recently, Brown et al. ([@brsw01]) have explored the evolution of both the early and late hot flashers through the helium core flash to the EHB in more detail. Their models show that a late hot helium flash on the white dwarf cooling curve will induce substantial mixing between the hydrogen envelope and helium core, leading to helium-rich EHB stars that are much hotter than canonical ones, as found previously by Sweigart ([@swei97]). This result has been confirmed by the calculations of Cassisi et al. ([@casc03]), who were able to follow the evolution of a late hot flasher completely through the helium core flash. Brown et al. ([@brsw01]) suggest that such flash mixing may be the key for understanding the evolutionary status of the blue hook stars. Such mixing may also be responsible for producing the helium-rich, high gravity field sdO stars (Lemke et al. [@lehe97]), whose origin is otherwise obscure. The flash mixing scenario predicts a gap of about 6000 K between the canonical EHB stars (i.e., stars without flash-mixing, including early hot flashers) and the late hot flashers as well as a helium dominated atmospheric composition for the late hot flashers. The hydrogen deficiency results in a flux redistribution 