arXiv 2510.024322025-10astro-ph.GAastro-ph.HE

超新星反馈影响与粗化模拟分辨率之间的纠缠

The Entangling of Supernova Feedback Impacts with Coarsening Simulation Resolution

University of California, Riverside（加州大学河滨分校）；University of Hawaii（夏威夷大学）；Tsinghua University（清华大学）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；University of Bologna（博洛尼亚大学）；INAF（意大利国家天体物理研究所）；Massachusetts Institute of Technology（麻省理工学院）；University of Virginia（弗吉尼亚大学）；Universität Heidelberg（海德堡大学）；York University（约克大学）；The University of Texas at Dallas（德克萨斯大学达拉斯分校）

Eric Zhang, Laura V. Sales, Thales A. Gutcke, Yunwei Deng, Hui Li, Rüdiger Pakmor, Federico Marinacci, Volker Springel, Mark Vogelsberger, Paul Torrey, Boyuan L… 展开作者

Eric Zhang, Laura V. Sales, Thales A. Gutcke, Yunwei Deng, Hui Li, Rüdiger Pakmor, Federico Marinacci, Volker Springel, Mark Vogelsberger, Paul Torrey, Boyuan Liu, Rahul Kannan, Aaron Smith, Greg L. Bryan

备注：: Published in the Open Journal of Astrophysics. 11 pages (excluding bibliography), 7 figures; comments welcome

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AI总结：

通过极高分辨率模拟孤立矮星系，发现超新星反馈在扩散区域驱动大尺度外流，在致密区域局部抑制恒星形成，但粗分辨率会混淆这些通道，导致密度估计错误和反馈效应误判。

摘要：

通常认为星系中的超新星（SN）反馈负责调节恒星形成（SF）并产生气体外流。然而，对模拟中星际介质（ISM）小尺度效应的详细观察表明，这些过程通过不同且分离的通道进行。我们在两个具有极高（$m_{\rm gas}$ $\sim \msun$）数值分辨率的孤立矮星系独立模拟中证明了这一发现，即{\small LYRA}和{\small RIGEL}。聚焦于SN周围的直接环境，我们的发现表明，给定SN对星系的宏观效应最好由其局部密度预测。外流由扩散区域中的SN驱动，在大尺度（$\sim$ kpc）上膨胀至其冷却半径，而致密SF区域则以局部（$\sim$ pc）方式被破坏。然而，这些分离的反馈通道只有在能够追踪质量尺度$\lesssim 10^2 \\,\msun$的极高分辨率下才能区分。当在较粗尺度上平均时，ISM密度被严重错误估计，不同SF和SN影响区域之间的变化被严重抹平。因此，仅从粗分辨率信息无法自洽地确定（1）SN倾向于贡献于外流还是直接抑制SF，以及（2）给定区域中的SF速率。特别是，粗分辨率（亚网格）模型中常用的参数，如SN冷却半径和SF密度阈值，可能需要由高分辨率研究提供的更详细处理。

英文摘要：

It is often understood that supernova (SN) feedback in galaxies is responsible for regulating star formation (SF) and generating gaseous outflows. However, a detailed look at the small-scale effects of SNe on the interstellar medium (ISM) in simulations shows that the macroscopic processes of SF suppression and outflow generation proceed in distinct channels. We demonstrate this finding in two independent simulations of isolated dwarf galaxies with very high (m_gas ~ Msun) numerical resolution, LYRA and RIGEL. Our findings suggest that the macroscopic effect of a given SN on the galaxy is best predicted by its local density. Outflows are primarily linked to SNe in diffuse regions expanding to their cooling radii on large (~kpc) scales, while dense SF regions are disrupted in a localized (~pc) manner. However, these separate feedback channels are only distinguishable at very high resolutions capable of following mass scales \lesssim 10^2 \msun. When averaging on coarser scales, ISM densities are greatly mis-estimated, and variations between different SF and SNe-affected regions are severely washed out. It therefore cannot be __self-consistently__ determined, from coarse-resolution information __alone__, (1) whether a SN tends to contribute to outflows or direct SF suppression, and (2) the rate of SF in a given region. In particular, commonly used parameters in coarse-resolution (subgrid) models, such as the SN cooling radius and SF density threshold, may require more detailed treatments informed by high-resolution studies.

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