The CHIANTI database has 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.
%filename: fe_18.elvlc %Observed energies (levels up to n=4):Del Zanna,G . 2006, Astron. Astroph. 459, 307 %Observed energies (n=5 levels): Landi & Phillips 2005, ApJS, 160, 286 %Observed energy level above ionization: Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175 %Theoretical energies (levels up to n=4): Witthoeft, M.C., Badnell, N.R., Del Zanna, G., Berrington, K.A., and Pelan, J.C. 2006, Astron. Astroph. 446, 361 %Theoretical energies (n=5 levels): Landi & Gu, 2006, ApJ, 640, 1171 % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % G. Del Zanna and Enrico Landi - Oct 2008 % February 2018 observed energy of level 337 replaced by observed value of Rudolph, J. K.; Bernitt, S.; Epp, S. W.; Steinbrugge, R.; Beilmann, C.; Brown, G. V.; Eberle, S.; Graf, A.; Harman, Z.; Hell, N.; Leutenegger, M.; Mueller, A.; Schlage, K.; Wille, H.-C.; Yavas, H.; Ullrich, J.; Crespo Lopez-Urrutia, J. R. X-Ray Resonant Photoexcitation: Linewidths and Energies of K-alpha Transitions in Highly Charged Fe Ions Physical Review Letters, vol. 111, Issue 10, id. 103002 DOI: 10.1103/PhysRevLett.111.103002 adsRef: http://adsabs.harvard.edu/abs/2013PhRvL.111j3002R theoretical energy of level 337 from optimized calculation with AUTOSTRUCTURE A Breit-Pauli distorted wave implementation for AUTOSTRUCTURE Badnell, N.R., 2011, Computer Physics Communications, 182, 1528 ADSref: http://adsabs.harvard.edu/abs/2011CoPhC.182.1528B using the Rudolph observed energy for optimimzation produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy K. Dere (GMU) - 2018 February 20 %comment: Fixed text problems in comments. No change to data. Peter Young, 25-Jul-2019
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_18.wgfa %Observed energies (levels up to n=4): Del Zanna, G. 2006, Astron. Astroph. 459, 307 %Observed energies (n=5 levels): Landi & Phillips 2005, ApJS, 160, 286 %Theoretical energies (levels up to n=4): Witthoeft, M.C., Badnell, N.R., Del Zanna, G., Berrington, K.A., and Pelan, J.C. 2006, Astron. Astroph. 446, 361 %Theoretical energies (n=5 levels): Landi & Gu, 2006, ApJ, 640, 1171 %observed energy level above ionization: Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175 %A-values (levels up to n=4): Del Zanna, G.: 2006, Astron. Astroph. 459, 307 %A-values (n=5 levels): Landi & Gu, 2006, ApJ, 640, 1171 % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % G. Del Zanna - Oct 2008 minimum branching ratio = 1.00e-05 % February 2018 revised transitions of 337 -> 1,2 Theoretical gf and A-values: Autostructure calculation A Breit-Pauli distorted wave implementation for AUTOSTRUCTURE Badnell, N.R., 2011, Computer Physics Communications, 182, 1528 ADSref: http://adsabs.harvard.edu/abs/2011CoPhC.182.1528B optimized by the observed energy of level 337 of Rudolph, J. K.; Bernitt, S.; Epp, S. W.; Steinbrugge, R.; Beilmann, C.; Brown, G. V.; Eberle, S.; Graf, A.; Harman, Z.; Hell, N.; Leutenegger, M.; Mueller, A.; Schlage, K.; Wille, H.-C.; Yavas, H.; Ullrich, J.; Crespo Lopez-Urrutia, J. R. X-Ray Resonant Photoexcitation: Linewidths and Energies of K-alpha Transitions in Highly Charged Fe Ions Physical Review Letters, vol. 111, Issue 10, id. 103002 DOI: 10.1103/PhysRevLett.111.103002 adsRef: http://adsabs.harvard.edu/abs/2013PhRvL.111j3002R produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy K. Dere (GMU) - 2018 February 20 %File processed with wgfa_tidy by pryoung on 6-Mar-2019 %comment: Fixed text problem in comments. No change to data. Peter Young, 25-Jul-2019 %File processed with wgfa_tidy by pryoung on 31-May-2023
contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).
% G. Del Zanna - Oct 2008 % % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration %comment: effective collision strengths for levels above ionization are given in the range 6.46e4 < T < 1.62e7 %comment: only excitations from the lowest three levels to the n=4 states are retained. %effective collision strengths (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171 %collision strengths (n=5 levels): Landi & Gu, 2006, ApJ, 640, 1171 %effective collision strengths (levels up to n=4): Witthoeft, M.C., Badnell, N.R., Del Zanna, G., Berrington, K.A., and Pelan, J.C. 2006, Astron. Astroph. 446, 361. %oscillator strengths (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171 %oscillator strengths (n=5 levels): Landi & Gu, 2006, ApJ, 640, 1171 %oscillator strengths (levels up to n=4): Witthoeft, M.C., Badnell, N.R., Del Zanna, G., Berrington, K.A., and Pelan, J.C., 2006, Astron. Astroph. 446, 361 %filename: fe_18.splups
contains the spline fits to the scaled proton collision strengths.
%filename: fe_18.psplups %rates: Foster V.J, Keenan F.P., Reid R.H.G., 1994, Phys. Rev. A 49, 3092-3095 %energies: Reader J., Sugar J., 1975, J.Phys.Chem.Ref.Data 4, 353 %comment: Fit valid for temperatures 2e6 to 2.5e8 K. %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Peter Young 16-May-2001
%filename: fe_18.ci %Collisional ionization population rate: Gu, M.F., 2003, ApJ, 582, 1241 %produced as part of the Arcetri/Cambridge/NRL CHIANTI atomic data base collaboration % % Enrico Landi - Feb 2004
Page created by Giulio Del Zanna on Mon Jun 26 11:16:09 2023