热四极系统HD 93206 = QZ的一致模型意见及其初步分析
Towards a consistent model of the hot quadruple system HD 93206 = QZ Carinae - I. Observations and their initial analyses
摘要：
热九分量系统HD 93206包含一个引力束缚食Ac 1 + Ac 2双星（$P=5.9987$ ~d）和一个光谱Aa 1 + Aa 2双星（$P=20.734$ ~d），它可以为研究大质量恒星的起源和演化提供重要的信息。利用档案和新的光谱，以及丰富的地面和空间光度观测，我们对这个物体进行了详细的研究。我们提供了一个更好的描述，这两个短轨道和一个很好的估计的共同周期的两个双星约14500~d（即40年）。首次在6.0 d食双星的光谱光学区探测到较暗分量的弱线，测量了它们的视向速度，并导出了$M_{\rm Ac2}/M_{\rm Ac1}=1.29$的质量比，这与国际紫外探测器（IUE）光谱估计的结果相反。我们确认，食子系统Ac是半分离的，因此，在其组件之间的大规模质量转移的阶段。充满罗奇瓣的光谱上较亮的分量Ac 1质量较轻，在次极小期被食。我们发现，大部分的\ha发射，迄今被认为是与食系统，移动的主要O9.7I成分Aa 1的20.73天的光谱双星。然而，在较高的巴耳末线的弱发射似乎与组件Ac 2周围的吸积盘。我们证明，可以获得准确的质量和其他基本的物理性质，包括这个独特的系统的距离，但需要一个更复杂的建模。在随附的论文~II（Brozin等人）中提出了朝着这个方向迈出的第一步。
英文摘要：
The hot nine-component system HD 93206, which contains a gravitationally bounded eclipsing Ac1+Ac2 binary ($P=5.9987$~d) and a spectroscopic Aa1+Aa2 ($P=20.734$~d) binary can provide~important insights into the origin and evolution of massive stars. Using archival and new spectra, and a~rich collection of ground-based and space photometric observations, we carried out a detailed study of this object. We provide a much improved description of both short orbits and a good estimate of the mutual period of both binaries of about 14500~d (i.e. 40 years). For the first time, we detected weak lines of the fainter component of the 6.0~d eclipsing binary in the optical region of the spectrum, measured their radial velocities, and derived a mass ratio of $M_{\rm Ac2}/M_{\rm Ac1}=1.29$, which is the opposite of what was estimated from the International Ultraviolet explorer (IUE) spectra. We confirm that the eclipsing subsystem Ac is semi-detached and is therefore in a phase of large-scale mass transfer between its components. The Roche-lobe filling and spectroscopically brighter component Ac1 is the less massive of the two and is eclipsed in the secondary minimum. We show that the bulk of the \ha emission, so far believed to be associated with the eclipsing system, moves with the primary O9.7I component Aa1 of the 20.73~d spectroscopic binary. However, the weak emission in the higher Balmer lines seems to be associated with the accretion disc around component Ac2. We demonstrate that accurate masses and other basic physical properties including the distance of this unique system can be obtained but require a more sophisticated modelling. A~first step in this direction is presented in the accompanying Paper~II (Brož et al.).
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