GMC evolution in a barred spiral galaxy with star formation and thermal feedback
GMC evolution in a barred spiral galaxy with star formation and thermal feedback
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棒旋星系中的 GMC 演化与恒星形成和热反馈
DOI：
10.1093/mnras/stw1461
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发表时间：
2016
影响因子：
4.8
通讯作者：
Christine M.
中科院分区：
文献类型：
--
作者：
Fujimoto;Yusuke; Bryan;Greg L.; Tasker;Elizabeth J.; Habe;Asao; Simpson;Christine M.
我们探讨了m83型棒旋星系中恒星形成和热恒星反馈对巨分子云形成的影响。我们比较了三个具有不同恒星形成/反馈模型的高分辨率模拟（1.5 pc单元大小）：一个没有恒星形成，一个有恒星形成但没有反馈，一个有恒星形成和热能注入。我们分析了由此产生的云的数量，发现我们可以识别出在我们之前的工作中（不包括恒星形成或反馈）发现的相同数量的大质量、生机云和瞬态、低表面密度云。恒星的形成和反馈可以影响我们识别的云的混合。特别是，恒星的形成本身只是将稠密的云气体转化为恒星，而云种群只有很小的变化，主要是导致瞬变种群的轻微减少。然而，反馈有更强的影响：虽然它通常不足以完全摧毁云，但它确实从云中喷射出气体，增加云间区域的气体密度。这减少了大量云的数量，但大大增加了瞬态云的数量。我们还发现，反馈倾向于驱动大质量云的径向净流入，导致棒状区域恒星形成率的增加。我们研究了一些可能的原因，并得出结论，云间密度增强的阻力可能是负责任的。
We explore the impact of star formation and thermal stellar feedback on the giant molecular cloud population forming in a M83-type barred spiral galaxy. We compare three high-resolution simulations (1.5 pc cell size) with different star formation/feedback models: one with no star formation, one with star formation but no feedback, and one with star formation and thermal energy injection. We analyse the resulting population of clouds, finding that we can identify the same population of massive, virialized clouds and transient, low-surface density clouds found in our previous work (that did not include star formation or feedback). Star formation and feedback can affect the mix of clouds we identify. In particular, star formation alone simply converts dense cloud gas into stars with only a small change to the cloud populations, principally resulting in a slight decrease in the transient population. Feedback, however, has a stronger impact: while it is not generally sufficient to entirely destroy the clouds, it does eject gas out of them, increasing the gas density in the intercloud region. This decreases the number of massive clouds, but substantially increases the transient cloud population. We also find that feedback tends to drive a net radial inflow of massive clouds, leading to an increase in the star formation rate in the bar region. We examine a number of possible reasons for this and conclude that it is possible that the drag force from the enhanced intercloud density could be responsible.