Resolved Specific Ion Data Collections

Temperature Range
0.078 eV → 23.27 eV


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  • Spontaneous Emission: O+3(i) → O+3(j) + hv
  • Electron Impact Excitation: O+3(i) + e → O+3(j) + e
2s2.2p 2P0.5 0.0 cm-1
2s2.2p 2P1.5 385.9 cm-1
2s.2p2 4P0.5 71439.8 cm-1
2s.2p2 4P1.5 71570.1 cm-1
2s.2p2 4P2.5 71755.5 cm-1
2s.2p2 2D1.5 126950.0 cm-1
2s.2p2 2D2.5 126936.0 cm-1
2s.2p2 2S0.5 164366.0 cm-1
2s.2p2 2P0.5 180481.0 cm-1
2s.2p2 2P1.5 180724.0 cm-1
2p3 4S1.5 231538.0 cm-1
2p3 2D1.5 255185.0 cm-1
2p3 2D2.5 255156.0 cm-1
2p3 2P0.5 289015.0 cm-1
2p3 2P1.5 289024.0 cm-1
 The ionisation potential and energy levels are from 'Tables of Spectra
 of Hydrogen, Carbon, Nitrogen and Oxygen Atoms and Ions' by C E Moore,
 edited by J W Gallacher (CRC Press). The ionisation potential adopted
 is 1.8 cm-1 less than that given by Kelly (J Chem Ref Data 1, 1987).
 The ordering of the levels is as given in the work used for the 
 effective collision strengths. The energies differ by at most 2.2 cm-1
 from those given by Edlen (Phys  Scripta 28, 483, 1983).

 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 (4.92-04 s-1). Other values
 include 1.39-3 s-1 from the multiconfiguration Dirac-Fock 
 calculations of Cheng, Kim and Desclaux (ADNDT 24, 111, 1979), and 
 5.17-4 s-1 from the Superstructure calculations done by Nussbaumer 
 and Storey (Astron Astrophys 115, 205, 1982) who used a 60 
 configuration basis.

 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 Blum and Pradhan (Ap J SS 80, 425, 
 1992) from a close-coupling R-matrix calculation involving all fine 
 structure calculations among and within the 2s2 2p, 2s 2p2 and 2p3 
 configurations were discussed. There was no consensus if these results 
 were more accurate than earlier close-coupling calculations. However, 
 there was no reason to think they were less accurate. It was suggested 
 that the Blum and Pradhan results be extended to higher temperatures. 
 This has been done and the results published by Zhang, Graziani and 
 Pradhan (Astron Astrophys 283, 319, 1994). The Zhang et al results were 
 obtained electronically and processed into ADF04 format.

 Sampson et al pointed out that effective collision strength for the 
 1-2 transition appears to rise spuriously with temperature. In the 
 newer results this does not occur. 

 J Lang
 A Lanzafame         May 1996


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