5 Conclusion

Total recombination coefficients for Ne⁺ ions and effective recombination coefficients for lines of Neii have been tabulated at temperatures and densities appropriate to nebular plasmas. The use of atomic data of high quality for bound-bound and bound-free radiative processes among all the terms with $n \leq 15$ means that the results given here should be more reliable than those of previous workers. It would be desirable to extend the calculations to higher electron densities to permit reliable interpretation of Neii emission from more dense objects such as young novae and stellar winds.

In Neii itself, further work is needed on the transition arrays where LS-coupling breaks down. Relatively strong recombination lines exist between 5g, 4f and 3d states which cannot be reliably used at present.