FIRE-2模拟：星系形成中的物理学与数值学
FIRE-2 Simulations: Physics versus Numerics in Galaxy Formation
摘要：
真实环境中的反馈（FIRE）项目探索宇宙学星系形成模拟中的反馈。为了保持一致性，以前的FIRE模拟使用了相同的源代码（FIRE-1）。出于更精确的数值的发展-包括流体动力学求解器，引力软化，超新星耦合算法-和探索新的物理（如磁场），我们介绍了消防-2，更新的数值实现消防物理的GIZMO代码。我们运行了一套模拟并与FIRE-1进行了比较：总体而言，FIRE-2的改进不会定性地改变星系尺度的性质。我们追求一个广泛的研究数字与物理。恒星形成算法的细节，冷却物理学和化学的影响很弱，只要我们包括金属线冷却和恒星形成发生在高于平均密度。我们提出了新的高分辨率星系模拟的分辨率标准。大多数星系尺度的性质对我们测试的数值是鲁棒的，只要：（1）Toomre质量被解析;（2）反馈耦合确保守恒;（3）单个超新星是时间解析的。恒星质量和轮廓是最强大的分辨率，其次是金属丰度和形态，其次是风和环银河系介质（CGM）的属性。大质量（L*）星系的中心（~kpc）质量浓度对数值敏感（通过热晕中风的捕获/再循环）。多重反馈机制起着关键作用：超新星调节恒星质量/恒星风;恒星质量损失促进后期恒星形成;辐射反馈抑制矮星吸积和盘中瞬时恒星形成。我们提供了所有的初始条件和数值算法。
英文摘要：
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.
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