W UMa型相接双星V523 Cas测光研究  

Study on Photometry of the W UMa System V523 Cas

作　　者：邢丽峰[1] 吴杰[1] 

机构地区：[1]郑州轻工业学院技术物理系,郑州450002

出　　处：《佳木斯大学学报（自然科学版）》2009年第4期620-621,共2页Journal of Jiamusi University：Natural Science Edition

基　　金：国家自然科学基金(10878015);郑州轻工业学院博士基金资助项目

摘　　要：对V523 Cas(W UMa型)相接双星系统进行了测光观测,并通过IRAF软件经行了测光处理,获得了其自转周期.双星系统的掩食过程中主极小和次主极小红化分别为0m.07和0m.06;主极大与相随的次主极大在V和B波段分别相差0m.018和0m.022,V523 Cas为非对称的短周期W UMa型相接双星.The light variations of the W UMa system V523 Cas were monitored. In our observations the system showed appreciable periodic light variability. By using the methods of the Phase Dispersion Minimization （PDM） and Fourier analysis （PERIOD04）, the rotational periods of these stars were determined. The color curve indicates that the system becomes redder by 0^m. 07 and 0^m. 06 during primary and secondary eclipse, respectively. This indicates that regions of cooler gas are visible at such times. The maximum following the secondary minimum is 0^m. 022 brighter in B and 0^m .018 bright in V.

关 键 词：天体物理 相接双星 光变周期 

分 类 号：P144.1[天文地球—天体物理]