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Gamma-rays can be produced by the interaction of a relativistic jet and thematter of the stellar wind in the subclass of massive X-ray binaries known as"microquasars". The relativistic jet is ejected from the surroundings of thecompact object and interacts with cold protons from the stellar wind, producingpions that then quickly decay into gamma-rays. Since the resulting gamma-rayemissivity depends on the target density, the detection of rapid variability inmicroquasars with GLAST and the new generation of Cherenkov imaging arrayscould be used to probe the clumped structure of the stellar wind. Inparticular, we show here that the relative fluctuation in gamma rays may scalewith the square root of the ratio of porosity length to binary separation,\sqrt{h/a}, implying for example a ca. 10 % variation in gamma ray emission fora quite moderate porosity, h/a ~ 0.01.

Using gamma-rays to probe the clumped structure of stellar winds