  Several cosmic-ray observatories have provided a high accuracy map of the sky
at TeV--PeV energies. The data reveals an O(0.1%) deficit from north galactic
directions that peaks at 10 TeV and then evolves with the energy, together with
other anisotropies at smaller angular scales. Using Boltzmann's equation we
derive expressions for the cosmic-ray flux that fit most of these features. The
anisotropies depend on the local interstellar magnetic field B_{IS}, on the
average galactic field B_{R} in our vicinity, and on the distribution of
dominant cosmic-ray sources. We show that the initial dipole anisotropy along
B_{IS} can be modulated by changes in the global cosmic ray wind, and that a
variation in the dipole direction would imply a given radius of coherence for
B_{IS}. We also show that small and medium-scale anisotropies may appear when
the full-sky anisotropy finds a turbulence acting as a magnetic lens.
