Mg IX - VERSION 5.1

The CHIANTI database consists of 4 primary ASCII files for each ion in the database.

• mg_9.elvlc (energy levels)

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

  References:

  %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 for each transition. Wavelengths are based on experimental level energies where available; wavelengths calculated from theoretical energies are less accurate and are given as negative values.

  References:

  %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 to 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.

  References:

  
  %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 (electron collision data)

  contains the spline fits to the scaled proton collision strengths.

  References:

  
  %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
  

  
  

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

  
  

• mg_9_table.html (html table)