Stellar winds and photoionization in a spiral arm
Stellar winds and photoionization in a spiral arm
复制标题
旋臂中的恒星风和光电离
DOI：
10.1093/mnras/stac025
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发表时间：
2022
影响因子：
4.8
通讯作者：
Ali A
中科院分区：
文献类型：
--
作者：
Ali A
不同的恒星反馈机制在巨大分子云中的作用还没有得到很好的理解。这对于在银河系旋臂中发现的具有许多相互作用的云的区域尤其如此。在本文中，基于Bending等人以前的工作，we extract提取asection部分of a spiral旋arm臂from a galaxy星系simulation模拟.我们使用平滑粒子流体动力学重新模拟该地区在更高的分辨率（1 M的粒子）。我们提出了一种方法，动量驱动的恒星风从主序星，包括光电离，自引力，银河系的潜力，和星际介质加热/冷却。我们还包括集群下沉粒子的吸积半径为0.78 pc跟踪星星/集群的形成。反馈方法与以前的单个云尺度模型（例如Dale等人）一样稳健。我们发现，光致电离主导的螺旋臂部分的中断，与恒星风只产生小腔（最多1.30秒差距）。恒星风不影响所产生的云的统计数据或综合的星星形成率/效率，不像电离，电离产生更多的恒星，和更多的云更高的密度和更高的速度色散相比，没有反馈的控制运行。风确实会影响星汇的性质，使星星的形成分布在更多的低质量星汇（102 M）上，而产生更少的高质量星汇（103 M）。总的来说，与光电离相比，恒星风充其量只是次要的作用，在许多方面，它们的影响可以忽略不计。
The role of different stellar feedback mechanisms in giant molecular clouds is not well understood. This is especially true for regions with many interacting clouds as would be found in a galactic spiral arm. In this paper, building on previous work by Bending et al., we extract asection of a spiral arm from a galaxy simulation. We use smoothed particle hydrodynamics to re-simulate the region at higher resolution (1 M⊙per particle). We present a method for momentum-driven stellar winds from main-sequence massive stars, and include this with photoionization, self-gravity, a galactic potential, and interstellar medium heating/cooling. We also include cluster-sink particles with accretion radii of 0.78 pc to track star/cluster formation. The feedback methods are as robust as previous models on individual cloud scales (e.g. Dale et al.). We find that photoionization dominates the disruption of the spiral arm section, with stellar winds only producing small cavities (at most ∼30 pc). Stellar winds do not affect the resulting cloud statistics or the integrated star formation rate/efficiency, unlike ionization, which produces more stars, and more clouds of higher density and higher velocity dispersion compared to the control run without feedback. Winds do affect the sink properties, distributing star formation over more low-mass sinks (∼102M⊙) and producing fewer high-mass sinks (∼103M⊙). Overall, stellar winds play at best a secondary role compared to photoionization, and on many measures, they have a negligible impact.