Recent UV observations of the globular cluster NGC 2808 ( Brown et al . [ 2001 ] ) show a significant population of hot stars fainter than the zero-age horizontal branch ( “ blue hook ” stars ) , which can not be explained by canonical stellar evolution .
Their results suggest that stars which experience unusually large mass loss on the red giant branch and which subsequently undergo the helium core flash while descending the white dwarf cooling curve could populate this region .
Theory predicts that these “ late hot flashers ” should show higher temperatures than the hottest canonical horizontal branch stars and should have helium- and carbon-rich atmospheres .
As a test of this late hot flasher scenario , we have obtained and analysed medium resolution spectra of a sample of blue hook stars in NGC 2808 to derive their atmospheric parameters .
Using the same procedures , we have also re-analyzed our earlier spectra of the blue hook stars in \omega Cen ( Moehler et al . [ 2002 ] ) for comparison with the present results for NGC 2808 .
The blue hook stars in these two clusters are both hotter ( { T _ { eff } } \geq 35,000 K ) and more helium-rich than canonical extreme horizontal branch stars in agreement with the late hot flasher scenario .
Moreover , we find indications for carbon enhancement in the three most helium-enriched stars in NGC 2808 .
However , the blue hook stars still show some hydrogen in their atmospheres , perhaps indicating that some residual hydrogen survives a late hot flash and then later diffuses to the surface during the horizontal branch phase .
We note that the presence of blue hook stars apparently depends mostly on the total mass of the globular cluster and not so much on its horizontal branch morphology .