other hand, show mostly super-solar abundances, with three exceptions: W8750, W9863, and W23198. Fig. \[ngc2808\_the\] shows that the helium-rich stars cluster between 35,000 K and 40,000 K, well beyond the hot end of the canonical EHB. We will now discuss the evolutionary status of the helium-poor and helium-rich stars in more detail.

[psfile=0505\_8.ps hscale=42 vscale=42 hoffset=-0 voffset=-70 angle=0]{}

Helium-Poor Stars
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As can be seen from Fig. \[ngc2808\_tg\], the six helium-poor stars cooler than 31,000 K occupy a range in effective temperature and surface gravity similar to the blue tail stars in NGC 6752. Their helium abundances are also similar to those observed in NGC 6752, indicating that the gravitational settling of helium has been equally efficient in both clusters. Thus, the helium-poor stars brighter than the gap at V$\approx$ agree with the predictions of canonical HB evolution.

The two helium-poor stars hotter than 40,000 K, W8750 and W9863, appear to be in a post-HB evolutionary state This can be seen in Fig. \[postHB\], where we compare the stellar parameters of these stars with HB and post-HB evolutionary tracks for canonical models, flash-mixed models with a thin hydrogen surface layer, and flash-mixed models with no envelope hydrogen. W9863 appears to 