论文标题
在十四个黯淡的二进制文件中检测到的轻度效果
Light-time effect detected in fourteen eclipsing binaries
论文作者
论文摘要
可用的14个选定要的二进制文件的最小时间（V1297 CAS，HD 24105，Ku Aur，Gu Cma，Gh Mon，Gh Mon，Gh Mon，az Vel，az Vel，di lyn，di lyn，dk her，gq dra，v624她，v1134她，V1134她，她，KIC 6187893，KIC 6187893，V1928，V1928 AQL，V246 CYG）。使用自动望远镜，调查和卫星数据，我们衍生了2500次日食，并伴随着我们自己的地面观测。这些数据用于检测这些多个系统中的周期变化。使用第三体假设和轻度时间效应描述了日食的时间变化。它们的周期分别为2.5、16.2、27、27、64、5.6、22、115、27、42、6.9、6.9、11.2、4.1和8.4岁，分别为这些系统。为每个系统计算了第三个身体的预测最小质量，我们在这里讨论它们的前瞻性可检测性。使用phoebe程序分析了HD 24105，GH MON，DK HER，V1134 HE，KIC 6187893，V1928 AQL和V2486 CYG的光曲线，导致组件的物理参数。在光曲线分析期间检测到了第三光的显着部分，支持我们对所有这些系统的三星级性质的假设。这些系统中的大多数（14个中的九个）已被称为视觉双打。我们的研究将它们转移到了可能的四倍体上，这使它们变得更加有趣。
The available minima timings of 14 selected eclipsing binaries (V1297 Cas, HD 24105, KU Aur, GU CMa, GH Mon, AZ Vel, DI Lyn, DK Her, GQ Dra, V624 Her, V1134 Her, KIC 6187893, V1928 Aql, V2486 Cyg) were collected and analyzed. Using the automatic telescopes, surveys, and satellite data, we derived more than 2500 times of eclipses, accompanied with our own ground-based observations. These data were used to detect the period variations in these multiple systems. The eclipse timing variations were described using the third-body hypothesis and the light-time effect. Their respective periods were derived as 2.5, 16.2, 27, 20, 64, 5.6, 22, 115, 27, 42, 6.9, 11.2, 4.1, and 8.4 years for these systems, respectively. The predicted minimal mass of the third body was calculated for each of the systems, and we discuss here their prospective detectability. The light curves of HD 24105, GH Mon, DK Her, V1134 Her, KIC 6187893, V1928 Aql, and V2486 Cyg were analyzed using the PHOEBE program, resulting in physical parameters of the components. Significant fractions of the third light were detected during the light-curve analysis, supporting our hypothesis of the triple-star nature of all these systems. The majority of these systems (nine out of 14) were already known as visual doubles. Our study shifts them to possible quadruples, what makes them even more interesting.
