High-mass microquasars are binary systems composed by a massive star and a compact object from which relativistic jets are launched .
Regarding the companion star , observational evidence supports the idea that winds of hot stars are formed by clumps .
Then , these inhomogeneities may interact with the jets producing a flaring activity .
In the present contribution we study the interaction between a jet and a clump of the stellar wind in a high-mass microquasar .
This interaction produces a shock in the jet , where particles may be accelerated up to relativistic energies .
We calculate the spectral energy distributions of the dominant non-thermal processes : synchrotron radiation , inverse Compton scattering , and proton-proton collisions .
Significant levels of X- and \gamma -ray emission are predicted , with luminosities in the different domains up to \sim 10 ^ { 34 } -10 ^ { 35 } erg s ^ { -1 } on a timescale of about \sim 1 h. Finally , jet-clump interactions in high-mass microquasars could be detectable at high energies .
These phenomena may be behind the fast TeV variability found in some high-mass X-ray binary systems , such as Cygnus X-1 , LS 5039 and LS I+61 303 .
In addition , our model can help to derive information on the properties of jets and clumpy winds .