PG激变星候选天体的光变曲线  

The Light Curves for PG CV Candidates

作　　者：陈建生[1] 蒋兆基[1] 李泳[1] 刘晓为 冯兴春[1] 

机构地区：[1]中国科学院北京天文台,北京100080

出　　处：《天体物理学报》1993年第3期225-232,共8页

基　　金：国家自然科学基金

摘　　要：我们于1989年用北京天文台兴隆观测站的60/90/180厘米施密特望远镜及Thomson红敏CCD对14个PG候选激变变星进行光度观测.其光变曲线特性表明:PG0027+260,PG0818+513,和PC1030+590为激变食变星,PG1341—079 是一个可能的激变食变星,PG1551+719为SU UM_a型矮新星,此外还有6个天体的光变曲线有激变星特有的闪变特征.因此PG样本中,激变变星的成功率为79％.PG1030+590的轨道周期为3~h279,PG1717+413的闪变变幅在二个月内有明显变化,它与本身的亮度无明显相关,说明闪变变幅的变化可能是亮斑的局部效应.This paper presents the observational result of the light curves for 14 PG cataclysmic variable candidates using the, 60/90/180 cm Schmidt Telescope and Thomson 576×384 CCD of Beijing Astronomical Observatory. The main results are:1. .3 candidates are shown to be CVB, which are PG0027 + 260, PG0818 + 513 and PG1030+ 590;2. One candidate PG1551 +719 is a SU UMa type CV;3. PG1341-079 is a possible CVB;4. 5 objects show definitely light flickering which is the characteristics of CV;g. The orbital period for PG1030 + 590 is determined from 5 observed minima, as P =3h.2792;6. The variation of the amplitude in flickering for PG1717 + 413 is significant in 2 month time-base line, and is not correlated with the magnitude of the object. It is suggested that the bright spot might be responsible for such phenomena;7. The probability of finding CV by using UVX and emission line technique is about 71%.

关 键 词：激变星 测光 光变曲线 侯选天体 

分 类 号：P145.2[天文地球—天体物理]