丝状体层次结构与超星团II：超星团和银河动力学对丝状体形成和碎裂的影响
Filamentary Hierarchies and Superbubbles II: Impact of superbubbles and galactic dynamics on filament formation and fragmentation
AI总结：
本文研究了银河剪切、超新星和磁场对丝状体形成和碎裂的影响，发现丝状体稳定性与磁场密切相关，且外盘区域的丝状体更易被剪切耗散。
摘要：
在螺旋星系中，如剪切、超新星和磁场等大尺度现象都参与了丝状结构和其中的恒星形成的形成和后续演化。在本文中，我们分析了 Zhao 等人 2024 年模拟的类似银河系中的丝状体的性质和动态。利用丝状体和超星团结构分析代码，我们研究了银河剪切、超新星和超星团以及磁场对丝状体稳定性和碎裂作用的角色。我们发现局部剪切对丝状体稳定性影响很小，盘外半径的最大型可能更易被剪切耗散而非超新星。丝状体大致与磁场平行，磁场在丝状体稳定性中起重要作用。通过测量丝状体表面压力与其中心轴压力的比值 $χ_f=P_{surf}/P_{central}$，我们发现 $χ_f \le 1$ 的丝状体主要由自身重力主导，具有强烈的引力超临界倾向，而 $χ_f > 1$ 的则可能是短暂或正在形成中的。最后，我们研究了星际介质压力对丝状体动态和稳定性的作用，发现盘内和盘外区域的丝状体稳定性和伴随的恒星形成率有显著变化。
英文摘要：
Large scale phenomena in spiral galaxies such as shear, supernovae, and magnetic fields all contribute to the formation and subsequent evolution of filamentary structure and star formation within them. In this paper, we analyze the properties and dynamics of filaments in a simulated Milky Way-like galaxy from Zhao et al. 2024. Using filament and superbubble structure analysis codes, we investigate the roles of galactic shear, supernovae and superbubbles, and magnetic fields on the stability and fragmentation of filaments. We find that local shear has little effect on filament stability and the largest structures at outer radii of the disk may be more likely to be dissipated by shear than supernovae. Filaments are largely parallel to the magnetic field, which plays a significant role in filament stability. By measuring the ratio of surface pressure on a filament to that on its central spine, $χ_f=P_{surf}/P_{central}$, we find that filaments with $χ_f \le 1$ are dominated by their own self gravity and have a strong tendency to be gravitationally supercritical, whereas those with $χ_f > 1$ are either transitory or in the act of being formed. Finally, we investigate the role of ISM pressure on filament dynamics and stability as a function of galactic radius, finding considerable changes in filament stability and the accompanying star formation rates in the inner versus outer regions of the disk.
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