Long‐term photometric study of the W UMa binary star V523 Cas
Long‐term photometric study of the W UMa binary star V523 Cas
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DOI：
10.1111/j.1365-2966.2004.07200.x
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发表时间：
2004
影响因子：
4.8
通讯作者：
X. Zhang;R. Zhang
中科院分区：
文献类型：
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作者：
X. Zhang;R. Zhang
我们提出了一个长期的光电和电荷耦合器件（CCD）测光研究的短周期W UMa星星V523 Cas从1986年至2000年。研究了该双星系统的轨道周期变化和光变曲线变化。从我们的数据中获得了47个新的极小值时间。一个周期的研究，涵盖了超过43 000个周期的基础上的光电和CCD测光时间的最小值证实了长期的，长期的周期变化的系统。发现在过去的30年中，轨道周期以dP/dt = 8.84 × 10 −8 dy r −1的速率持续增加。从我们的结果中没有发现循环周期的变化。八个历元的观测形成了八条V和五条B全覆盖光变曲线。的光变曲线是W UMa型，并显示出显着的不对称与不等的最大值。在每个光变曲线的两个最大值之间的差异似乎是周期性的时间尺度约8年。基于单点模型，使用Wilson‐Devinney代码分析光变曲线。光度解决方案揭示了一个W-亚型，接触配置V523 Cas。测得光度质量比为0.51，
We present a long-term photoelectric and charge-coupled device (CCD) photometric study of the short-period W UMa star V523 Cas made from 1986 to 2000. The orbital-period changes and light-curve variations of the binary system are studied. 47 new times of minima are obtained from our data. A period study covering more than 43 000 cycles based on the photoelectric and CCD photometric times of minima confirms the long-term, secular period changes of the system. It is found that the orbital period has been continuously increasing in the past three decades at a rate of dP/dt = 8.84 × 10 −8 dy r −1 . No cyclic period variations are found from our result. Eight V and five B completely covered light curves are formed from the observations made in eight epochs. The light curves are of W UMa type and show marked asymmetries with unequal maxima. The differences between the two maxima in each light curve appear to be cyclic over a time-scale of about 8 yr. Based on a one-spot model, the light curves are analysed with the Wilson‐Devinney code. The photometric solutions reveal a W-subtype, contact configuration for V523 Cas. The photometric mass ratio is found to be 0.51, and the