2017MNRAS.471.2286S

ξ¹ CMa is a monoperiodically pulsating, magnetic β Cep star with magnetospheric X-ray emission that, uniquely amongst magnetic stars, is clearly modulated with the star's pulsation period. The rotational period P_rot has yet to be identified, with multiple competing claims in the literature. We present an analysis of a large ESPaDOnS data set with a 9 yr baseline. The longitudinal magnetic field <B_z> shows a significant annual variation, suggesting that P_rot is at least of the order of decades. The possibility that the star's H α emission originates around a classical Be companion star is explored and rejected based upon Very Large Telescope Interferometer AMBER and PIONIER interferometry, indicating that the emission must instead originate in the star's magnetosphere and should therefore also be modulated with P_rot. Period analysis of H α equivalent widths measured from ESPaDOnS and CORALIE spectra indicates P_rot > 30 yr. All evidence thus supports that ξ¹ CMa is a very slowly rotating magnetic star hosting a dynamical magnetosphere. H α also shows evidence for modulation with the pulsation period, a phenomenon that we show cannot be explained by variability of the underlying photospheric line profile, i.e. it may reflect changes in the quantity and distribution of magnetically confined plasma in the circumstellar environment. In comparison to other magnetic stars with similar stellar properties, ξ¹ CMa is by far the most slowly rotating magnetic B-type star, is the only slowly rotating B-type star with a magnetosphere detectable in H α (and thus, the coolest star with an optically detectable dynamical magnetosphere), and is the only known early-type magnetic star with H α emission modulated by both pulsation and rotation.