  For 30 years, cyclical wind variability in OB stars has puzzled the
astronomical community. Phenomenological models involving co-rotating bright
spots provide a potential explanation for the observed variations, but the
underlying physics remains unknown. We present recent results from
hydrodynamical simulations constraining bright spot properties and compare them
to what can be inferred from space-based photometry. We also explore the
possibility that these spots are caused by magnetic fields and discuss the
detectability of such fields.
