  Using N-body simulations we study the evolution of separate stellar
populations in dwarf galaxies in the context of the tidal stirring scenario for
the formation of dwarf spheroidal (dSph) galaxies in the Local Group. The dwarf
galaxies, initially composed of a stellar disk and a dark matter halo, are
placed on seven different orbits around the Milky Way. The stars are divided
into two populations, within and outside the half-light radius, and their
positions are followed for 10 Gyr. We find that the populations retain
different density distributions even over such long timescales. Some of the
stars of the outer population migrate to the central part of the dwarf forming
an extended core while the stars of the inner population develop a tail in the
outer parts. In addition, the outer population is more heavily stripped by
tidal forces from the Milky Way and may become subdominant at all radii on
tight enough orbits. We conclude that the tidal stirring model is fully
compatible with the presence of multiple stellar populations in dSph galaxies.
