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It is observationally as well as theoretically well established that thewinds of hot, massive OB-stars are highly structured on a broad range ofspatial scales. This paper first discusses consequences of the small-scalestructures associated with the strong instability inherent to the line-drivingof these winds. We demonstrate the importance of a proper treatment of suchwind clumping to obtain reliable estimates of mass-loss rates, and also showthat instability simulations that are perturbed at the lower boundary indeeddisplay significant clumping quite close to the wind base, in general agreementwith observations. But a growing subset of massive stars has also been found topossess strong surface magnetic fields, which may channel the star's outflowand induce also large-scale wind structures and cyclic behavior of spectraldiagnostics. The paper concludes by showing that multi-dimensional,magneto-hydrodynamical wind simulations, together with detailedradiative-transfer modeling, can reproduce remarkably well the periodic Balmerline emission observed in slowly rotating magnetic O stars like HD191612.

Diagnosing small- and large-scale structure in the winds of hot, massive OB-star