Flash mixing on the white dwarf cooling curve: Understanding hot horizontal branch anomalies in NGC 2808

We present an ultraviolet color-magnitude diagram (CMD) spanning the hot ho rizontal branch (HB), blue straggler, and white dwarf populations of the gl obular cluster NGC 2808. These data were obtained with the far-UV and near- UV cameras on the Space Telescope Imaging Spectrograph (STIS). Although pre vious optical CMDs of NGC 2808 show a high-temperature gap within the hot H B population, no such gap is evident in our UV CMD. Instead, we find a popu lation of hot subluminous HB stars, an anomaly only previously reported for the globular cluster omega Cen. Our theoretical modeling indicates that th e location of these subluminous stars in the UV CMD, as well as the high-te mperature gap along the HB in optical CMDs, can be explained if these stars underwent a late helium-core flash while descending the white dwarf coolin g curve. We show that the convection zone produced by such a late helium fl ash will penetrate into the hydrogen envelope, thereby mixing hydrogen into the hot helium-burning interior, where it is rapidly consumed. This phenom enon is analogous to the "born again" scenario for producing hydrogen-defic ient stars following a late helium-shell flash. The flash mixing of the env elope greatly enhances the envelope helium and carbon abundances, and leads , in turn, to a discontinuous increase in the HB effective temperatures at the transition between canonical and flash-mixed stars. We argue that the h ot HB gap is associated with this theoretically predicted dichotomy in the HB properties. Moreover, the changes in the emergent spectral energy distri bution caused by these abundance changes are primarily responsible for expl aining the hot subluminous HB stars. Although further evidence is needed to confirm that a late helium-core flash can account for the subluminous HB s tars and the hot HB gap, we demonstrate that an understanding of these star s requires the use of appropriate theoretical models for their evolution, a tmospheres, and spectra.