Be星LQ And的快速光变  

RAPID LIGHT VARIATION OF BE STAR LQ AND

作　　者：杭恒荣[1] 陈亚峰 臧志云 黄磷[2] 郭子和[2] 郝晋新[2] 

机构地区：[1]中国科学院紫金山天文台,南京210008 [2]中国科学院北京天文台,北京100080

出　　处：《天文学报》1993年第4期351-358,共8页Acta Astronomica Sinica

基　　金：国家自然科学基金;中国科学院天文委员会的资助

摘　　要：1990年至1992年期间,本文作者用北京天文台兴隆站的60cm镜对LQ And作了UBV测光,取得了317组的观测数据,并结合1983年至1988年共479组数据进行了分析.结果表明:观测期间LQ And有稳定的快光变周期.新确定的光变周期同文献中给出的略有差别,为0.309418天.UBV photometric observations of LQ And were made at Beijing Astronomical Observatory with 60 cm telescope between 1990 and 1992. 317 data sets are obtained.HR9011 is used invariably as the comparison star. The Journal of the observations is presented in Table 1. In addition to these new observations, we have also analysed some published UBV measurements of LQ And secured during 1983—1988. To search for periods of light variation, the phase-fold CHI-square method was used. Figure 1 shows the searching for maximum CHI-square as a function of period. The phase diagrams of UBV data of LQ And for our best-fit period of 0.309418 day are displayed in Figure 2 and 3a with an epoch of HJD 2445621.5964 suggested by P. Harmanec [7]. Some phase diagrams of our data of LQ And for periods given by previous observers are also plotted in Figure 3b for comparison. Table 2 shows the differences in phase calculated with various periods between fixed epochs of minimum light. We suggest that the ephemeris for minimum light should be. T min. light=HJD 2445621.5964+0.309418(±0.000002)d*N. Figure 4 shows the phase diagrams of UBV data of LQ And for a period of 0.618836 day, which is two times of our best-fit period of 0.309418 day. Figure 5 shows the long term brightness variations in UBV (annual mean magnitude), indicating that the variation tendency in B was opposed to that in V and U.

关 键 词：BE星 LQ-And 快光变周期 

分 类 号：P145.2[天文地球—天体物理]