Polarimetric detection of non-radial oscillation modes in the β Cephei star β Crucis

Here we report the detection of polarization variations due to non-radial modes in the β Cephei star β Crucis. In so doing we confirm 40-year-old predictions of pulsation-induced polarization variability and its utility in asteroseismology for mode identification. In an approach suited to other β Cephei stars, we combine polarimetry with space-based photometry and archival spectroscopy to identify the dominant non-radial mode in polarimetry, f 2 , as mode degree ℓ = 3, azimuthal order m = −3 (in the m -convention of Dziembowski) and determine the stellar axis position angle as 25 (or 205) ± 8°. The rotation axis inclination to the line of sight was derived as ~46° from combined polarimetry and spectroscopy, facilitating identification of additional modes and allowing for asteroseismic modelling. This reveals a star of 14.5 ± 0.5 M ⊙ and a convective core containing ~28% of its mass—making β Crucis the most massive star with an asteroseismic age. This Article reports the detection of oscillations in the massive star β Crucis using polarized light. Such oscillatory modes provide information about stellar structure; in this case the stellar mass, inclination of the rotation axis and size of the convective core.