| Home | Download | Help | User Guides | Direct access | News - History | Applications |
|---|---|---|---|---|---|---|
| Team | Line Lists | Links | ADS Citations | Acknowledging CHIANTI | CHIANTI papers | CHIANTI and other codes |
The CHIANTI database consists of the following primary ASCII files for this ion:
contains the energy levels in cm^(-1) It includes both experimental and theoretical values of the levels energies.
%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
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: fe_11.wgfa
%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
%comment: The wavelengths for the transitions from level 37 have been changed to be
consistent with the energy of level 37 in the third column of the .elvlc
file (PRY 13-Nov-2008)
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young - Nov 2008
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: 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
contains the spline fits to the scaled proton collision strengths.
%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