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INTEGRAL tripled the number of super-giant high-mass X-ray binaries (sgHMXB)known in the Galaxy by revealing absorbed and fast transient (SFXT) systems.Quantitative constraints on the wind clumping of massive stars can be obtainedfrom the study of the hard X-ray variability of SFXT. A large fraction of thehard X-ray emission is emitted in the form of flares with a typical duration of3 ksec, frequency of 7 days and luminosity of 1E36 ergs/s. Such flares are mostprobably emitted by the interaction of a compact object orbiting at ~ 10 R*with wind clumps (1E(22-23) g) representing a large fraction of the stellarmass-loss rate. The density ratio between the clumps and the inter-clump mediumis 1E(2-4) . The parameters of the clumps and of the inter-clump medium,derived from the SFXT flaring behavior, are in good agreement withmacro-clumping scenario and line-driven instability simulations. SFXT arelikely to have larger orbital radius than classical sgHMXB.

Probing clumpy stellar winds with a neutron-star