相互作用双星RY Scuti质量外流的光谱研究
A Spectroscopic Study of Mass Outflows in the Interacting Binary RY Scuti
摘要：
大质量相互作用双星RY Scuti是一个活跃的质量转移系统的重要代表，这个系统在我们的眼前正在发生变化，它可能是通过潮汐剥离形成沃尔夫-拉叶星的一个例子。利用新的和以前发表的光谱，我们提出的例子说明吸收和发射功能的数量如何变化的二元轨道。我们确定了与每个组件相关的光谱特征，计算了一个新的双线光谱双星轨道，并发现明亮的超巨星质量为7.1 +/- 1.2 M太阳，隐藏的大质量伴星质量为30.0 +/- 2.1 M太阳。通过层析重建的组成光谱的复合光谱，我们确认了O9.7 Ibpe光谱类的明亮的超巨星，并发现了B0.5 I光谱与隐藏的大质量的同伴，但是，我们建议，后者实际上是光谱的吸积环的光球立即周围的大质量的同伴。我们在最近的beta Lyr流体动力学模型的背景下描述了系统质量损失流的复杂性质，这使我们得出结论，RY Scuti以两种方式离开系统：1）隐藏的大质量伴星产生的风的两极外流，2）明亮的O9.7 Ibpe超巨星的质量从L2点附近的区域流出，致密环双星盘这个环双星盘（半径约1天文单位）可能为周围的双环形星云（半径约2000天文单位）提供食物。
英文摘要：
The massive interacting binary RY Scuti is an important representative of an active mass-transferring system that is changing before our eyes and which may be an example of the formation of a Wolf-Rayet star through tidal stripping. Utilizing new and previously published spectra, we present examples of how a number of illustrative absorption and emission features vary during the binary orbit. We identify spectral features associated with each component, calculate a new, double-lined spectroscopic binary orbit, and find masses of 7.1 +/- 1.2 M_sun for the bright supergiant and 30.0 +/- 2.1 M_sun for the hidden massive companion. Through tomographic reconstruction of the component spectra from the composite spectra, we confirm the O9.7 Ibpe spectral class of the bright supergiant and discover a B0.5 I spectrum associated with the hidden massive companion; however, we suggest that the latter is actually the spectrum of the photosphere of the accretion torus immediately surrounding the massive companion. We describe the complex nature of the mass loss flows from the system in the context of recent hydrodynamical models for beta Lyr, leading us to conclude RY Scuti has matter leaving the system in two ways: 1) a bipolar outflow from winds generated by the hidden massive companion, and 2) mass from the bright O9.7 Ibpe supergiant flowing from the region near the L2 point to fill out a large, dense circumbinary disk. This circumbinary disk (radius ~ 1 AU) may feed the surrounding double-toroidal nebula (radius ~ 2000 AU).
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