  High velocity clouds moving toward the disk will reach the Galactic plane and
will inevitably collide with the disk. In these collisions a system of two
shocks is produced, one propagating through the disk and the other develops
within the cloud. The shocks produced within the clouds in these interactions
have velocities of hundreds of kilometers per second. When these shocks are
radiative they may be inefficient in accelerating fresh particles, however they
can reaccelerate and compress Galactic cosmic rays from the background. In this
work we investigate the interactions of Galactic cosmic rays within a shocked
high velocity cloud, when the shock is induced by the collision with the disk.
This study is focused in the case of radiative shocks. We aim to establish
under which conditions these interactions lead to significant nonthermal
emission, especially gamma rays. We model the interaction of cosmic ray protons
and electrons reaccelerated and further energized by compression in shocks
within the clouds, under very general assumptions. We also consider secondary
electron-positron pairs produced by the cosmic ray protons when colliding with
the material of the cloud. We conclude that nearby clouds reaccelerating
Galactic cosmic rays in local shocks can produce high-energy radiation that
might be detectable with existing and future gamma-ray detectors. The emission
produced by electrons and secondary pairs is important at radio wavelengths,
and in some cases it may be relevant at hard X-rays. Concerning higher
energies, the leptonic contribution to the spectral energy distribution is
significant at soft gamma rays.
