  There could be a significant population of double white dwarf binaries (DWDs)
inside globular clusters (GCs), however, these are often too faint to be
individually observed. We have utilized a large number GC models evolved with
the Monte Carlo Cluster Simulator (MOCCA) code, to create a large statistical
dataset of DWDs. These models include multiple-stellar populations, resulting
in two distinct initial populations: one dense and another less dense. Due to
the lower density of one population, a large number of objects escape during
the early GC evolution, leading to a high mass-loss rate. In this dataset we
have analysed three main groups of DWDs, namely in-cluster binaries, escaped
binaries, and isolated evolution of primordial binaries. We compared the
properties of these groups to observations of close and wide binaries. We find
that the number of escaping DWDs is significantly larger than the number of
in-cluster binaries and those that form via the isolated evolution of all
promiridial binaries in our GC models. This suggests that dynamics play an
important role in the formation of DWDs. For close binaries, we found a good
agreement in the separations of escaped binaries and isolated binaries, but
in-cluster binaries showed slight differences. We could not reproduce the
observed extremely low mass WDs due to the limitations of our stellar and
binary evolution prescriptions. For wide binaries, we also found a good
agreement in the separations and masses, after accounting for observational
selection effects. We conclude that, even though the current observational
samples of DWDs are extremely biased and incomplete, our results compare
reasonably well with observations.
