The spectrum of γ Velorum has been observed with a resolving power of 330 in the |12\,-\,13\,μ m| spectral region. The 12.8 μm forbidden line of [Ne II] has a rectangular profile, as expected for an optically thin line formed at large radii. The wind terminal velocity implied by this profile is |1520\,±\,200\,km\,s⁻¹|. This velocity, combined with the known radio flux, implies a mass loss rate of |8.8\,×\,10⁻⁵\,M_\,yr⁻¹| for γ Vel. An analysis of the He I and He II recombination lines observed in the spectrum implies that the |He⁺/He²⁺| ratio exceeds 6 in the 12 μm emitting region, confirming previous inferences that the degree of ionization decreases outwards in the wind. The flux measured in the [Ne II] line is used, along with the published [Ne III] 15.5 μm line flux, to rederive the abundance of neon in the wind of γ Vel, using improved analysis techniques. A Ne/He number ratio of |1.0\,±\,0.35\,×\,10⁻³| is found, a factor of 9 lower than previously estimated. This neon abundance is only slightly higher than would be expected for an initial cosmic abundance ratio. The large enhancement in the abundance of neon that is theoretically predicted for WC stars, due to the creation of 22Ne, is not present in the case of γ Vel.
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Barlow et al. (1988) studied this question.