground level: Merkelis et al., 1999, Physica Scripta 59,122
% A values for forbidden transitions with 2s.2p4 and 2p5: Merkelis et al., 1999, Physica Scripta 59, 122
% A and gf values for transitions with n=3 levels: Bhatia A.K., Young P.R., 1998, ADNDT, 68, 219
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% G. Del Zanna, May 2001

mg_6.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_6.splups
%oscillator strengths (up to level 15): Zhang, Sampson, 1999, ADNDT, 72, 153
%oscillator strengths (levels above 15): Bhatia A.K., Young P.R., 1998, ADNDT, 68, 219
%collision strengths (up to level 15): Zhang, Sampson, 1999, ADNDT, 72, 153
%collision strengths (levels above 15): Bhatia A.K., Young P.R., 1998, ADNDT, 68, 219
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% G. Del Zanna, 2001 (1-15) and P.R. Young June 1997 (15-23). 

mg_6.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: mg_6.psplups
%rates: Bhatia, A.K. & Young, P.R. 1998, ADNDT 68, 219
%energies: Observed values from CHIANTI mg_6.elvlc file.
%comment: Fitted using single_temp.pro with scalx=0.9.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young  17-Dec-2001

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

mg_6_table.html (html table)


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