  Previous spectroscopic analyses of Blue Horizontal Branch (BHB) stars in six
globular clusters revealed too low masses in four clusters when compared to
canonical evolutionary theory, while the masses of the BHB stars in NGC 6752
and M 5 are found to be consistent with theory. We recalculated BHB star masses
using new cluster distances derived by Reid (1997a,b) from HIPPARCOS parallaxes
of local subdwarfs by main sequence fitting. The new distances are larger than
previous estimates resulting in larger masses for the BHB stars. Since the
increase in distance is small for NGC 6752 and M 5, the agreement with
predicted masses persists. For M 15 and M 92 the masses now come into good
agreement with theoretical predictions, while for NGC 288 and NGC 6397 the mass
deficit is reduced but the BHB star masses remain slightly too low. Previous
spectroscopic analyses also highlighted the problem of too low gravities for
some BHB stars. The gravities and absolute magnitudes of BHB stars are
revisited in the light of new evolutionary Horizontal Branch models.
