  High-mass microquasar jets propagate under the effect of the wind from the
companion star, and the orbital motion of the binary system. The stellar wind
and the orbit may be dominant factors determining the jet properties beyond the
binary scales.} An analytical study is performed to characterize the effects of
the stellar wind and the orbital motion on the jet properties. Accounting for
the wind thrust transferred to the jet, we derive analytical estimates to
characterize the jet evolution under the impact of the stellar wind. We include
the Coriolis force effect, induced by orbital motion and enhanced by the wind
presence. Large-scale evolution of the jet is sketched accounting for
wind-to-jet thrust transfer, total energy conservation, and wind-jet flow
mixing. If the angle of the wind-induced jet bending is larger than its
half-opening angle, the following is expected: (i) a strong recollimation
shock; (ii) bending against orbital motion, caused by Coriolis forces and
enhanced by the wind presence; and (iii) non-ballistic helical propagation
further away. Even if disrupted, the jet can reaccelerate due to ambient
pressure gradients, but wind entrainment can weaken this acceleration. On large
scales, the opening angle of the helical structure is determined by the
wind-jet thrust relation, and the wind-loaded jet flow can be rather slow. The
impact of stellar winds on high-mass microquasar jets can yield non-ballistic
helical jet trajectories, jet partial disruption and wind mixing, shocks, and
possibly non-thermal emission. Among several observational diagnostics at
different bands, the radio morphology on milliarcsecond scales can be
particularly insightful regarding the wind-jet interaction.
