  We examine the theoretical implications of a population of low-mass
helium-core white dwarfs in globular clusters. In particular, we focus on the
observed population in the core of NGC 6397, where several low-mass white dwarf
canditates have been identified as ``non-flickerers'' by Cool and
collaborators. Age and mass estimates from cooling models, combined with
dynamical and evolutionary considerations, lead us to infer that the dark
binary companions are C/O white dwarfs rather than neutron stars. Furthermore,
we find that the progenitor binaries very likely underwent an exchange
interaction within the last 1.e9 years. We examine the prospects for detecting
a similar population in other globular clusters, with particular attention to
the case of 47 Tuc.
