Fe XXV - VERSION 8.0


The CHIANTI database has the following primary ASCII files for this ion:

  1. fe_25.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    %filename:  fe_25.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
    
    %observed energy levels: Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8
    
    %observed energy (level 34):  Martin,W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995,
    NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    % K.P.Dere and E.Landi 2000
    %
    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.
    
    Observed energy levels (1s2s, 1s2p):  Artemyev, A. N.; Shabaev, V. M.; Yerokhin, V. A.; Plunien, G.; Soff, G., 2005, Phys. Rev. A, 72, 2104
    ADSref:  http://adsabs.harvard.edu/abs/2005PhRvA..71f2104A
    
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2014 July 26
     -1
     
    

  3. fe_25.wgfa (radiative data)
  4. 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_25.wgfa
    
    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
    
    %A values(1-4, two-photon):  Drake, G. W. F., Phys Rev A, 1986, 34, 2871
    %A values (1-2,2-5,1-6):  Lin, C. D., Johnson, W.R., Dalgarno, A., Phys Rev A, 1977, 15, 154
    %A values (1-2,5,6,7; 2-3,6): Palmeri, P., Mendoza, C., Kallman, T.R., Bautista, M.A. 2003, A&A, 403, 1175
    
    Observed wavelengths:  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.
    
    Observed wavelength (1-7):  Beiersdorfer, P., Bitter, M., von Goler, S., Hill, K. W., 1986, Phys. Rev. A, 40, 150
    
    minimum branching ratio =   1.00e-04
    
    produced as a part of the  'CHIANTI' atomic database for astrophysical spectroscopy
    K. Dere (GMU) - 2014 July 26
    

  5. fe_25.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    %filename:  fe_25.upsdat
    Theoretical gf A values:  Whiteford, A. D., Badnell, N. R., Ballance, C. P., O'Mullane, M. G., Summers, H. P., Thomas, A. L., 2001, J. Phys. B, 34, 3179
    minimum branching ratio =   1.00e-04
    collision strengths provided in the range   1.25e+05 to   1.25e+09 K
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
    K. Dere (GMU) - 2012 September 16
    
    

  7. (proton collisional data) Not available in this VERSION.
  8. fe_25.reclvl (total recombination population rates)
  9.  
    filename:  fe_25.reclvl
    %Radiative recombination rates for recombination onto Fe XXVI to form Fe XXV
    Badnell, N. R., 2006, ApJS, 167, 334
    Radiative Recombination Data for Modeling Dynamic Finite-Density Plasmas
    adsLink:  http://adsabs.harvard.edu/abs/2006ApJS..167..334B
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2014 April 24
    


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

    fe_25_table.html (html table)

    Page created by Giulio Del Zanna on Fri Sep 18 13:27:18 2015