Ca XVIII - VERSION 5.1

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

• ca_18.elvlc (energy levels)

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

  References:

  %energy levels (1-24): Martin, W.C., Zalubas, R., 1983, J. Phys. Chem. Ref. Data, 12, 323.
  %Theoretical energy levels (1-24): Zhang,H.L., Sampson,D.H., Fontes,C.J., ADNDT, 44, 31.
  %Innershell 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
  %Innershell theoretical energy levels: Goett, S.J., Sampson, D.H., 1983, ADNDT, 29, 535
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % E. Landi - July 1999
  

  
  

• ca_18.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: Sugar, J., Corliss, C., 1979, J.Phys.Chem.Ref.Data, 8, 865
  %observed energy levels: Kelly, R.L., 1987, J.Phys.Chem.Ref.Data, 16, Suppl. 1
  %comments:  4s, 4p and 4p levels from Kelly
  %oscillator strengths: H.L. Zhang, D.H. Sampson, C.J. Fontes, 1990, ADNDT, 44, 31
  %oscillator strengths: Martin, I., Karwowski, J., Diercksen, G.H.F., Barrientos, C., 1993, A&AS, 100, 595
  % Innershell radiative data: Goett, S.J., Sampson, D.H., 1983, ADNDT, 29, 535
  %A values (autoionizing): Vainshtein, L.A., Safronova, U.I., 1978, ADNDT, 21, 49
     and 1980, ADNDT, 25, 311 - updated by U.I. Safronova, 1999
  %Comment: Other radiative data were calculated using SUPERSTRUCTURE with a 23 configuration model
  %comment:  the following lines identified by Feldman, U., Doschek, G., Kreplin, R.W., 1980, ApJ, 238, 365
      2   36         3.2066      5.910e-01      9.615e+13        1s2.2p 2P0.5 -         1s.2p2 2D1.5   (k)              
      3   39         3.2033      1.344e+00      2.192e+14        1s2.2p 2P1.5 -         1s.2p2 2P1.5   (a)              
  %comment:  unobserved lines
      1   26        -3.2260      1.103e-03      3.532e+11        1s2.2s 2S0.5 -  1s.(2S).2s.2p 4P0.5                 
      1   27        -3.2241      6.620e-03      1.061e+12        1s2.2s 2S0.5 -  1s.(2S).2s.2p 4P1.5                 
      1   28        -3.2209      6.669e-06      7.142e+08        1s2.2s 2S0.5 --  1s.(2S).2s.2p 4P2.5                
      1   29        -3.1988      3.691e-01      1.202e+14        1s2.2s 2S0.5 -  1s.(2S).2s.2p 2P0.5                 
      1   30        -3.1961      9.666e-01      1.577e+14        1s2.2s 2S0.5 -  1s.(2S).2s.2p 2P1.5                 
      2   25        -3.2634      8.502e-03      2.661e+12        1s2.2p 2P0.5 -         1s.2s2 2S0.5                 
      2   31        -3.2210      3.368e-03      1.082e+12        1s2.2p 2P0.5 -         1s.2p2 4P0.5                 
      2   32        -3.2182      7.303e-05      1.175e+10        1s2.2p 2P0.5 -         1s.2p2 4P1.5                 
      2   38        -3.1970      5.507e-01      1.796e+14        1s2.2p 2P0.5 -         1s.2p2 2P0.5                 
      2   40        -3.1783      2.860e-02      9.439e+12        1s2.2p 2P0.5 -         1s.2p2 2S0.5                 
      3   25        -3.2678      1.215e-02      3.792e+12        1s2.2p 2P1.5 -         1s.2s2 2S0.5                 
      3   31        -3.2252      1.522e-04      4.877e+10        1s2.2p 2P1.5 -         1s.2p2 4P0.5                 
      3   32        -3.2225      4.753e-03      7.628e+11        1s2.2p 2P1.5 -         1s.2p2 4P1.5                 
      3   33        -3.2197      1.974e-02      2.115e+12        1s2.2p 2P1.5 -         1s.2p2 4P2.5                 
      3   38        -3.2012      1.952e-01      6.349e+13        1s2.2p 2P1.5 -         1s.2p2 2P0.5                 
      3   40        -3.1824      2.153e-01      7.087e+13        1s2.2p 2P1.5 -         1s.2p2 2S0.5                 
  
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % E. Landi - July 1999
  

  
  

• ca_18.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: ca_18.splups
  %oscillator strengths: H.L. Zhang, D.H. Sampson, C.J. Fontes, 1990, ADNDT, 44, 31
  %oscillator strengths: Martin, I., Karwowski, J., Diercksen, G.H.F., Barrientos, C., 1993, A&AS, 100, 595
  %collision strengths: Zhang, Sampson, Fontes, 1990, ADNDT, 44, 31
  %Collision strengths innershell transitions: Goett, S.J., Sampson, D.H., 1983, ADNDT, 29, 535
  % produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % E.Landi and K.P.Dere - July 1999
  

  
  

• ca_18.psplups (electron collision data) - Not Present in CHIANTI 5.1

  contains the spline fits to the scaled proton collision strengths.
  

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

  
  

• ca_18_table.html (html table)