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, f₂, 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.

在这里，我们报告了对仙王座 β 十字星中非径向模式引起的偏振变化的检测。通过这样做，我们证实了 40 年前关于脉动引起的极化变异性的预测及其在星震学中用于模式识别的实用性。在一种适用于其他 β Cephei 恒星的方法中，我们将旋光法与基于空间的光度法和档案光谱学相结合，以确定旋光法中的主要非径向模式f ₂，模式度ℓ  = 3，方位角阶m  = -3（在米_-Dziembowski 的约定）并确定星轴位置角为 25（或 205）±8°。旋转轴对视线的倾角是从偏振测量和光谱组合得出的约 46°，有助于识别其他模式并允许星震建模。这揭示了一颗 14.5 ± 0.5  M⊙的_恒星和一个包含约 28% 质量的对流核心——使 β Crucis 成为具有星震年龄的最大质量恒星。