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_22.elvlc Theoretical energy levels: 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 Autostructure calculation optimized with 'SHFTIC' file using energy corrections from the following sources: Observed energy levels: Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/asd [2012, September 14]. National Institute of Standards and Technology, Gaithersburg, MD. %experimental energies 518, 519: 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) - 2017 December 29 %comment: Fixed text problem 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_22.wgfa.e1e2.imp5 Theoretical wavelengths, gf, 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 Autostructure calculation optimized with 'SHFTIC' file using energy corrections from the following sources: Observed energy levels: Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/asd [2012, September 14]. National Institute of Standards and Technology, Gaithersburg, MD. %experimental energies 518, 519: 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 Lóopez-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 Observed wavelength 1-2: Feldman, U.; Curdt, W.; Landi, E.; Wilhelm, K. Identification of Spectral Lines in the 500-1600 Å Wavelength Range of Highly Ionized Ne, Na, Mg, Ar, K, Ca, Ti, Cr, Mn, Fe, Co, and Ni Emitted by Flares (Te>=3×106 K) and Their Potential Use in Plasma Diagnostics 2000ApJ...544..508F adsRef: http://adsabs.harvard.edu/abs/2000ApJ...544..508F DOI: 10.1086/317203 sorted by lvl12 elvlcName = fe_22.elvlc wgfaName = fe22.wgfa.e1e2.sorted allWvl = 1 minDiff = 0.00010 wavelengths determined from energy levels produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy K. Dere (GMU) - 2019 February 07 minimum branching ratio = 1.00e-04 2019 February 07 %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).
%comment: Fixed text problem in comments. No change to data. Peter Young, 25-Jul-2019 fe_23 IP ev = 1.95858e+03 Ip invcm = 15797000.000 Ip Ryd = 143.95285 fe_22 IP ev = 1.79901e+03 Ip invcm = 14510000.000 Ip Ryd = 132.22485 K. Dere (GMU) - 2017 December 29 adsRef: http://adsabs.harvard.edu/abs/2013PhRvL.111j3002R DOI: 10.1103/PhysRevLett.111.103002 Physical Review Letters, vol. 111, Issue 10, id. 103002 X-Ray Resonant Photoexcitation: Linewidths and Energies of K-alpha Transitions in Highly Charged Fe Ions 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 Lóopez-Urrutia, J. R. %experimental energies 518, 519: Observed energy levels: Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/asd [2012, September 14]. National Institute of Standards and Technology, Gaithersburg, MD. Autostructure calculation optimized with 'SHFTIC' file using energy corrections from the following sources: ADSref: http://adsabs.harvard.edu/abs/2011CoPhC.182.1528B Badnell, N.R., 2011, Computer Physics Communications, 182, 1528 A Breit-Pauli distorted wave implementation for AUTOSTRUCTURE Theoretical energy levels: Autostructure calculation 2018 December 10 levels renumbered by K. Dere % Enrico Landi - Mar 2005 % %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration %comment: data from Badnell & Griffin have been adapted to the level ordering given by the Flexible Atomic Code %comment: effective collision strengths from Badnell et al. (2001) are used in the temperature range 6.4 < Log T < 8.0 %collisional data (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171 %Collision strengths (205-513): Landi & Gu, 2006, ApJ, 640, 1171 %effective collision strengths (1-204): Badnell, N.R., Griffin, D.C., Mitnik, D.M., 2001, J.Phys.B, 34, 5071 %oscillator strengths (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171 %oscillator strengths (205-513): Landi & Gu, 2006, ApJ, 640, 1171 %oscillator strengths (1-204): Badnell, N.R., Griffin, D.C., Mitnik, D.M., 2001, J.Phys.B, 34, 5071 %filename: fe_22.splups filename fe_22.scups_rnmbr
contains the spline fits to the scaled proton collision strengths.
%filename: fe_22.psplups %rates: Foster VJ, Keenan FP, Reid RHG, ADNDT 67, 99, 1997 %energies: From .elvlc file, experimental energies %comment: The rate coefficients are in units cm^3/s. %comment: Fits valid for temperatures 2e6 to 6e7 K. %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Peter Young 15-May-2001
%filename: fe_22.cilvl %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
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