The two variables in the triple system HR 6469 = V819 Her: One eclipsing, one spotted
The two variables in the triple system HR 6469 = V819 Her: One eclipsing, one spotted
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三重系统中的两个变量 HR 6469 = V819 Her：一是食色，一是斑点
DOI：
10.1086/116962
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发表时间：
1994
期刊：
影响因子：
--
通讯作者：
R. Tatum
中科院分区：
文献类型：
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作者：
W. Hamme;D. Hall;A. Hargrove;G. Henry;R. Wasson;W. S. Barkslade;S. Chang;R. Fried;C. L. Green;H. C. Lines;R. Lines;P. Nielsen;H. Powell;R. C. Reisenweber;C. W. Rogers;S. Shervais;R. Tatum
利用范德比尔特大学-田纳西州立大学（VU-TSU）自动望远镜14个夜晚的观测数据，给出了一个完整的BV光变曲线，并用Wilson-Devinney程序进行了求解。第三个光被评估，伴星星星在V中亮0.58（sup m），在B中亮0.11（sup m）。日食是日偏食。推断的颜色指数产生F2 V和F8 V的食对和G8 IV-III的遥远的伴星星星。在去除食变后，我们研究了G8 IV-III星星在1982 - 1992这10年间的剩余光变。每一年的光变曲线都用两点模型拟合。三个相对长寿的斑点被确定，与旋转周期85.9（sup d），85.9（sup d）和86.1（sup d）。这种微弱和间歇性的变化是可以理解的，因为G8 IV-III星星的罗斯比数处于开始出现严重斑点的阈值。
A complete BV light curve, from 14 nights of good data obtained with the Vanderbilt University-Tennessee State University (VU-TSU) automatic telescope, are presented and solved with the Wilson-Devinney program. Third light is evaluated, with the companion star brighter by 0.58(sup m) in V and 0.11(sup m) in B. The eclipses are partial. Inferred color indices yield F2 V and F8 V for the eclipsing pair and G8 IV-III for the distant companion star. After removing the variability due to eclipses, we study the residual variability of the G8 IV-III star over the ten years 1982 to 1992. Each yearly light curve is fit with a two-spot model. Three relatively long-lived spots are identified, with rotation periods of 85.9(sup d), 85.9(sup d), and 86.1(sup d). The weak and intermittent variability is understood because the G8 IV-III star has a Rossby number at the threshold for the onset of heavy spottedness.