Resolved Specific Ion Data Collections

Temperature Range
0.215 eV → 64.63 eV


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  • Spontaneous Emission: Ne+5(i) → Ne+5(j) + hv
  • Electron Impact Excitation: Ne+5(i) + e → Ne+5(j) + e
2s2.2p 2P0.5 0.0 cm-1
2s2.2p 2P1.5 1308.0 cm-1
2s.2p2 4P0.5 100298.0 cm-1
2s.2p2 4P1.5 100742.0 cm-1
2s.2p2 4P2.5 101390.0 cm-1
2s.2p2 2D1.5 179022.0 cm-1
2s.2p2 2D2.5 178992.0 cm-1
2s.2p2 2S0.5 230855.0 cm-1
2s.2p2 2P0.5 249281.0 cm-1
2s.2p2 2P1.5 250109.0 cm-1
2p3 4S1.5 321617.0 cm-1
2p3 2D1.5 359612.0 cm-1
2p3 2D2.5 359543.0 cm-1
2p3 2P0.5 406008.0 cm-1
2p3 2P1.5 406053.0 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 152 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 (1.95-02 s-1). The
 multiconfiguration Dirac-Fock calculations of Cheng, Kim and 
 Desclaux (ADNDT 24, 111, 1979) yielded 2.83-02 s-1.

 The results of Dankwort and Trefftz (Astron Astrophys 65, 93, 1978) 
 have been adopted for the majority of transitions. Their calculation 
 used the multiconfiguration Hartree-Fock ansatz with Breit-Pauli 
 corrections. For transitions 3-12, 3-14, 3-15, 4-12, 4-13, 4-14, 
 4-15, 5-12, 5-13, 5-15, 6-11, 7-11, 8-11, 8-12, 9-11 and 10-11 
 Dankwort and Trefftz did not give results. Accordingly the results 
 of Merkelis, Vilkas, Gaigalas and Kisielius were used (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.

 In their assessment of effective collision strengths for the B-like 
 sequence Sampson, Zhang and Fontes (ADNDT 57, 98, 1994) review the 
 available results. The results of Hayes (J Phys b25, 2649, 1992 were
 recommended. These were close coupling calculations by the R-matrix 
 method for transitions between the 2s2 2p 2P and 2s 2p2 4P energy 
 terms and from them to the energy terms of the 2s 2p2, 2p3, 2s2 3s, 
 2s2 3p and 2s2p3s configurations. 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

 Update:  03/08/97 Ralph Dux - Corrected error in indexing in Upsilon rows.
                               Swapped indices 6 and 7




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