  The morphologies of detected jets in X-ray binaries are almost as diverse as
their number. This is due to different jet properties and ambient media that
these jets encounter. It is important to understand the physics of these
objects and to obtain information about possible sites suitable for particle
acceleration in order to explain the observations at very high energies. Here I
present the results obtained from the first relativistic hydrodynamical
simulations of jets in high-mass microquasars. Our results allow us to make
estimates for the emission originated in different sites of the whole structure
generated by the jets. These works represent a first step in trying to obtain a
deeper understanding of the physics and emission processes related with jets in
high-mass microquasars.
