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arXiv 1202.0105astro-ph.SR
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FM星：脉动双星的傅立叶视图，一种光度测量径向速度的新技术

FM stars: A Fourier view of pulsating binary stars, a new technique for measuring radial velocities photometrically

Hiromoto Shibahashi, Donald W. Kurtz

备注：
15 pages, 14 figures, accepted for publication in MNRAS
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摘要：

有些脉动恒星是很好的时钟。当它们在双星中被发现时，它们的光度变化频率会受到轨道运动引起的多普勒效应的调制。对于每一个脉动频率，这表现为在恒星光变曲线的傅里叶变换中被轨道频率分离的多重态。我们推导的理论关系，利用数据的傅里叶变换，以获得所有的参数传统上提取的光谱径向速度，包括质量函数，这是很容易从第一轨道旁瓣的振幅比，每个脉动频率的中心频率。这是一种新的技术，从脉动频率的多普勒频移中产生径向速度，从而消除了获得频谱的需要。对于有脉动成分的双星，轨道解可以单独从光变曲线得到。我们给出了一个完整的推导，并证明它与人工数据，并与一个层次的食二进制与{ \it开普勒}任务数据，KIC 4150611（HD 181469）的情况下。我们表明，这是可能的，以我们的技术检测到的质量为100亿颗行星轨道$δ$ Sct和其他脉动恒星。我们还展示了如何区分轨道频率多重峰从潜在的类似的非径向$m$模式多重峰和斜脉动多重峰。

英文摘要：

Some pulsating stars are good clocks. When they are found in binary stars, the frequencies of their luminosity variations are modulated by the Doppler effect caused by orbital motion. For each pulsation frequency this manifests itself as a multiplet separated by the orbital frequency in the Fourier transform of the light curve of the star. We derive the theoretical relations to exploit data from the Fourier transform to derive all the parameters of a binary system traditionally extracted from spectroscopic radial velocities, including the mass function which is easily derived from the amplitude ratio of the first orbital sidelobes to the central frequency for each pulsation frequency. This is a new technique that yields radial velocities from the Doppler shift of a pulsation frequency, thus eliminates the need to obtain spectra. For binary stars with pulsating components, an orbital solution can be obtained from the light curve alone. We give a complete derivation of this and demonstrate it both with artificial data, and with a case of a hierarchical eclipsing binary with {\it Kepler} mission data, KIC 4150611 (HD 181469). We show that it is possible to detect Jupiter-mass planets orbiting $δ$ Sct and other pulsating stars with our technique. We also show how to distinguish orbital frequency multiplets from potentially similar nonradial $m$-mode multiplets and from oblique pulsation multiplets.

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