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首页> 外文期刊>The Astrophysical journal >TOMOGRAPHIC SEPARATION OF COMPOSITE SPECTRA. Ⅷ. THE PHYSICAL PROPERTIES OF THE MASSIVE COMPACT BINARY IN THE TRIPLE STAR SYSTEM HD 36486 (δ ORIONIS A)
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TOMOGRAPHIC SEPARATION OF COMPOSITE SPECTRA. Ⅷ. THE PHYSICAL PROPERTIES OF THE MASSIVE COMPACT BINARY IN THE TRIPLE STAR SYSTEM HD 36486 (δ ORIONIS A)

机译：层析分离复合光谱。 Ⅷ。三重星系HD 36486（δOrionis A）中大型紧缩双星的物理性质

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We present the first double-lined spectroscopic orbital elements for the central binary in the massive triple δ Orionis A. The solutions are based on fits of cross-correlation functions of IUE high-dispersion UV spectra and He Ⅰ λ6678 profiles. The orbital elements for the primary agree well with previous results, and in particular, we confirm the apsidal advance with a period of 224.5 +- 4.5 yr. We also present tomographic reconstructions of the primary and secondary stars' spectra that confirm the O9.5 Ⅱ classification of the primary and indicate a B0.5 Ⅲ type for the secondary. The relative line strengths between the reconstructed spectra suggest magnitude differences of Δm = -2.5 log (F_s/F_p) = 2.6 +- 0.2 in the UV and Δm = 2.5 +- 0.3 at 6678 A. The widths of the UV cross-correlation functions are used to estimate the projected rotational velocities, V sin i = 157 +- 6 and 138 +- 16 km s~(-1) for the primary and secondary, respectively (which implies that both the primary and the secondary rotate faster than the orbital motion). We used the spectroscopic results to make a constrained fit of the Hipparcos light curve of this eclipsing binary, and the model fits limit the inclination to the range i = 67 °-77 °. The lower limitcorresponds to a near Roche-filling configuration that has an absolute magnitude that is consistent with the photometrically determined distance to Ori OB1b, the Orion Belt cluster in which δ Ori resides. The i = 67 ° solution results in masses of M_p = 11.2 and M_s = 5.6 solar mass, both of which are substantially below the expected masses for stars of their luminosity. The binary may have experienced a mass ratio reversal caused by case A Roche lobe overflow or the system may have suffered extensive mass loss through a binary interaction (perhaps during a common envelope phase) in which most of the primary's mass was lost from the system rather than transferred to the secondary. We also made three-component reconstructions to search for the presumed stationary spectrum of the close visual companion δ Ori Ab (Hei 42 Ab). There is no indication of the spectral lines of this tertiary in the UV spectrum, but a broad and shallow feature is apparent in the reconstruction of He ? λ6678 indicative of an early B-type star. The tertiary may be a rapid rotator (V sin i ≈ 300 km s~(-1)) or a spectroscopic binary.
机译：我们提出了大规模三重δOrionis A中中心双星的第一个双线光谱轨道元素。这些解决方案基于IUE高色散UV光谱和HeⅠλ6678轮廓的互相关函数的拟合。小行星的轨道元素与先前的结果非常吻合，特别是，我们确认了224.5±4.5年的两栖动物前进。我们还提供了对原初和次要恒星光谱的层析成像重建，证实了原初O9.5Ⅱ的分类，并指出了次生恒星的B0.5Ⅲ类型。重建的光谱之间的相对线强度表明，在UV中，Δm= -2.5 log（F_s / F_p）= 2.6 +-0.2，在6678 A时，Δm= 2.5 +-0.3的幅度差异。UV互相关函数的宽度分别用于估算初级和次级的预计旋转速度V sin i = 157 + -6和138 +-16 km s〜（-1）（这意味着初级和次级旋转均快于轨道运动）。我们使用光谱结果对该日蚀双星的Hipparcos光曲线进行了约束拟合，并且模型拟合将倾斜度限制在i = 67°-77°范围内。下限对应于具有绝对光度的近罗氏填充构型，该绝对量与通过光度法确定的距Ori OB1b（δOri所在的Orion Belt团簇）的距离一致。 i = 67°的解得到的质量为M_p = 11.2和M_s = 5.6太阳质量，两者均大大低于其光度恒星的预期质量。二进制可能经历了Roche瓣溢出引起的质量比逆转，或者系统可能由于二进制交互作用（可能在公共包络阶段）遭受了广泛的质量损失，其中大部分初级质量都从系统中损失了，而不是比转移到中学。我们还进行了三部分重构，以寻找接近的视觉伴侣δOri Ab（Hei 42 Ab）的假定平稳光谱。在UV光谱中没有显示该叔分子的谱线的迹象，但是在He的重建中很明显有一个宽而浅的特征。表示早期B型星的λ6678。第三级可以是快速旋转器（V sin i≈300 km s〜（-1））或分光镜二进制。

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