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It has been widely thought that measuring the misalignment angle between the orbital plane of a transiting exoplanet and the spin of its host star was a good discriminator between different migration processes for hot‐Jupiters. Specifically, well‐aligned hot‐Jupiter systems (as measured by the Rossiter–McLaughlin effect) were thought to have formed via migration through interaction with a viscous disc, while misaligned systems were thought to have undergone a more violent dynamical history. These conclusions were based on the assumption that the planet‐forming disc was well‐aligned with the host star. Recent work by a number of authors has challenged this assumption by proposing mechanisms that act to drive the star–disc interaction out of alignment during the pre‐main‐sequence phase. We have estimated the stellar rotation axis of a sample of stars which host spatially resolved debris discs. Comparison of our derived stellar rotation axis inclination angles with the geometrically measured debris–disc inclinations shows no evidence for a misalignment between the two.

On the alignment of debris discs and their host stars’ rotation axis – implications for spin‐orbit misalignment in exoplanetary systems