  In a recent paper (Moskalenko et al., 2002), it has been shown that the flux
of secondary cosmic ray (CR) antiprotons appears to be contradictory to
measurements of secondary to primary nuclei ratios in cosmic rays when
calculated in the same Galactic propagation model. The contradiction appears as
a value of the diffusion coefficient necessary to match the secondary ratios
antiproton/proton and B/C. In particlular, it was shown that the reacceleration
models designed to match secondary to primary nuclei ratios produce too few
antiprotons. It is, however, clear that some reacceleration is unavoidable in
the turbulent interstellar medium. Here we discuss an idea of how to improve
reacceleration model by allowing for the damping of interstellar turbulences on
the small scale by cosmic rays, mostly protons. This would lead to increase in
the mean free path lenghts at low energies, the well-known phenomena
empirically discovered in the Leaky Box models, thus producing less secondary
nuclei. Antiprotons will remain almost non-affected due to their high energy
threshold of production cross section.
