致密的分子小球和尘埃弧朝向逃逸的O星AE Aur（HD 34078）
Dense molecular globulettes and the dust arc towards the runaway O star AE Aur (HD 34078)
摘要：
一些逃逸恒星在其周围显示出红外线的弧形结构，这是由于它们与周围的星际物质相互作用的结果。这些特征的性质以及它们形成的过程仍然知之甚少。我们的目标是了解的物理机制，形状的尘埃弧附近观察到的失控O星AEAur（HD 34078）。我们获得并分析了以HD 34078为中心的CO（1-0）发射的高空间分辨率地图，该地图结合了IRAM干涉仪和30米单碟天线的数据。朝向HD 34078的视线与检测到的小球状体之一的外部相交，这解释了在现场观察到的漫射UV光的性质和在HD 34078的光谱中检测到的许多分子吸收线，包括来自高度激发的H2的吸收线。它们与恒星的模型距离与它们位于3D抛物面上的事实是一致的，这符合24 μm斯皮策图像中检测到的弧形。另外四个紧凑的CO小球在映射区检测。这些小球具有高密度和线宽，并且是强压力限制或瞬态的。CO小球状体和红外线弧之间良好的空间相关性表明，它们是由HD 34078发出的辐射和风与周围气体相互作用的结果。然而，这种互动的细节仍不清楚。一个风的质量损失率显着大于从紫外线推断的值是有利的大红外线弧的大小，但不容易解释的CO小球的低速度。辐射压力对尘埃颗粒的影响在解释观测结果时也遇到了几个问题。需要进一步的观测和理论工作，以充分阐明的过程中形成的气体和尘埃的弓形冲击周围失控的O型星。（节录）
英文摘要：
Some runaway stars are known to display IR arc-like structures around them, resulting from their interaction with surrounding interstellar material. The properties of these features as well as the processes involved in their formation are still poorly understood. We aim at understanding the physical mechanisms that shapes the dust arc observed near the runaway O star AEAur (HD34078). We obtained and analyzed a high spatial resolution map of the CO(1-0) emission that is centered on HD34078, and that combines data from both the IRAM interferometer and 30m single-dish antenna. The line of sight towards HD34078 intersects the outer part of one of the detected globulettes, which accounts for both the properties of diffuse UV light observed in the field and the numerous molecular absorption lines detected in HD34078's spectra, including those from highly excited H2 . Their modeled distance from the star is compatible with the fact that they lie on the 3D paraboloid which fits the arc detected in the 24 μm Spitzer image. Four other compact CO globulettes are detected in the mapped area. These globulettes have a high density and linewidth, and are strongly pressure-confined or transient. The good spatial correlation between the CO globulettes and the IR arc suggests that they result from the interaction of the radiation and wind emitted by HD 34078 with the ambient gas. However, the details of this interaction remain unclear. A wind mass loss rate significantly larger than the value inferred from UV lines is favored by the large IR arc size, but does not easily explain the low velocity of the CO globulettes. The effect of radiation pressure on dust grains also meets several issues in explaining the observations. Further observational and theoretical work is needed to fully elucidate the processes shaping the gas and dust in bow shocks around runaway O stars. (Abridged)
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