  Microquasars are X-ray binaries with relativistic jets. These jets are
powerful energy carriers, thought to be fed by accretion, which produce
non-thermal emission at different energy bands. To date, several Galactic
sources showing extended radio emission, among them at least one confirmed
microquasar, Cygnus X-1, have been detected in the TeV range. All of them show
complex patterns of spectral and temporal behavior. In this work, we discuss
the physics behind the very high-energy emission in microquasars. In concrete,
we focus on the microquasar Cygnus X-1, and also in the other two TeV binaries
with detected extended outflows, LS 5039 and LS I +61 303, pointing out
relevant aspects of the complex phenomena occurring in them. We conclude that
the TeV emission is likely of leptonic origin, although hadrons cannot be
discarded. In addition, efficient electromagnetic cascades can hardly develop
since even relatively low magnetic fields suppress them. Also, the modeling of
the radiation from some of the detected sources points to them as either
extremely efficient accelerators, and/or having the TeV emitter at a distance
from the compact object of about 10e12 cm. Finally, we point out that the role
of a massive and hot stellar companion, due to its strong photon field and
wind, cannot be neglected when trying to understand the behavior of
microquasars at high and very high energies. The complexity of microquasars
precludes straightforward generalizations to a whole population, and are better
studied presently in a source by source base.
