ON THE PULSATIONAL–ORBITAL-PERIOD RELATION OF ECLIPSING BINARIES WITH δ-SCT COMPONENTS
ON THE PULSATIONAL–ORBITAL-PERIOD RELATION OF ECLIPSING BINARIES WITH δ-SCT COMPONENTS
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DOI：
10.1088/0004-637x/777/1/77
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发表时间：
2013-10
期刊：
影响因子：
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通讯作者：
X. Zhang;C. Luo;J. Fu
中科院分区：
文献类型：
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作者：
X. Zhang;C. Luo;J. Fu
本文根据近双星的洛希叶填充，推导出脉动星的脉动与轨道周期之间的理论关系。它似乎是一个简单的线性形式，与脉冲常数的函数的斜率，质量比，和填充因子为一个单独的系统。对69个已知的包含δ-Sct型分量的食双星的数据进行检验，得出Ppul-Porb关系的经验斜率为0.020 ± 0.006。进一步导出了食双星中δ-Sct星的Ppul/Porb比值的上限值为0.09 ± 0.02。这个值可以作为判别食双星中的变星是否以p模脉动的标准。应用推导出的Ppul-Porb关系，计算了食系统中37颗δ-Sct星的主脉动常数，并给出了光度解。这些周期在0.008到0.033天之间，平均值约为0.014天，这表明食双星中的δ-Sct星大多在第四或第五泛音中脉动。
We have deduced a theoretical relation between the pulsation and orbital-periods of pulsating stars in close binaries based on their Roche lobe filling. It appears to be of a simple linear form, with the slope as a function of the pulsation constant, the mass ratio, and the filling factor for an individual system. Testing the data of 69 known eclipsing binaries containing δ-Sct-type components yields an empirical slope of 0.020 ± 0.006 for the Ppul–Porb relation. We have further derived the upper limit of the Ppul/Porb ratio for the δ-Sct stars in eclipsing binaries with a value of 0.09 ± 0.02. This value could serve as a criterion to distinguish whether or not a pulsator in an eclipsing binary pulsates in the p-mode. Applying the deduced Ppul–Porb relation, we have computed the dominant pulsation constants for 37 δ-Sct stars in eclipsing systems with definite photometric solutions. These ranged between 0.008 and 0.033 days with a mean value of about 0.014 days, indicating that δ-Sct stars in eclipsing binaries mostly pulsate in the fourth or fifth overtones.