Fig. 7
Profiles for the Hγ, Hα, and He ii λ4541 lines of the CSPN NGC 6826 calculated with the model atmosphere code Fastwind (Puls, priv. comm.) using the stellar parameters derived by Kudritzki et al. (1997), compared to the observed profiles. Note in particular the sensitive dependence of the emission line Hα on the mass loss rate. The different predicted line profiles correspond to mass loss rates of Ṁ = 1.9 × 10-7 M⊙/yr (dotted), Ṁ = 2.5 × 10-7 M⊙/yr (dashed), and Ṁ = 3.6 × 10-7 M⊙/yr (dash-dotted).
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