An Updated Catalog of 4680 Northern Eclipsing Binaries with Algol-type Light-curve Morphology in the Catalina Sky Surveys
An Updated Catalog of 4680 Northern Eclipsing Binaries with Algol-type Light-curve Morphology in the Catalina Sky Surveys
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DOI：
10.3847/1538-4365/aad8a9
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发表时间：
2018-08
期刊：
影响因子：
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通讯作者：
A. Papageorgiou;M. Catelán;P. Christopoulou;A. Drake;S. Djorgovski
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作者：
A. Papageorgiou;M. Catelán;P. Christopoulou;A. Drake;S. Djorgovski
我们提出了一个更新的4680个北方食双星（EB）的目录，具有大陵五型光变曲线（LC）形态（即，利用卡塔利纳巡天的数据，我们可以清楚地看到初食和次食的开始和结束。我们的工作包括修订的周期确定，现象学参数的LC，和系统形态分类的基础上机器学习技术。虽然大多数新的周期与原始的卡塔利纳星表中提供的周期非常一致，但现在可以为10%的恒星提供改进的值。共有3456个EB被归类为分离型，449个被归类为半分离型，而145个不能明确地归类为任一亚型。大多数SD系统似乎是由短周期的Algols。通过应用颜色标准，我们在这些数据中寻找K型和M型矮星，并提出了一个子样本的609 EB候选人进行进一步的研究。我们报告了119个EB（占总样本的2.5%），这些EB在长时间尺度上表现出最大的正交光变化，周期范围为4.5-18年，分数光度变化范围为0.04-0.13。我们讨论了可能的原因，利用模型的变量星斑活动在我们的解释结果。
We present an updated catalog of 4680 northern eclipsing binaries (EBs) with Algol-type light-curve (LC) morphology (i.e., with well-defined beginnings and ends of primary and secondary eclipses), using data from the Catalina Sky Surveys. Our work includes revised period determinations, phenomenological parameters of the LCs, and system morphology classifications based on machine-learning techniques. While most of the new periods are in excellent agreement with those provided in the original Catalina catalogs, improved values are now available for ∼10% of the stars. A total of 3456 EBs were classified as detached and 449 were classified as semi-detached, while 145 could not be classified unambiguously into either subtype. The majority of the SD systems seem to be comprised of short-period Algols. By applying color criteria, we searched for K- and M-type dwarfs in these data, and present a subsample of 609 EB candidates for further investigation. We report 119 EBs (2.5% of the total sample) that show maximum quadrature light variations over long timescales, with periods bracketing the range 4.5–18 years and a fractional luminosity variance range of 0.04–0.13. We discuss possible causes for this, making use of models of variable starspot activity in our interpretation of the results.