  Microquasars are binary systems that harbor a normal star and a compact
object (black-hole or neutron star), and show relativistic outflows (or jets).
The matter that forms these jets is of likely stellar origin, previously
expelled from the star and trapped in the potential well of the compact object.
This matter is accreted by the compact object, forming a disk due to its
angular momentum, and is eventually ejected in the form of a bipolar outflow
(the jets), which generates radio emission and could also be a very high-energy
emitter. To study and understand the radiation from microquasars, there is a
set of elements that can play a major role and are to be taken into account:
the photons and the expelled matter from the star in the case of high-mass
systems; the accreted matter radiation; the jet; the magnetic field carried by
the jet or filling the binary system; and the medium surrounding the
microquasar at large scales (~pc). In this lecture, we consider these elements
of the microquasar scenario and briefly describe the physical conditions and
processes involved in the production of non-thermal radiation from radio to
gamma-rays. The required energetics, particle acceleration and transport,
several radiative mechanisms, and the impact of different photon absorption
processes, are discussed.
