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OB stars exhibit various types of spectral variability associated with windstructures, including the apparently ubiquitous discrete absorption components(DACs). These are proposed to be caused by either magnetic fields or non-radialpulsations (NRPs). In this paper, we evaluate the possible relation betweenlarge-scale, dipolar magnetic fields and the DAC phenomenon by investigatingthe magnetic properties of a sample of 13 OB stars exhibiting well-documentedDAC behaviour.  Using high-precision spectropolarimetric data acquired in part in the contextof the Magnetism in Massive Stars (MiMeS) project, we find no evidence forsurface dipolar magnetic fields in any of these stars. Using Bayesianinference, we compute upper limits on the strengths of the fields and use theselimits to assess two potential mechanisms by which the field may influence windoutflow: magnetic wind confinement and local photospheric brightnessenhancements. Within the limits we derive, both mechanisms fail to provide asystematic process capable of producing DACs in all of the stars of our sample.Therefore, this implies that dipolar fields are highly unlikely to beresponsible for these structures in all massive stars, meaning that some othermechanism must come into play.

Investigating the origin of cyclical wind variability in hot, massive stars - I. On the dipolar magnetic field hypothesis