Characterizing the dynamical magnetosphere of the extremely slowly rotating magnetic O9.7 V star HD 54879 using rotational modulation of the Hα profile.

The magnetic field in the O9.7 V star HD 54879 has been monitored for almost a decade. Spectropolarimetric observations reveal a rather strong mean longitudinal magnetic field that varies with a period of about 7.41 years. Observations in the Hα$$ \alpha $$ line show a variation with the same period, while the Hβ$$ \beta $$ line shows only little variation. Assuming the periodic variation to be caused by a slow rotation and a dipolar magnetic field, we find a magnetic field strength of ≥$$ \ge $$2 kG at the magnetic poles. With the relatively low mass loss rate of 10−9M⊙$$ {10}^{-9}{M}_{\odot } $$ year−1, this star is a case of extremely strong magnetic confinement. Both theoretical arguments and numerical simulations indicate the presence of an extended disk of increased gas density in the equatorial plane of the magnetic field, where gas from the line‐driven stellar wind is trapped. This disk is likely to be the origin of the observed Hα$$ \alpha $$ emission, which peaks together with the strongest line‐of‐sight magnetic field. The profile of the Hα$$ \alpha $$ line is resolved in several components and shows a remarkable variability with the rotation period. [ABSTRACT FROM AUTHOR]

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