Formation of the cosmic-ray halo: Galactic spectrum of primary cosmic
  rays
  A self-consistent model of a one-dimensional cosmic-ray (CR) halo around the
Galactic disk is formulated with the restriction to a minimum number of free
parameters. It is demonstrated that the turbulent cascade of MHD waves does not
necessarily play an essential role in the halo formation. Instead, an increase
of the Alfven velocity with distance to the disk leads to an efficient generic
mechanism of the turbulent redshift, enhancing CR scattering by the
self-generated MHD waves. As a result, the calculated size of the CR halo at
lower energies is determined by the halo sheath, an energy-dependent region
around the disk beyond which the CR escape becomes purely advective. At
sufficiently high energies, the halo size is set by the characteristic
thickness of the ionized gas distribution. The calculated Galactic spectrum of
protons shows a remarkable agreement with observations, reproducing the
position of spectral break at ~ 0.6 TeV and the spectral shape up to ~ 10 TeV.
