FIRE-2 simulations: physics versus numerics in galaxy formation
FIRE-2 simulations: physics versus numerics in galaxy formation
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DOI：
10.1093/mnras/sty1690
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发表时间：
2017-02
影响因子：
4.8
通讯作者：
P. Hopkins;A. Wetzel;D. Keres̆;C. Faucher-Giguère;E. Quataert;M. Boylan-Kolchin;N. Murray;C. Hayw
中科院分区：
文献类型：
--
作者：
P. Hopkins;A. Wetzel;D. Keres̆;C. Faucher-Giguère;E. Quataert;M. Boylan-Kolchin;N. Murray;C. Hayw
现实环境中的反馈(FIRE)项目探索了宇宙星系形成模拟中的反馈。之前的火灾模拟使用了相同的源代码(“FIRE-1”)以保证一致性。受更精确数值计算的发展--包括流体动力解算器、引力软化和超新星耦合算法--以及对新物理(例如磁场)的探索的推动，我们为Gizmo代码引入了火灾物理的最新数值实现--FIRE-2。我们运行了一套模拟并与FIRE-1进行了比较：总体而言，FIRE-2的改进并不会定性地改变星系规模的属性。我们对数值和物理进行了广泛的研究。恒星形成算法、冷却物理和化学的细节有微弱的影响，如果我们包括金属线冷却和恒星形成发生在高于平均密度的情况下。我们为高分辨率星系模拟提出了新的分辨率标准。大多数星系尺度的性质对我们测试的数值是稳健的，前提是：(1)Toomre质量被分解；(2)反馈耦合确保守恒；(3)单个超新星是时间分辨的。恒星质量和轮廓的分辨率最强，其次是金属丰度和形态，其次是风和环星系介质(CGM)的性质。大质量(>；L*)星系的中心(∼kpc)质量浓度对数值(通过捕获/再循环热晕中的风)很敏感。多种反馈机制发挥着关键作用：超新星调节恒星质量/风；恒星质量损失推动后期恒星形成；辐射反馈抑制矮星的吸积和盘中瞬时恒星的形成。我们提供了所用的所有初始条件和数值算法。
The Feedback In Realistic Environments (FIRE) project explores feedback in cosmological galaxy formation simulations. Previous FIRE simulations used an identical source code (“FIRE-1”) for consistency. Motivated by the development of more accurate numerics – including hydrodynamic solvers, gravitational softening, and supernova coupling algorithms – and exploration of new physics (e.g. magnetic fields), we introduce “FIRE-2”, an updated numerical implementation of FIRE physics for the GIZMO code. We run a suite of simulations and compare against FIRE-1: overall, FIRE-2 improvements do not qualitatively change galaxy-scale properties. We pursue an extensive study of numerics versus physics. Details of the star-formation algorithm, cooling physics, and chemistry have weak effects, provided that we include metal-line cooling and star formation occurs at higher-than-mean densities. We present new resolution criteria for high-resolution galaxy simulations. Most galaxy-scale properties are robust to numerics we test, provided: (1) Toomre masses are resolved; (2) feedback coupling ensures conservation, and (3) individual supernovae are time-resolved. Stellar masses and profiles are most robust to resolution, followed by metal abundances and morphologies, followed by properties of winds and circum-galactic media (CGM). Central (∼kpc) mass concentrations in massive (>L*) galaxies are sensitive to numerics (via trapping/recycling of winds in hot halos). Multiple feedback mechanisms play key roles: supernovae regulate stellar masses/winds; stellar mass-loss fuels late star formation; radiative feedback suppresses accretion onto dwarfs and instantaneous star formation in disks. We provide all initial conditions and numerical algorithms used.