  We present the results of detailed N-body simulations of clusters moving in a
realistic Milky Way (MW) potential. The strong interaction with the bulge and
the disk of the Galaxy leads to the formation of tidal tails, emanating from
opposite sides of the cluster. Some characteristic features in the morphology
and orientation of these streams are recognized and intepreted. The tails have
a complex morphology, in particular when the cluster approaches its
apogalacticon, showing multiple ``arms'' in remarkable similarity to the
structures observed around NGC 288 and Willman 1. Actually, the tails are
generally good tracers of the cluster path quite far from the cluster center
(>7--8 tidal radii), while on the smaller scale they are mainly pointing in the
direction of the Galaxy center. In particular, the orientation of the inner
part of the tails is highly correlated to the cluster orbital phase and to the
local orbital angular acceleration. This implies that, in general, the orbital
path cannot be estimated directly from the orientation of the tails, unless a
sufficient large field around the cluster is available.
