  Cosmic rays in the energy range from about 10's GeV to several 100's TeV are
observed on Earth with an energy-dependent anisotropy of order 0.01-0.1%, and a
consistent topology that appears to significantly change at higher energy. The
nearest and most recent galactic cosmic ray sources might stochastically
dominate the observation and possibly explain a change in orientation of the
anisotropy as a function of energy. However, the diffusion approximation is not
able to explain its non-dipolar structure and, in particular, the significant
contribution of small angular scale features. Particle propagation within the
mean free path in the local interstellar medium might have a major role in
determining the properties of galactic cosmic rays, such as their arrival
distribution. In particular, scattering on perturbations induced in the local
interstellar magnetic field by the heliosphere wake, may cause a
re-distribution of anisotropic cosmic rays below about 100 TeV toward the
direction of the elongated heliotail and of the local interstellar magnetic
field in the outer heliosphere. Such scattering processes are considered
responsible of the observed TeV cosmic ray global anisotropy and its fine
angular structure.
