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)

S XV - VERSION 4.2

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

  1. s_15.elvlc (energy levels)

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

     
%observed energy levels: Martin,W.C., Sugar,J., Musgrove,A., Dalton,G.R., 1995,
     NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61.
%observed energy levels (1s2p 3P): Chen, M.H., Cheng, K.T., Johnson, W.R., 1993, Ph.Rev.A, 47, 3692
%theoretical energy levels: Sampson, D.H., Goett, S.J., Clark, R.E.H., 1983, ADNDT, 29, 467
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% K.P.Dere and E.Landi 2000

  2. s_15.wgfa (radiative data)

    3. 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: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995,
   NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61.
%observed energy levels (2s2p 3P): Chen, M.H., Cheng, K.T., Johnson, W.R., 1993, Ph.Rev.A, 47, 3692
%theoretical energy levels: Sampson, D.H., Goett, S.J., Clark, R.E.H., 1983, ADNDT, 29, 467
%A values (1-3, 2-phot): Drake, G.W.F., Phys Rev A, 1986, 34, 2871
%A values (1-2,5,6; 2-4,5,6): Lin, C.D., Johnson, W.R., Dalgarno, A., Phys Rev A, 1977, 15, 154
%oscillator strengths (transitions involving lower levels 1,2,3): Sampson, D.H., Goett, S.J., 
   Clark, R.E.H., 1983, ADNDT, 29, 467, Hydrogenic values
%oscillator strengths: Wiese, W.L., Smith, M.W., Glennon, B.M., 1966, Atomic Transition Probabilities, NSRDS-NBS-4. 
%comment: Wiese's oscillator strengths are hydrogenic
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% K.P.Dere and E.Landi 2000

  3. s_15.splups (electron collision data)

    4. 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: s_15.splups
%oscillator strengths (transitions involving lower levels 1,2,3): Sampson, D.H., Goett, S.J.,
   Clark, R.E.H., 1983, ADNDT, 29, 467, Hydrogenic values
%oscillator strengths: Wiese, W.L., Smith, M.W., Glennon, B.M., 1966, Atomic Transition 
   Probabilities, NSRDS-NBS-4, Hydrogenic values
%effective collision strengths: Zhang, H., Sampson, D.H., 1987, ApJSS, 63, 487
%collison strengths: Sampson, D.H., Goett, S.J., Clark, R.E.H., 1983, ADNDT, 29, 467,  Hydrogenic values
%comment: effective collision strengths were provided in the temperature range 6.2 < Log T < 7.6
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% K.P.Dere and E. Landi 1998

  4. s_15.splups (proton collisional data) Not available in this VERSION.

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

    s_15_table.html (html table)


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