Bo Zhao, Ralph E. Pudritz, Rachel Pillsworth, Hector Robinson and James Wadsley
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引用次数: 0
摘要
现在有大量的观测证据表明,恒星形成是一个高度动态的过程,它将星系尺度的千帕斯卡细丝和超级气泡到 100 pc 尺度的巨分子云(GMC)和星团(1 pc)的细丝层次结构和超新星反馈联系在一起。在这里,我们介绍银河系多尺度 MHD 模拟,在一个磁化的、类似银河系的、经历超新星驱动反馈过程的星系中,跟踪从银河系尺度到亚秒尺度的结构形成过程。为此,我们采用了一种新颖的放大技术,跟踪典型的 3 kpc 子区域的演变,而不切断周围的星系环境,从而使我们能够在单个放大区域达到 0.28 pc 的分辨率。我们发现了广泛的形态和层次结构,包括超泡泡、湍流、千波长原子气体丝(通常与超泡泡压缩有关)、小尺度丝状 GMC 和其中的星团区域。气体的吸积和压缩最终会驱使丝状气体超过临界线质量,从而导致引力不稳定性,产生 GMC 和星团。在较安静的区域,银河剪切会在 100 pc 尺度的扁平旋转盘状结构中产生丝状 GMC。令人震惊的是,我们的模拟证明了螺旋磁场的形成与这些盘状结构的形成有关。
Filamentary Hierarchies and Superbubbles: Galactic Multiscale Magnetohydrodynamic Simulations of Giant Molecular Cloud to Star Cluster Formation
There is now abundant observational evidence that star formation is a highly dynamical process that connects filament hierarchies and supernova feedback from galaxy-scale kiloparsec filaments and superbubbles to giant molecular clouds (GMCs) on 100 pc scales and star clusters (1 pc). Here we present galactic multiscale MHD simulations that track the formation of structure from galactic down to subparsec scales in a magnetized, Milky Way–like galaxy undergoing supernova-driven feedback processes. We do this by adopting a novel zoom-in technique that follows the evolution of typical 3 kpc subregions without cutting out the surrounding galactic environment, allowing us to reach 0.28 pc resolution in the individual zoom-in regions. We find a wide range of morphologies and hierarchical structures, including superbubbles, turbulence, and kiloparsec atomic gas filaments hosting multiple GMC condensations that are often associated with superbubble compression, down to smaller-scale filamentary GMCs and star cluster regions within them. Gas accretion and compression ultimately drive filaments over a critical, scale-dependent line mass leading to gravitational instabilities that produce GMCs and clusters. In quieter regions, galactic shear can produce filamentary GMCs within flattened, rotating disklike structures on 100 pc scales. Strikingly, our simulations demonstrate the formation of helical magnetic fields associated with the formation of these disklike structures.