  It has been shown that supernova blast waves interacting with winds from
massive stars in compact star clusters may be capable of producing cosmic-ray
(CR) protons to above $10^{17}$ eV. We give a brief description of the
colliding-shock-flows mechanism and look at generalizations of the diffusion of
~ 100 PeV CRs in the turbulent galactic magnetic field present in the galactic
disk. We calculate the temporal evolution of the CR anisotropy from a possible
distribution of young compact massive star clusters assuming the sources are
intermittent on time scales of a few million years, i.e., comparable to their
residence time in the Milky Way. Within the confines of our model, we determine
the galactic/extra-galactic fraction of high-energy CRs resulting in
anisotropies consistent with observed values. We find that galactic star
clusters may contribute a substantial fraction of ~ 100 PeV CRs without
producing anisotropies above observed limits.
