太阳型接触双星BX Pegasi的再研究
The Solar-Type Contact Binary BX Pegasi Revisited
摘要：
我们提出了新的CCD测光的接触二进制BX钉，在连续三个月的2008年9月开始的结果。正如历史上的光变曲线一样，我们的观测显示了奥康奈尔效应，11月的数据本身就表明了非常短时间的亮度扰动的明确证据。对于这些变化，将模型点分别应用于第I组的两个数据集（9月至9月）。（10月）第二组（11月）。前者用次级光球上的一个冷点来描述，后者用两点模型来描述，一个冷点在冷星上，另一个热点在两颗星上。这些都是双星系统磁活动的一般表现。从Wilson-Devinney代码计算的20个光变曲线时间用于周期研究，以及所有其他最小时期。BX Peg复杂的周期变化可以分为长期周期减少，主要是由于磁性恒星风制动引起的角动量损失，由于低质量第三伴星轨道的光旅行时间（LTT）效应，以及以前未知的短期振荡。这最后一个周期调制可能是由第二个LTT轨道产生的，由于第四个机构的存在，周期约为16年，或由磁活动的影响，周期长度约为12年。
英文摘要：
We present the results of new CCD photometry for the contact binary BX Peg, made during three successive months beginning on September 2008. As do historical light curves, our observations display an O'Connell effect and the November data by themselves indicate clear evidence for very short-time brightness disturbance. For these variations, model spots are applied separately to the two data set of Group I (Sep.--Oct.) and Group II (Nov.). The former is described by a single cool spot on the secondary photosphere and the latter by a two-spot model with a cool spot on the cool star and a hot one on either star. These are generalized manifestations of the magnetic activity of the binary system. Twenty light-curve timings calculated from Wilson-Devinney code were used for a period study, together with all other minimum epochs. The complex period changes of BX Peg can be sorted into a secular period decrease caused dominantly by angular momentum loss due to magnetic stellar wind braking, a light-travel-time (LTT) effect due to the orbit of a low-mass third companion, and a previously unknown short-term oscillation. This last period modulation could be produced either by a second LTT orbit with a period of about 16 yr due to the existence of a fourth body or by the effect of magnetic activity with a cycle length of about 12 yr.
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