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The common - arguably ubiquitous - large-scale variability of optical and UVlines profiles of hot, massive stars is widely interpreted as the directconsequence of structured, variable winds. Many of the variability phenomenaare observed to recur on timescales compatible with stellar rotation,suggesting a picture in which perturbations at the base of the wind - carriedinto view by stellar rotation - produce large-scale outward-propagating densitystructures. Magnetic fields have been repeatedly proposed to be at the root ofthese phenomena, although evidence supporting this view remains tenuous. Inthis review I discuss the evidence for large-scale structures in the winds ofO-type stars, the relationship between the observed recurrence timescales andthe expected stellar rotational periods, the magnetic and variabilityproperties of known magnetic O-type stars, and their implications forunderstanding wind variability of the broader population.

Magnetism, rotation and large-scale wind variability of O-type stars