The Eclipsing δ Scuti Star EPIC 245932119
The Eclipsing δ Scuti Star EPIC 245932119
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DOI：
10.3847/1538-3881/aaf0fb
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发表时间：
2018-11
期刊：
影响因子：
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通讯作者：
Jae Woo Lee;K. Hong;M. Kristiansen
中科院分区：
文献类型：
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作者：
Jae Woo Lee;K. Hong;M. Kristiansen
我们展示了 EPIC 245932119 (Kp = +9.82) 的物理特性，通过 K2 光度测量显示出日食和脉动。二元模型表明，食系统处于分离或半分离构型，质量比分别为0.283和0.245，其光变参数几乎不受脉动影响。从观测数据中减去二元效应后，对外部主食阶段的光残差进行了多频率分析。我们在 0.62–6.28 day−1 和 19.36–24.07 day−1 两个区域检测到 35 个信噪比大于 4.0 的频率。其中，一些接近奈奎斯特极限fNy的高信号可能是真实脉动频率的反映(2)。低频区域中的所有频率（f8、f9、f14、f18、f24、f32）都是轨道谐波，三个高频（f19、f20、f22）似乎是从主频率 f1 = 22.77503 day−1 分裂出来的旁瓣。其中大多数被认为是由轨道频率引起的混叠效应。对于其他 26 个频率，脉动周期和脉动常数分别在 0.041-0.052 天和 0.013-0.016 天的范围内。这些值和赫罗图的位置表明主要部件是 δ Sct 脉动器。 EPIC 245932119 的观测特性与具有 δ Sct 型脉动分量的食双星的观测特性非常一致。
We present the physical properties of EPIC 245932119 (Kp = +9.82) exhibiting both eclipses and pulsations from the K2 photometry. The binary modeling indicates that the eclipsing system is in detached or semi-detached configurations with a mass ratio of 0.283 or 0.245, respectively, and that its light-curve parameters are almost unaffected by pulsations. Multiple frequency analyses were performed for the light residuals in the outside-primary eclipsing phase after subtracting the binarity effects from the observed data. We detected 35 frequencies with signal-to-noise amplitude ratios larger than 4.0 in two regions of 0.62–6.28 day−1 and 19.36–24.07 day−1. Among these, it is possible that some high signals close to the Nyquist limit fNy may be reflections of real pulsation frequencies (2 ). All frequencies (f8, f9, f14, f18, f24, f32) in the lower frequency region are orbital harmonics, and three high frequencies (f19, f20, f22) appear to be sidelobes split from the main frequency of f1 = 22.77503 day−1. Most of them are thought to be alias effects caused by the orbital frequency. For the 26 other frequencies, the pulsation periods and pulsation constants are in the ranges of 0.041–0.052 days and 0.013–0.016 days, respectively. These values and the position in the Hertzsprung–Russell diagram reveal that the primary component is a δ Sct pulsator. The observational properties of EPIC 245932119 are in good agreement with those for eclipsing binaries with δ Sct-type pulsating components.