论文标题
缎面项目I：银河系模拟中的动荡的多相ISM，并带有来自恒星群集的SNE反馈
The SATIN project I: Turbulent multi-phase ISM in Milky Way simulations with SNe feedback from stellar clusters
论文作者
论文摘要
我们介绍了缎面的恒星形成和超新星反馈模型（通过具有非平衡效应的ISM模拟AGN）项目，以模拟整个磁盘星系的恒星形成多相星际介质（ISM）的演变。成功的ISM反馈模型的这种星系范围内的实现自然涵盖了气体表面密度，剪切和径向运动的数量级。它是在9 pc的峰值分辨率的自适应网格改进代码公羊中实现的。新恒星由巨大恒星的单个SN延迟时间的恒星簇（水槽）颗粒表示。通过SN反馈，冷却和重力，银河系ISM形成了现实的三相结构。恒星形成速率自然遵循当地银河系气体表面密度的缩放关系。 sne驱动在温暖（300 k <$ t $ <10 $^4 $ k）气体中的额外湍流，并增加冷气的动能，从而从温暖的阶段冷却。离开银河ISM的大多数气体都是温暖而热的，质量负载因子为$ 3 \leη\ le 10 $。当热气离开系统时，温暖和冷气以银河喷泉流回到碟片上。
We introduce the star formation and Supernova (SN) feedback model of the SATIN (Simulating AGNs Through ISM with Non-Equilibrium Effects) project to simulate the evolution of the star forming multi-phase interstellar medium (ISM) of entire disk galaxies. This galaxy-wide implementation of a successful ISM feedback model naturally covers an order of magnitude in gas surface density, shear and radial motions. It is implemented in the adaptive mesh refinement code RAMSES at a peak resolution of 9 pc. New stars are represented by star cluster (sink) particles with individual SN delay times for massive stars. With SN feedback, cooling and gravity, the galactic ISM develops a realistic three-phase structure. The star formation rates naturally follow observed scaling relations for the local Milky Way gas surface density. SNe drive additional turbulence in the warm (300 K < $T$ < 10$^4$ K) gas and increase the kinetic energy of the cold gas, cooling out of the warm phase. The majority of the gas leaving the galactic ISM is warm and hot with mass loading factors of $3 \le η\le 10$. While the hot gas is leaving the system, the warm and cold gas falls back onto the disc in a galactic fountain flow.
