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首页> 外文期刊>Astronomy and astrophysics >Planetary candidates around the pulsating sdB star KIC?5807616 considered doubtful
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Planetary candidates around the pulsating sdB star KIC?5807616 considered doubtful

机译：围绕sdB脉动星KIC？5807616的行星候选被怀疑

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Context. It has been suggested that two weak signals observed in the low frequency region of the Fourier transform amplitude spectra from the KIC 5807616 Q5-Q8 data can be interpreted as a result of the light reflection from planets orbiting the host star. Ever since the last results on KIC?5807616 were presented, the Kepler spacecraft has collected over two years of additional data, which we analysed using asteroseismological methods. Aims. To verify and improve on previous results, we used the Q?5-Q?17 Kepler data to identify pulsational modes, determine multiplet splitting, and to re-analyse the low frequency region between 33?49?μHz where two frequencies, claimed as the planetary signature, were found. Methods. Since Fourier transform amplitude spectra of the KIC?5807616 data do not show any clear multiplets, we used two stable acoustic modes to determine the theoretical width of gravity mode multiplets and their splittings. The period spacing and histograms of common multiplet component separations were used to identify pulsation modes and the observed gravity mode splittings. In the low frequency region, we analysed the amplitude variations of two planetary signature frequencies over the whole observing run. Results. We determined the rotational period of the star from the splittings. Analysis of the low frequency region shows that the amplitude and frequency change of the signals found there have similar characteristics to other gravity modes. Conclusions. New data allow for identifying gravity modes in a limited period range, as well as better rotational period estimations. We suggest that the so-called planetary signature frequencies found in previous work might instead be pulsation modes visible beyond the cut-off frequency of the star.
机译：上下文。已经提出，可以将来自KIC 5807616 Q5-Q8数据的傅立叶变换幅度谱的低频区域中观察到的两个微弱信号解释为来自环绕主恒星运行的行星的光反射的结果。自从提出有关KIC？5807616的最新结果以来，开普勒航天器已经收集了两年多的附加数据，我们使用了星震学方法对其进行了分析。目的为了验证和改进先前的结果，我们使用Q？5-Q？17开普勒数据识别脉动模式，确定多重分裂，并重新分析33？49？μHz之间的低频区域，其中两个频率称为发现了行星标志。方法。由于KIC？5807616数据的傅立叶变换幅度谱没有显示清晰的多重峰，因此我们使用了两个稳定的声学模式来确定重力模式多重峰及其分裂的理论宽度。常见多重组分分离的周期间隔和直方图用于识别脉动模式和观测到的重力模式分裂。在低频区域，我们分析了整个观测过程中两个行星特征频率的振幅变化。结果。我们根据裂隙确定了恒星的旋转周期。对低频区域的分析表明，在那里发现的信号的幅度和频率变化与其他重力模式具有相似的特性。结论。新的数据可以识别有限周期范围内的重力模式，以及更好的旋转周期估算。我们建议在先前的工作中发现的所谓行星特征频率可能是可见的脉动模式，超出了恒星的截止频率。

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