星际气泡破裂时辐射压力驱动的尘埃波
Radiation-pressure-driven dust waves inside bursting interstellar bubbles
摘要：
大质量恒星通过它们的辐射能和机械能输入来驱动星际介质的演化。诞生后，它们形成被致密外壳包围的热气泡。传统上，气泡的形成是通过强大的恒星风的输入来解释的，尽管缺乏支持这种情况的直接证据。在这里，我们探讨了斯皮策和赫歇尔太空望远镜所看到的星际气泡的可能性，这些气泡是由log（L/L_sun）< 5.2的恒星吹出的，由于伴随着周围气体电离的热压而形成和膨胀。我们表明，密度梯度的出生云或穿刺扫壳导致电离气体流通过气泡进入一般的星际介质，这是由附近的恒星尘埃波跟踪，表明在这一阶段的辐射压力的重要性。尘埃波为H II气泡内尘埃的存在提供了一个自然的解释，提供了一种新的方法来研究H II区域的尘埃，并提供了直接的证据，表明气泡通过香槟流将压力释放到ISM中，作为大质量恒星与周围环境辐射相互作用的探针。我们创建了一个参数空间连接的环境密度，电离源的光度，和尘埃波的位置，同时使用研究的H II气泡RCW 120和RCW 82作为我们的模型的基准。最后，我们简要地研究了我们的研究的影响，在超亮红星系团（ULIRGs），合并星系和早期宇宙，这发生在非常明亮和密集的环境中，辐射压力预计将占主导地位的动力学演化形成的超级星团的环境。
英文摘要：
Massive stars drive the evolution of the interstellar medium through their radiative and mechanical energy input. After their birth, they form bubbles of hot gas surrounded by a dense shell. Traditionally, the formation of bubbles is explained through the input of a powerful stellar wind, even though direct evidence supporting this scenario is lacking. Here we explore the possibility that interstellar bubbles seen by the Spitzer- and Herschel space telescopes, blown by stars with log(L/L_sun) < 5.2, form and expand due to the thermal pressure accompanying ionization of the surrounding gas. We show that density gradients in the natal cloud or a puncture in the swept up shell lead to an ionized gas flow through the bubble into the general interstellar medium, which is traced by a dust wave near the star, demonstrating the importance of radiation pressure during this phase. Dust waves provide a natural explanation for the presence of dust inside H II bubbles, offer a novel method to study dust in H II regions and provide direct evidence that bubbles are relieving their pressure into the ISM through a champagne flow, acting as a probe of the radiative interaction of a massive star with its surroundings. We create a parameter space connecting the ambient density, the ionizing source luminosity, and the position of the dust wave, while using the well-studied H II bubbles RCW 120 and RCW 82 as benchmarks of our model. Finally, we briefly examine the implications of our study for the environments of super star clusters formed in UltraLuminous InfraRed Galaxies (ULIRGs), merging galaxies and the early Universe, which occur in very luminous and dense environments and where radiation pressure is expected to dominate the dynamical evolution.
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