  We show that the large-scale cosmic ray anisotropy at ~10 TeV can be
explained by a modified Compton-Getting effect in the magnetized flow field of
old supernova remnants. This approach suggests an optimum energy scale for
detecting the anisotropy. Two key assumptions are that propagation is based on
turbulence following a Kolmogorov law and that cosmic ray interactions are
dominated by transport through stellar winds of the exploding stars. A
prediction is that the amplitude is smaller at lower energies due to incomplete
sampling of the velocity field and also smaller at larger energies due to
smearing.
