武仙座AM低态线剖面的新复杂性
New Complexities in the Low-State line profiles of AM Herculis
摘要：
当吸积暂时停止在极地AM她，发射线配置文件被称为开发几个不同的组件，其起源仍然知之甚少。这里报道的新的低态光谱具有比早期工作更有利的光谱分辨率（R~4500），时间分辨率（~3分钟曝光）和S/N的组合，揭示了线轮廓的轨道依赖性的额外细节。发现H-α的中心强特征由两个强度相似的分量组成，一个具有K~100 km/sec，并与副星的运动相关联，另一个具有很小或没有可检测的径向速度变化。我们属性的中心线组件附近的耦合区域的气体，也许与辐射的第二颗星的贡献。这两个卫星分量在中央强H-α峰两侧的RV偏移约为+/-250 km/sec。这些卫星最有可能出现在第二颗恒星附近的大型磁约束气体环中，这是由于供体恒星上的磁场活动和/或两颗恒星磁场的相互作用。多普勒地图显示，这两个卫星特征在与系统中L4和L5的速度位置相匹配的速度下具有浓度。
英文摘要：
When accretion temporarily ceases in the polar AM Her, the emission line profiles are known to develop several distinct components, whose origin remains poorly understood. The new low-state spectra reported here have a more favorable combination of spectral resolution (R~4500), time resolution (~3-min exposures), and S/N than earlier work, revealing additional details of the orbital dependence of the line profiles. The central strong feature of H-alpha is found to be composed of two components of similar strength, one having K~100 km/sec and phased with the motion of the secondary star, the other having little or no detectable radial velocity variations. We attribute the central line component to gas near the coupling region, perhaps with a contribution from irradiation of the secondary star. The two satellite components have RV offsets of ~+/-250 km/sec on either side of the central strong H-alpha peak. These satellites most likely arise in large loops of magnetically confined gas near the secondary star due to magnetic activity on the donor star and/or interactions of the magnetic fields of the two stars. Doppler maps show that these two satellite features have concentrations at velocities that match the velocity locations of L4 and L5 in the system.
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