Snap，Crackle，Pop：盘状星系AMR模拟中的次网格超新星反馈
Snap, Crackle, Pop: sub-grid supernova feedback in AMR simulations of disk galaxies
摘要：
我们比较了超新星（SN）反馈的自适应网格加密（AMR）模拟孤立矮星系和L-星盘星系与20-40 pc分辨率的5个亚网格模型。这些模型是热转储，随机热，“机械”（注入能量或动量取决于分辨率），动力学和延迟冷却反馈。我们专注于每个模型抑制恒星形成和产生外流的能力。我们的最高分辨率运行勉强解决了反馈事件的绝热阶段，这对应于40个SN爆炸，前三个模型产生几乎相同的结果，可能表明动力学和延迟冷却反馈收敛到错误的结果。在较低的分辨率下，所有模型都不同，热转储反馈变得低效。热转储，随机和机械反馈产生多相流出的质量加载因子$β\ll 1$，这是远远低于观察到的。对于随机反馈的情况下，我们比较出版的SPH模拟，并发现更低的流出率。动力学反馈产生快速，热流出与$β\sim 1$，但只有当风是有效的流体动力学解耦的磁盘通过使用一个大的气泡半径。延迟冷却产生寒冷，密集和缓慢的风与$β> 1$，但大量的气体占据区域的温度-密度空间的冷却时间很短。我们的结论是，要么我们的分辨率太低，以保证物理动机的模型SN反馈，反馈机制比SNe是重要的，或其他方面的星系演化，如恒星形成，需要更好的治疗。
英文摘要：
We compare 5 sub-grid models for supernova (SN) feedback in adaptive mesh refinement (AMR) simulations of isolated dwarf and L-star disk galaxies with 20-40 pc resolution. The models are thermal dump, stochastic thermal, 'mechanical' (injecting energy or momentum depending on the resolution), kinetic, and delayed cooling feedback. We focus on the ability of each model to suppress star formation and generate outflows. Our highest-resolution runs marginally resolve the adiabatic phase of the feedback events, which correspond to 40 SN explosions, and the first three models yield nearly identical results, possibly indicating that kinetic and delayed cooling feedback converge to wrong results. At lower resolution all models differ, with thermal dump feedback becoming inefficient. Thermal dump, stochastic, and mechanical feedback generate multiphase outflows with mass loading factors $β\ll 1$, which is much lower than observed. For the case of stochastic feedback we compare to published SPH simulations, and find much lower outflow rates. Kinetic feedback yields fast, hot outflows with $β\sim 1$, but only if the wind is in effect hydrodynamically decoupled from the disk by using a large bubble radius. Delayed cooling generates cold, dense and slow winds with $β> 1$, but large amounts of gas occupy regions of temperature-density space with short cooling times. We conclude that either our resolution is too low to warrant physically motivated models for SN feedback, that feedback mechanisms other than SNe are important, or that other aspects of galaxy evolution, such as star formation, require better treatment.
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