食双星的绝对尺寸。XXVI。设定新标准：F型系统AD Bootis、VZ Hydrae和WZ Ophiuchi的质量、半径和丰度
Absolute dimensions of eclipsing binaries. XXVI. Setting a new standard: Masses, radii, and abundances for the F-type systems AD Bootis, VZ Hydrae, and WZ Ophiuchi
摘要：
我们确定的绝对尺寸和丰度的三个F型主序星分离食双星AD布，VZ Hya，WZ Oph和最近的恒星演化模型的结果进行了详细的比较。紫外光变曲线和标准光度测定法在欧洲南方天文台获得，径向速度观测在CfA设施，高分辨率光谱与欧洲南方天文台的FEROS摄谱仪。采用最先进的方法进行分析。已经为组件建立了分别精确到0.5-0.7%和0.4- 0.9%的质量和半径，其范围为1.1至1.4 M_sun和1.1至1.6 R_sun。[Fe/H]丰度在-0.27 ~+0.10之间，不确定度在0.07 ~ 0.15 dex之间。我们发现WZ Oph的α-元素丰度略高于[α/Fe] ~+0.1 $。AD Boo的次要组分和WZ Oph的两种组分似乎具有轻微活性。Yale-Yonsai和Riza-Regina进化模型几乎同样适合AD Boo和VZ Hya的组成部分，假设同时代形成，年龄约为1.75/1.50 Gyr（AD Boo）和1.25/1.00 Gyr（VZ Hya）。然而，BaSTI模型预测的主要和次要成分的年龄略有不同。对于WZ Oph，所有三个网格的模型都比观测到的要热得多。低He含量，降低的包层对流加上表面活动，和/或更高的星际吸收将消除差异，但其原因尚未明确确定。我们已经证明了使用食双星来测试和比较最近恒星演化模型的能力，前提是它们的丰度是已知的。最大的限制和挑战是由T_eff和星际吸收测定，以及它们对丰度结果的影响和相关性。
英文摘要：
We determine absolute dimensions and abundances for the three F-type main-sequence detached eclipsing binaries AD Boo, VZ Hya, and WZ Oph and perform a detailed comparison with results from recent stellar evolutionary models. uvby light curves and standard photometry were obtained at ESO,radial velocity observations at CfA facilities, and high-resolution spectra with ESO's FEROS spectrograph. State-of-the-art methods were applied for the analyses. Masses and radii that are precise to 0.5-0.7% and 0.4-0.9%, respectively, have been established for the components, which span the ranges of 1.1 to 1.4 M_sun and 1.1 to 1.6 R_sun. The [Fe/H] abundances are from -0.27 to +0.10, with uncertainties between 0.07 and 0.15 dex. We find indications of a slight alpha-element overabundance of [alpha/Fe] ~ +0.1$ for WZ Oph. The secondary component of AD Boo and both components of WZ Oph appear to be slightly active. Yale-Yonsai and Victoria-Regina evolutionary models fit the components of AD Boo and VZ Hya almost equally well, assuming coeval formation, at ages of about 1.75/1.50 Gyr (AD Boo) and 1.25/1.00 Gyr (VZ Hya). BaSTI models, however, predict somewhat different ages for the primary and secondary components. For WZ Oph, the models from all three grids are significantly hotter than observed. A low He content, decreased envelope convection coupled with surface activity, and/or higher interstellar absorption would remove the discrepancy, but its cause has not been definitively identified. We have demonstrated the power of testing and comparing recent stellar evolutionary models using eclipsing binaries, provided their abundances are known. The strongest limitations and challenges are set by T_eff and interstellar absorption determinations, and by their effects on and correlation with abundance results.
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