斑点食双星CV Bootis的绝对性质
Absolute properties of the spotted eclipsing binary star CV Bootis
摘要：
我们提出了新的V波段差分亮度测量以及新的径向速度测量的分离，圆形，0.84天的周期，双线食双星系统CV Boo。这些数据以及其他观测从文献中结合起来，以获得改进的绝对尺寸的恒星的目的，测试各个方面的理论建模。尽管我们在系统中检测到固有变异性的并发症，尽管组件的快速旋转，我们能够确定的绝对质量和半径分别优于1.3%和2%。对于较热、较大、质量较大的主星（恒星A），我们得到M（A）= 1.032 +/-0.013 M（太阳）和R（B）= 1.262 +/- 0.023 R（太阳）;对于伴星，我们得到M（B）= 0.968 +/- 0.012 M（太阳）和R（B）= 1.173 +/- 0.023 R（太阳）。估计的有效温度为5760 +/- 150 K和5670 +/- 150 K。周期比轨道周期短约1%的固有变化被解释为是由于一个或两个组件上的斑点的调制。这意味着斑点星的旋转速度必须比同步速率快，这与当前潮汐演化模型的预测不一致，根据该模型，两颗恒星应该同步。我们还发现，次级恒星的半径比恒星演化计算的预期大约10%，这一差异也见于其他（大多是低质量和活跃的）食双星。我们估计该系统的年龄约为9 Gyr。这两个成分都接近其主序阶段的结束，主序阶段可能已经开始了外壳的氢燃烧阶段。
英文摘要：
We present new V-band differential brightness measurements as well as new radial-velocity measurements of the detached, circular, 0.84-day period, double-lined eclipsing binary system CV Boo. These data along with other observations from the literature are combined to derive improved absolute dimensions of the stars for the purpose of testing various aspects of theoretical modeling. Despite complications from intrinsic variability we detect in the system, and despite the rapid rotation of the components, we are able to determine the absolute masses and radii to better than 1.3% and 2%, respectively. We obtain M(A) = 1.032 +/- 0.013 M(Sun) and R(B) = 1.262 +/- 0.023 R(Sun) for the hotter, larger, and more massive primary (star A), and M(B) = 0.968 +/- 0.012 M(Sun) and R(B) = 1.173 +/- 0.023 R(Sun) for the secondary. The estimated effective temperatures are 5760 +/- 150 K and 5670 +/- 150 K. The intrinsic variability with a period about 1% shorter than the orbital period is interpreted as being due to modulation by spots on one or both components. This implies that the spotted star(s) must be rotating faster than the synchronous rate, which disagrees with predictions from current tidal evolution models according to which both stars should be synchronized. We also find that the radius of the secondary is larger than expected from stellar evolution calculations by about 10%, a discrepancy also seen in other (mostly lower-mass and active) eclipsing binaries. We estimate the age of the system to be approximately 9 Gyr. Both components are near the end of their main-sequence phase, and the primary may have started the shell hydrogen-burning stage.
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