大陵型双星S Equulei和KO Aquilae的光谱研究：绝对参数和质量传递
A Spectroscopic Study of the Algol-type Binaries S Equulei and KO Aquilae: Absolute Parameters and Mass Transfer
摘要：
我们提出并分析了大陵五双星S Equ和KO Aql的高分辨率光谱。新的准确的径向速度的较热的主要成分得到。由于互相关程序，我们能够测量，第一次我们的知识，径向速度也为冷的二次组件的S Equ和KO Aql。将径向速度曲线的解和光变曲线的解相结合，得到了系统可靠的绝对参数。测量了S Equ和KO Aql较热分量的旋转速度，发现两个系统的增益器比同步旋转快约30%。这可能是由于从较冷部件到较热部件的拉格朗日L1点的质量传递。与相同质量的正常主序星相比，这些系统中质量增加部分的光度较低，这也可能是质量转移的影响。的H-α档案揭示了明确的证据，质量转移和吸积结构。在这两个系统中，我们清楚地观察到额外的吸收线。从这些特征的积分吸收和径向速度变化，我们发现，质量吸积是非常密集的碰撞区域周围的较热的组件。在日食之外，可以看到S Equ光谱中的双峰发射。这些峰中的一个可能起源于质心和较冷部件之间的区域，该区域被流动物质占据。此外，S Equ和KO Aql的H-α差谱也显示出发射特征，这应该是由较冷组分的磁活动引起的。
英文摘要：
We present and analyze high-resolution optical spectra of the Algol binaries S Equ and KO Aql. New accurate radial velocities for the hotter primary components are obtained. Thanks to the cross-correlation procedure, we were able to measure, for the first time to our knowledge, radial velocities also for the cool secondary components of S Equ and KO Aql. By combining the parameters obtained from the solution of the radial velocity curves with those obtained from the light curve analysis, reliable absolute parameters of the systems have been derived. The rotational velocity of the hotter components of S Equ and KO Aql has been measured and it is found that the gainers of both systems rotate about 30 % faster than synchronously. This is likely due to mass transfer across the Lagrangian L1 point from the cooler to the hotter component. The lower luminosity of the mass-gaining components of these systems compared to normal main-sequence stars of the same mass can be also an effect of the mass transfer. The H-alpha profiles reveal clear evidence of mass transfer and accretion structures. In both systems we clearly observed extra-absorption lines. From the integrated absorption and the radial velocity variations of these features, we found that the mass accretion is very dense around the impact region of the hotter components. A double-peaked emission in the spectra of S Equ was seen outside the eclipses. One of these peaks is likely originated in a region between the center of mass and the cooler component, which is occupied by the flowing matter. Furthermore, the H-alpha difference spectra of S Equ and KO Aql display also emission features, which should be arising from the magnetic activity of the cooler components.
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