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_19.elvlc Observed energies: 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 [2013, May 3]. National Institute of Standards and Technology, Gaithersburg, MD. Theoretical energies: Butler, K. & Badnell, N. R. 2008, A&A, 489, 1369 Levels 343-630 are from CHIANTI v.7.1: Theoretical energy levels (below ionization): Landi & Gu, 2006, ApJ, 640, 1171 Produced for the CHIANTI database v.8 by G. Del Zanna Mar 2014 revised in Feb 2018 by K. Dere 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 optimized through an ISHFTIC file with the observed energies of: NIST for levels 1-10 and , for levels 631 and 632: 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 19 %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_19.wgfa Observed energies: 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 [2013, May 3]. National Institute of Standards and Technology, Gaithersburg, MD. Theoretical energies: Butler, K. & Badnell, N. R. 2008, A&A, 489, 1369 Levels 343-630 are from CHIANTI v.7.1: observed energy levels (above ionization): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A&A, 403, 1175 Theoretical energy levels (below ionization): Landi & Gu, 2006, ApJ, 640, 1171 Radiative data (below ionization): Landi & Gu, 2006, ApJ, 640, 1171 Produced for the CHIANTI database v.8 by G. Del Zanna Mar 2014 Revised in Feb 2018 by K. Dere Theoretical energy levels, oscillator strengths and A values for transitions from autoionizing 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 optimized through an ISHFTIC file with the observed energies of: NIST for levels 1-10 and , for levels 631 and 632 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 19 minimum branching ratio = 1.00e-05 %File processed with wgfa_tidy by pryoung on 6-Mar-2019 %comment: Fixed text problems 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).
Modified by G. Del Zanna on 2018 Oct 30 to fix the high-energy extrapolation of the Butler & Badnell data. Produced for the CHIANTI database v.8 by G. Del Zanna Mar 2014 Collisional data (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171 Collision strengths (343-630) computed with the Flexible Atomic Code - Gu, M.F., 2003, ApJ, 582, 1241 oscillator strengths (above ionization): Bautista, M.A., Mendoza, C., Kallman, T.R., Palmeri, P., 2004, A&A, 418, 1171 The data for levels 343-636 are from CHIANTI v.7.1: Levels 1-342: data from Butler & Badnell A&A v489, 1369 (2008).
contains the spline fits to the scaled proton collision strengths.
%filename: fe_19.psplups %rates: Ryans R.S.I., Keenan F.P., Reid R.H.G., unpublished. %energies: Observed values, from .elvlc file %comment: Fits valid for temperatures 2e6 to 4e7 K. %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % Peter Young 15-May-2001
%filename: fe_19.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 Wed Apr 16 17:42:56 2025