CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.

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Naval Research Laboratory (USA) - Rutherford Appleton Laboratory (UK)
University of Cambridge (UK) - George Mason University (USA) - Universita' degli Studi di Firenze (Italy)

C IV - VERSION 4.2


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

  1. c_4.elvlc (energy levels)
  2. contains the energy levels in cm^(-1) It includes both experimental and theoretical values of the levels energies.

     
    %energy levels: Fuhr, J.R., Kelleher, D.E., Martin, W.C., Musgrove, A., Sugar, J., Wiese, W.L.,
            Dalton, G.R., Dragoset, R.A., Mohr, P.J., Olsen, K., Reader, J., Saloman, E.B., Sansonetti, C.J.,
            Wiersma, G., "NIST Atomic Spectra Database" Ver. 2.0, March 1999, NIST Physical Reference Data.
    % Theoretical energy levels: Badnell, N.R., Pindzola, M.S., 2000, J.Phys.B, 33, 1013
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % E. Landi Jun 2001
     
    

  3. c_4.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.

     
    %observed energy levels: Fuhr, J.R., et al., "NIST Atomic Spectra Database" Ver. 2.0, 
        March 1999, NIST Physical Reference Data.
    %oscillator strengths: Martin, I., Karwowski, J., Diercksen, G.H.F., Barrientos, C., 1993, A&AS, 100, 595.
    %oscillator strengths: W.L. Wiese, M.W. Smith, B.M. Glennon, Atomic Transition Probabilities, 
        Vol I, NSRDS-NBS 4, 1966.
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % E.Landi Jun 2001
    

  5. c_4.splups (electron collision data)
  6. 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: c_4.splups
    %oscillator strengths: Martin, I., Karwowski, J., Diercksen, G.H.F., Barrientos, C., 1993, A&AS, 100, 595
    %oscillator strengths: W.L. Wiese, M.W. Smith, B.M. Glennon, Atomic Transition Probabilities,
        Vol I, NSRDS-NBS 4, 1966
    %collision strengths: Badnell, N.R., Pindzola, M.S., 2000, J.Phys.B, 33, 1013
    %comment: the original effective collision strengths are provided in LS coupling. These 
        have been transformed into intermediate coupling effective collision strengths 
        according to the statistical weights
    %comment: the original data are given in the temperature range 4.2 < Log T < 6.5.
    %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
    %
    % Enrico Landi Jun 2001
    

  7. c_4.splups (proton collisional data) Not available in this VERSION.

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

    c_4_table.html (html table)


    Last revised by G. Del Zanna on 4-Sep-2009