  Strong interactions between jets and stellar winds at binary system spatial
scales could occur in high-mass microquasars. We study here, mainly from a
dynamical but also a radiative point of view, the collision between a dense
stellar wind and a mildly relativistic hydrodynamical jet of supersonic
nature.}{We have performed numerical 2-dimensional simulations of jets, with
cylindrical and planar (slab) symmetry, crossing the stellar wind material.
  From the results of the simulations, we derive estimates of the particle
acceleration efficiency, using first order Fermi acceleration theory, and give
some insight on the possible radiative outcomes. We find that, during jet
launching, the jet head generates a strong shock in the wind. During and after
this process, strong recollimation shocks can occur due to the initial
overpressure of the jet with its environment. The conditions in all these
shocks are convenient to accelerate particles up to $\sim$ TeV energies, which
can lead to leptonic (synchrotron and inverse Compton) and hadronic
(proton-proton) radiation. In principle, the cylindrical jet simulations show
that the jet is stable, and can escape from the system even for relatively low
power. However, when accounting for the wind ram pressure, the jet can be bent
and disrupted for power $\la 10^{36}$ erg s$^{-1}$.
