  We study the effect of dynamical friction on globular clusters and on the
stars evaporated from the globular clusters (stellar streams) moving in a
galactic halo. Due to dynamical friction, the position of a globular cluster
(GC) as a stream progenitor starts to shift with respect to its original
position in the reference frame of initial GC orbit. Therefore the stars that
have evaporated at different times have different mean position with respect to
the GC position. This shifting results in a certain asymmetry in stellar
density distribution between the leading and trailing arms of the stream. The
degree of the asymmetry depends on the characteristics of the environment in
which the GC and the stream stars move. As GCs are located mainly in outer
parts of a galaxy, this makes dynamical friction a unique probe to constrain
the underlying dark matter spatial density and velocity distributions. For a GC
NGC 3201 we compared our theoretical shift estimates with available
observations. Due to large uncertainties in current observation data, we can
only conclude that the derived estimates have the same order of magnitude.
