Fe XI - VERSION 5.1

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

• fe_11.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: NIST Database for Atomic Spectroscopy, Version 1.0, 
    NIST Standard Reference Database 61, 1995.
  %observed energy levels (12,13,41): Jupen et al., MNRAS, 264, 627, 1993
  %theoretical energy levels 1-9: Gupta & Tayal, 1999, ApJ, 510, 1078
  %theoretical energy levels: Bhatia & Doschek 1996, ADNDT, 64, 183
  %comment: The third column of energies contains scaled superstructure values.
  %comment: Have had problems with the identification of some of the Fe XI
     lines. The following are proposed.
  
     Level 37 has been proposed as giving the 188.30 line (Jupen et
     al.). Don't think this is right, as the 3P2 - 3S1 transition is
     quite weak. Can not find any lines which correspond to the 3S1
     transitions, so have put the scaled superstructure value in.
  
     Level 38 (3P2) is identified from the strong line at 188.23.
  
     Level 39 (1P1) is identified as the strong line at 188.30.
  
     There's only one line from level 40 (3P0), whose identification
     I'm uncertain about (near 189.10 AA?). Have used the scaled 
     superstructure energy relative to the 3P1 level.
  
     Level 41 (3P1) has been identified from the 184.704 line seen by
     Jupen et al., two other transitions from this level match up
     nicely with the 189.123 and 189.733 lines seen by Behring et
     al.(1976).
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  %  P.R. Young  Feb. 1996 & Enrico Landi Apr. 1999
  

  
  

• fe_11.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: NIST Database for Atomic Spectroscopy, Version 1.0,
    NIST Standard Reference Database 61, 1995.
  %observed energy levels (12,13,41): Jupen et al., MNRAS, 264, 627, 1993
  %theoretical energy levels 1-9: Gupta & Tayal, 1999, ApJ, 510, 1078
  %theoretical energy levels: Bhatia & Doschek 1996, ADNDT, 64, 183
  %A values: obtained from a 13 configuration model of Fe XI used in "superstructure", 
  %comment: the configurations used were:
  
  	3s2 3p4, 3s 3p5, 3s2 3p3 3d, 3p6
  	3s2 3p3 {4s, 4p, 4d, 4f}
  	3s 3p4 3d, 3s2 3p2 3d2
  	3p5 3d, 3s 3p3 3d2, 3s2 3p 3d3
  
     The most striking difference between this model and the 4 conf
     model occurs for the (2D*) 3P1, 3S1 and 1P1 levels. Essentially,
     the 3S1 level is pushed closer to the other two levels,
     increasing the amount of interaction between them. The data
     below, from "superstructure" shows this.
  
     The first column gives the levels; the second and third the
     theoretical energies for the 4 conf model and the 13 conf model;
     the next three columns give the percentage contributions of the
     three levels to each other: "a/b" means a is percentage for 4
     conf model, while b is percentage for 13 conf model.
  
  				3S1	3P1	1P1
  	3S1	532878	547264	97/71	-/-	-/10
  	3P1	555764	553263	1/14	50/42	11/7
  	1P1	564755	542936 	-/12	21/16	17/16
  
     Clearly the change of energies gives rise to different
     interactions. Most notably, 1P1 starts mixing with 3S1, whereas
     it did not before
  
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % Peter Young    Jul 2000.
  

  
  

• fe_11.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: fe_11.splups
  %oscillator strengths: obtained from a SUPERSTRUCTURE calculation (see fe_11.wgfa for details)
  %effective collision strengths levels 1-9: Gupta & Tayal, 1999, ApJ, 510, 1081
  %collision strengths: Bhatia, A.K., Doschek, G.A., 1996, ADNDT, 64, 183
  %comment: effective collision strengths were provided in the temperature range 5.7 < Log T < 6.7
  %comment:
     Selected transitions have been fitted in order to reproduce the 
     level balance of the complete collisional data. Essentially all 
     significant collision strengths involving the levels 1-5 and 
     14,20,23,24,25,30.
  
     This file contains fits to the SCALED Bhatia omega data. It was
     found that the 4 configuration collisional model does not
     accurately predict some important collision strengths, so it was
     decided to scale all the 3s2 3p2 - 3s2 3p 3d collision strengths
     (for which there was a corresponding oscillator strength) by the
     factor:
  
  	(accurate "superstructure" oscillator strength)
  	-----------------------------------------------
  	     (original Bhatia oscillator strength)
  
     In particular, this improves the agreement of the 188.22, 188.30 lines
     with theory.
  %
  % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % P.R.Young Aug 1997 and E.Landi Apr 1999
  

  
  

• fe_11.psplups (electron collision data)

  contains the spline fits to the scaled proton collision strengths.

  References:

  
  %filename: fe_11.psplups
  %rates: Landman, D.A., ApJ 240, 709, 1980
  %energies: Observed energies from CHIANTI .elvlc file
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % Peter Young   13-Jun-2001
  

  
  

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

  
  

• fe_11_table.html (html table)