  We report on the search for overall kinematical or structural conditions that
have allowed some Milky Way globular clusters to presently develop tidal tails.
For this purpose, we build a comprehensive catalogue of globular clusters with
studies focused on their outermost regions and classified them in three
categories: those with observed tidal tails, those with extra-tidal features
different from tidal tails and those without any signature of extended stellar
density profiles. When exploring different kinematical and structural parameter
spaces, we found that globular clusters - irrespective from the presence of
tidal tails, or any other kind of extra-tidal features or the absence of them -
behave similarly. In general, globular clusters whose orbits are relatively
more eccentric and very inclined respect to the Milky Way plane have undergone
a larger amount of mass-loss by tidal disruption. The latter has also
accelerated the internal dynamics toward a comparatively more advanced stage of
evolution. These outcomes show that it is not straightforward to find any
particular set of parameter space and dynamical conditions that can definitely
predict tidal tails along globular clusters in the Milky Way.
