色球活动

自从1976年，Hall明确地提出RsCVn型双星的定义以来，密近双星的类太阳活动（也叫色球活动或磁活动）性质就引起众多天文工作者的极大兴趣。

Since RS CVn-type binary was defined by Hall in 1976 , the solar-type activity (" chromospheric activity " or " magnetic activity ") of contact binaries interests many astronomic researchers .

ⅡPeg的色球活动很强烈，有明显的自转调制现象，在我们观测的每个自转周里都有耀斑事件发生，且这样的耀斑事件是贯穿整个色球层的。

The chromospheric activity of II Peg is very strong , and exhibits an obvious rotational modulation phenomenon . The optical flare is happened In every rotational period , and it is through each layer of the chromosphere .

1984年2月14日大角星色球活动的CaⅡH，K线观测

Chromospheric Activity of Arcturus Observed at Call H and K Lines on February 14 , 1984

类太阳色球活动星εEri磁场的观测研究

An observation study of the magnetic field on the solar-like chromosphere active star ε eri

晚型矮星的色球活动

Chromospheric Activity of Late - type Dwarf Stars

演化恒星的色球活动与恒星自转周期间存在很好的相关性。

The relation between stellar chromospheric activity and rotation of evolution stars have a good relativity .

但是细致分析显示演化恒星色球活动水平随恒星自转周期间的分布对恒星光谱型和恒星表面有效温度有很强的依赖，并对这些现象提出了几种可能的解释。

But meticulous analysis show chromospheric activity of evolution stars depend on stellar spectral type and effective temperature strongly .

该系统的光球活动和色球活动是相互联结的，光学耀斑和黑子活动区在空间上有着一一对应的关系，说明这些活动源于同一个磁流管。

This has told us that the photospheric activity and chromospheric activity origin from the same magnetic flux tube .

然后，借助多普勒成像技术得出了这两颗恒星的光球黑子活动区的结构，利用综合光谱减技术计算了它们的色球活动指标。

Then , we have obtained the structure of photospheric spot active regions for above two stars by using Doppler imaging technique , and their chromospheric activity indicators with the aid of synthesized spectral subtraction technique .

分析认为我们观测到的是大角星的一次以天计的短时标色球剧烈活动，它伴随着物质的向外抛射，也引起星周物质的向外运动。

Our conclusion is that we happened to observe an intensive short time-scale activity of the chromosphere of Arcturus characterized by mass outflow and outward motions of circumstellar matter .