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

al_12.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: Sampson, D.H., Goett, S.J., Clark, R.E.H., 1983, ADNDT, 29, 467
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E.Landi and K.P.Dere 2002
 

al_12.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.

 
%filename: al_12.wgfa
%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.
%oscillator strengths (up to 3-37): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1983, ADNDT, 29, 467, Hydrogenic values
%oscillator strengths from 4-8 to end of file: Wiese, W.L., Smith, M.W., Glennon, B.M., 
    1966, Atomic Transition Probabilities, NSRDS-NBS-4
%oscillator strengths (1 - 13, 1 - 23): Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995,
    NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61
%A values (1-2,5,6; 2-4,5,6): Lin, C.D., Johnson, W.R., Dalgarno, A., Phys Rev A, 1977, 15, 154
%A values (1-3;2 phot): Drake, G.W.F., Phys Rev A, 1986, 34, 2871
%comment: hydrogenic f values
%comment: correction (Nov 2003) for A and gf value of transition 1-7. It affects the line at 7.7573 A.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% K.P.Dere and E.Landi - Jan 2005

al_12.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: al_12.splups
%oscillator strengths: Sampson, D.H., Goett, S.J., Clark, R.E.H., 1983, ADNDT, 29, 467, Hydrogenic values
%effective collision strengths transitions (1-2,3,4,5,6,7): interpolated using O VII, Ne IX, Mg XI, Si XIII, S XV, Ar XVII and Ca XIX
%collison strengths all other transitions: Sampson, D.H., Goett, S.J., Clark, R.E.H.  1983, ADNDT, 29, 467
%comment: Sampson et al collision strengths are hydrogenic values
%comment: The interpolated values differ from the Sampson et al values by 25% at maximum. They've been
inserted to take into account resonances from Zhang & Sampson 1987, available in all the other ions.
%comment: Interpolated effective collision strengths are most reliable in the temperature range 5.9 < log T < 7.4
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% K.P. Dere and E. Landi - Jan 2005

al_12.splups (proton collisional data) Not available in this VERSION.

al_12.reclvl (total recombination population rates)

 
%filename: al_12.reclvl
%Radiative recombination rates: Mewe, R, Gronenschild, E.H.B.M, and van den Oord, G.H.J, 1982, A&AS, 62, 197
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% E. Landi - Aug 2006

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

al_12_table.html (html table)


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