Resolved Specific Ion Data Collections

Temperature Range
1.043 eV → 313 eV


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  • Spontaneous Emission: S+11(i) → S+11(j) + hv
  • Electron Impact Excitation: S+11(i) + e → S+11(j) + e
2s2.2p 2P0.5 0.0 cm-1
2s2.2p 2P1.5 13136.0 cm-1
2s.2p2 4P0.5 193920.0 cm-1
2s.2p2 4P1.5 198713.0 cm-1
2s.2p2 4P2.5 205426.0 cm-1
2s.2p2 2D1.5 346716.0 cm-1
2s.2p2 2D2.5 346981.0 cm-1
2s.2p2 2S0.5 439562.0 cm-1
2s.2p2 2P0.5 464807.0 cm-1
2s.2p2 2P1.5 471431.0 cm-1
2p3 4S1.5 610113.0 cm-1
2p3 2D1.5 689936.0 cm-1
2p3 2D2.5 690465.0 cm-1
2p3 2P0.5 774040.0 cm-1
2p3 2P1.5 775815.0 cm-1
 The ionisation potential is from Kelly (J Phys Chem Ref Data 16, 
 Suppl 1, 1987). The energies are from Edlen (Phys Scripta 28, 483, 
 1983). The ordering of the levels is as given in the work used for 
 the effective collision strengths. There are differences in energy
 of up to 58 cm-1 with the data from the NIST discs.

 For the transition between the 1/2 and 3/2 levels of the ground term 
 the multiconfiguration Hartree-Fock Breit-Pauli result of C Froese 
 Fischer (J Phys B 16, 157 1983) is used (20.4 s-1). The
 multiconfiguration Dirac-Fock calculations of Cheng, Kim and 
 Desclaux (ADNDT 24, 111, 1979) yielded 21.1 s-1 and the calcuations 
 of Flower and Nussbaumer (Astron Astrophys 45, 349, 1975) gave
 19.6 s-1.

 The results of of Merkelis, Vilkas, Gaigalas and Kisielius were 
 adopted (Phys Scripta 51, 233, 1995). Their calculation employed 
 the stationary second order many-body perturbation theory, the 
 relativistic corrections being included using the Breit-Pauli 
 approximation. They say that for 12<=Z<=20 their results are 
 more accurate than the multiconfiguration Hartree-Fock with 
 Breit-Pauli correction results of Dankwort and Trefftz (Astron 
 Astrophys 65, 93, 1978) adopted for O IV and Ne VI. For allowed 
 E1 transitions their results obtained in intermediate LSJ-coupling
 are close to those determined by Dankwort and Trefftz and Cheng
 et al.

 In their assessment of effective collision strengths for the B-like 
 sequence Sampson, Zhang and Fontes (ADNDT 57, 98, 1994) review the 
 available results. Close coupling results were then available
 for transitions between the lowest two levels and from them to the
 next higher 13 levels. These calculations by Saha and Trefftz (Z.
 Naturforschung A 37, 744 1982) included intermediate coupling 
 effects and used UCL codes. However, Sampson et al anticipated 
 the R-matrix close coupling calculations of Zhang, Graziana and 
 Pradhan (Astron Astrophys 283, 319,1994) for the 105 fine structure
 transitions among the 15 levels of the 2s2 2p, 2s 2p2 and 2p3 
 configurations. These results are adopted here. The data were 
 obtained electronically and processed into ADF04 format.

 J Lang
 A Lanzafame         May 1996


  • Jim Lang
  • Hong Zhang
  • Douglas Sampson
  • Alessandro Lanzafame
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