S X - VERSION 4.0

The CHIANTI database consists of 4 primary ASCII files for each ion in the database.

• s_10.elvlc (energy levels)

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

  References:

  %Observed energy levels (1-15): Edlen, 1984, Phys.Scripta, 30, 135  
  %Observed energy levels (16-22): 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: Bell and Ramsbottom, 2000, ADNDT 76, 176
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % G. Del Zanna, Dec 2001.
  

  
  

• s_10.wgfa (radiative data)

  contains wavelengths, gf and A values for each transition. Wavelengths are based on experimental level energies where available; wavelengths calculated from theoretical energies are less accurate and are given as negative values.

  References:

  %Observed energy levels (1 - 15): Edlen, 1984, Phys.Scripta, 30, 135
  %Observed energy levels (16 - 22): 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
  % A values for transitions within the ground configuration: Merkelis et al., 1999, Physica Scripta 59,122
  % gf values for transitions between the (1 - 15) levels: Zhang, Sampson, ADNDT, 1999, 72, 153
  % A values for transitions with 2s.2p4 and 2p5: Zhang, Sampson, ADNDT, 1999, 72, 153
  % A values for forbidden transitions with 2s.2p4 and 2p5: Merkelis et al., 1999, Physica Scripta 59,122
  % A and gf values for transitions from levels 16-22: SUPERSTRUCTURE calculation by E.Landi Jan 2002
  % Comment: 24 configurations used for the SUPERSTRUCTURE calculation:
  %
  %                     2s2.2p3, 2s.2p4, 2p5, 2s.2p3.3l (l=s,p,d)
  %                     2s.2p3.4l (l=s,p,d,f), 2p4.3l (l=s,p,d)
  %                     2p4.4l (l=s,p,d,f), 2s2.2p2.3l (l=s,p,d)
  %                     2s2.2p2.4l (l=s,p,d,f)
  %
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % G. Del Zanna and E.Landi, May 2001
  

  
  

• s_10.splups (electron collision data)

  contains the spline fits to the electron collision strengths scaled according to 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.

  References:

  
  %filename: s_10.splups 
  %oscillator strengths (1 - 15):  Zhang, Sampson, 1999, ADNDT, 72, 153
  %oscillator strengths (16 - 22): SUPERSTRUCTURE calculation (see s_10.wgfa)
  %effective collision strengths: Bell and Ramsbottom, 2000, ADNDT, 76, 176 
  % Comment: Corrected errors in the transitions: 1-12, 2-22, 8-22, 12-19
  % Comment: effective collision strengths are provided in the temperature range 4.6 < Log T < 6.7
  % Comment: the effective collision strength at Log T=4.6 of transition 12-18 has been omitted from the fit
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % G. Del Zanna, Dec 2001.
  

  
  

• s_10.psplups (electron collision data) - Not Present in CHIANTI 4

  contains the spline fits to the scaled proton collision strengths.

The html tables below contain the radiative data of all the lines sorted in wavelength