密近双星系统的长期磁活动。I.颜色变化的模式
Long-term magnetic activity in close binary systems. I. Patterns of color variations
摘要：
我们提出的结果进行了长期的光度监测项目在卡塔尼亚天体物理观测站，旨在研究磁活动在密切的双星系统。我们提出了完整的观测数据集（38，000光电观测UBV）和调查的新结果的亮度和颜色变化的起源在近距离双星：AR Psc，VY Ari，UX Ari，V711 Tau，EI Eri，V1149 Ori，DH Leo，HU Vir，RS CVn，V775 Her，AR Lac，SZ Psc，II Peg和BY Dra。进行了相关和回归分析。我们发现存在两种不同的颜色变化模式。我们的样本中有八颗恒星：BY Dra，VY Ari，V775 Her，II Peg，V1149 Ori，HU Vir，EI Eri和DH Leo在变暗时变得更红。其他六颗恒星则表现出相反的行为，即它们变得更暗时变得更蓝。对于V711 Tau，这种行为可以解释为当较冷的组分变得较暗时，较早类型的组分的相对U-和B-通量贡献增加。另一方面，对于AR Psc，UX Ari，RS CVn，SZ Psc和AR Lac，必须援引热光球光斑的存在。我们还发现，在单线和双线双星中，暗成分是不活跃或活动少得多的V星等相关的B-V和U-B的颜色变化在60%以上的观测季节。的相关性被发现在不到40%的观测季节时，较暗的组件有一个不可忽略的活动水平和/或热光斑存在，但他们无论是空间或时间不相关的斑点。
英文摘要：
We present the results of a long-term photometric monitoring project carried out at Catania Astrophysical Observatory and aimed at studying magnetic activity in close binary systems. We present the complete observations dataset (38,000 photoelectric observations in UBV) and new results of an investigation on the origin of brightness and color variations observed in the close binary stars: AR Psc, VY Ari, UX Ari, V711 Tau, EI Eri, V1149 Ori, DH Leo, HU Vir, RS CVn, V775 Her, AR Lac, SZ Psc, II Peg and BY Dra. Correlation and regression analyses are carried out. We find the existence of two different patterns of color variations. Eight stars in our sample: BY Dra, VY Ari, V775 Her, II Peg, V1149 Ori, HU Vir, EI Eri and DH Leo become redder when they get fainter. The other six stars show the opposite behaviour, i.e. they become bluer when they get fainter. For V711 Tau this behaviour could be explained by the increased relative U- and B- flux contribution by the earlier-type component of the binary system when the cooler component gets fainter. On the other hand, for AR Psc, UX Ari, RS CVn, SZ Psc and AR Lac the existence of hot photospheric faculae must be necessarily invoked. We also found that in single-lined and double-lined binary stars in which the fainter component is inactive or much less active the V magnitude is correlated to B-V and U-B color variations in more than 60% of observation seasons. The correlation is found in less than 40% of observation seasons when the fainter component has a non-negligible level of activity and/or hot faculae are present but they are either spatially or temporally uncorrelated to spots.
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