Towards a consistent model of the hot quadruple system HD 93206 = QZ Carinæ: I. Observations and their initial analyses
Towards a consistent model of the hot quadruple system HD 93206 = QZ Carinæ: I. Observations and their initial analyses
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走向热四联系统的一致模型 HD 93206 = QZ Cariné：I. 观察及其初步分析
DOI：
10.1051/0004-6361/202142108
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发表时间：
2022
影响因子：
6.5
通讯作者：
Chini, R.
中科院分区：
文献类型：
--
作者：
Mayer, P.;Harmanec, P.;Zasche, P.;Brož, M.;Catalan-Hurtado, R.;Barlow, B. N.;Frondorf, W.;Wolf, M.;Drechsel, H.;Chini, R.
热的九组分系统HD 93206，其中包含引力有界的食AC1+Ac2双星(P= 5.9987 d)和光谱AA1+AA2(P= 20.734 d)双星，可以为大质量恒星的起源和演化提供重要的见解。利用档案和新光谱，以及丰富的地面和空间光度观测资料，我们对这一天体进行了详细的研究。我们对短轨道的描述做了很大的改进，并很好地估计了两颗双星相互作用的周期约为14500d(即40年)。我们首次在光谱的光学区探测到了6.0d食双星较弱成分的弱线，测量了它们的径向速度，得到了MAc2/Mac1= 1.29的质量比，这与国际紫外探测器光谱的估算结果相反。我们确认，食相子系统Ac是半分离的，因此处于其组件之间的大规模质量转移阶段。罗氏叶填充和光谱亮度较高的AC1是两个分量中质量较小的一个，处于次极小值。我们发现，到目前为止被认为与食食系统有关的大部分Hα发射，都与20.73d光谱双星的主要O9.7i分量Aa1一起移动。然而，较高的巴尔默谱线的微弱发射似乎与Ac2分量周围的吸积盘有关。我们证明，可以获得准确的质量和其他基本物理性质，包括这个独特系统的距离，但需要更复杂的建模。向这一方向迈出的第一步载于所附文件二(ž等人)。
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 14 500 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 ofMAc2/MAc1= 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 Hαemission, so far believed to be associated with the eclipsing system, moves with the primary O9.7 I 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.).