  The population of compact binaries in dense stellar systems is affected
strongly by frequent dynamical interactions between stars and their interplay
with the stellar evolution. In this contribution, we consider these effects on
binaries with a white dwarf accretor, in particular cataclysmic variables and
AM CVns. We examine which processes can successfully lead to the creation of
such X-ray binaries. Using numerical simulations, we identify predominant
formation channels and predict the expected numbers of detectable systems. We
discuss also why the distribution of cataclysmic variables has a weaker
dependence upon the cluster density than the distribution of quiescent low-mass
X-ray binaries and why dwarf nova outbursts may not occur among globular
cluster cataclysmic variables.
