论文标题
Epsilon CRA的时间序列光谱。通过扩展功能分析的518 nm mg i三元组区域
Time sequence spectroscopy of Epsilon CrA. The 518 nm Mg I triplet region analyzed with Broadening Functions
论文作者
论文摘要
使用在两周内四个完整和四个部分夜晚获得的时间监测序列获得的W UMA型二元二元epsilon CRA的高分辨率光谱观察已被用于得出系统的轨道元素，并讨论了卢比模型的有效性，以描述径向效率数据的描述。与接触二进制二进制AW UMA的类似时间序列观察相比，观察结果具有更广泛的时间覆盖范围和更好的质量。这两个二进制文件具有几种物理特性，两者都显示出与露西模型非常相似的偏差：主要成分是一个快速旋转的恒星几乎不受二级成分的存在影响，而后者则嵌入复杂的气流中，并且似乎具有其自身的旋转效率 - 与模型的矛盾。发现光谱质量比大于从光曲线分析中得出的质量比，与许多其他W UMA型二进制文件类似，但是Epsilon CRA的这种差异相对较小，这表明了一种通常会影响其他确定的观察方法的系统问题。复杂速度流的存在与实体旋转假设相矛盾，这表明对露西模型进行了修改，这可能沿Stepien（2009）（2009）概述的二进制组件之间的能量传递的概念。
High-resolution spectroscopic observations of the W UMa-type binary Epsilon CrA obtained as a time monitoring sequence on four full and four partial nights within two weeks have been used to derive orbital elements of the system and discuss the validity of the Lucy model for description of the radial-velocity data. The observations had more extensive temporal coverage and better quality than similar time-sequence observations of the contact binary AW UMa. The two binaries share several physical properties with both showing very similar deviations from the Lucy model: The primary component is a rapidly-rotating star almost unaffected by the presence of the secondary component, while the latter is embedded in a complex gas flow and appears to have its own rotation-velocity field, in contradiction to the model. The spectroscopic mass ratio is found to be larger than the one derived from the light-curve analysis, similarly as in many other W UMa-type binaries, but this discrepancy for Epsilon CrA is relatively minor suggesting a systematic problem with one of the observational methods commonly affecting other determinations. The presence of the complex velocity flows contradicting the solid-body rotation assumption suggest a necessity of modification to the Lucy model, possibly along the lines outlined by Stepien (2009) in his concept of the energy transfer between the binary components.
