We present Transiting Exoplanet Survey Satellite (TESS) photometry of the triple star system V1031 Ori (AB)C, which exhibits short-period oscillations superimposed on an eclipsing light curve.The high-quality data were analyzed in detail and combined with the published spectroscopic measurements to obtain the fundamental stellar parameters of the program target. The masses and radii of the eclipsing pair (AB) were determined to about $0.5\%$ and $0.7\%$ precision, respectively. We found 23 significant frequencies in two ranges of <2 d−1 and 10.9–12.7 d−1 from the eclipse-subtracted residuals. Among them, 16 in the gravity (g)-mode region may be aliases and artefacts due to imperfect removal of the systematic trends and the binary effects from the TESS data. Seven frequencies in the pressure (p)-mode region were separated by the orbital frequency and split by an average offset of 0.042 ± 0.003 d−1 from their adjacent harmonics. Further, the pulsation amplitudes are clearly modulated with the binary star orbit. The results indicate that the p-mode frequencies are tidally perturbed pulsations from the secondary component and the pulsation axis could be aligned with the tidal axis.

中文翻译：

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层次三重系统 V1031 Orionis 中的潮汐扰动倾斜脉动

我们展示了三合星系统 V1031 Ori (AB)C 的凌日系外行星测量卫星 (TESS) 光度测量，它显示出叠加在食光曲线上的短周期振荡。对高质量数据进行了详细分析，并结合已发表的光谱测量以获得计划目标的基本恒星参数。食对 (AB) 的质量和半径分别确定为大约 $0.5\%$ 和 $0.7\%$ 精度。我们从蚀减残差中发现了 23 个显着频率在 <2 d-1 和 10.9-12.7 d-1 的两个范围内。其中，重力（g）模式区域中的 16 个可能是由于系统趋势和 TESS 数据的二元效应去除不完善而造成的混叠和伪影。压力 (p) 模式区域中的七个频率被轨道频率隔开，并被与其相邻谐波的 0.042 ± 0.003 d-1 的平均偏移量分开。此外，脉动幅度明显受到双星轨道的调制。结果表明，p 模式频率是来自次要分量的潮汐扰动脉动，并且脉动轴可以与潮汐轴对齐。