星系中延迟的金属再循环：碰撞超壳层模拟中冷气体富集的无效性
Delayed metal recycling in galaxies: the inefficiency of cold gas enrichment in colliding supershell simulations
摘要：
数值研究了年轻OB星协向星际介质中喷射金属粒子的命运。特别是，我们研究了冷气相的富集，这是形成分子云的材料。根据以前的工作，在一个弥漫的ISM中的两个超壳层的膨胀和碰撞进行了模拟，在这种情况下，还引入了一个平流量，它代表了年轻恒星排出的金属。我们采用最简单的方法，不区分来自恒星风和来自超新星的金属。尽管ISM的热扩散阶段从恒星接收了大量的金属，但冷阶段被有效地屏蔽了，金属富集很少。因此，冷ISM的显著富集将至少延迟该热相的冷却时间。云的金属丰度与OB协会或方向的距离没有变化，这意味着壳碰撞并没有提高冷团块的金属丰度。我们的结论是，由壳层碰撞引发的分子结构形成的恒星一代不能显着富集。
英文摘要：
The fate of metals ejected by young OB associations into the Interstellar Medium (ISM) is investigated numerically. In particular, we study the enrichment of the cold gas phase, which is the material that forms molecular clouds. Following previous work, the expansion and collision of two supershells in a diffuse ISM is simulated, in this case also introducing an advected quantity which represents the metals expelled by the young stars. We adopt the simplest possible approach, not differentiating between metals coming from stellar winds and those coming from supernovae. Even though the hot, diffuse phase of the ISM receives a significant amount of metals from the stars, the cold phase is efficiently shielded, with very little metal enrichment. Significant enrichment of the cold ISM will therefore be delayed by at least the cooling time of this hot phase. No variations in cloud metallicity with distance from the OB association or with direction are found, which means that the shell collision does little to enhance the metallicity of the cold clumps. We conclude that the stellar generation that forms out of molecular structures, triggered by shell collisions cannot be significantly enriched.
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