How to model supernovae in simulations of star and galaxy formation
How to model supernovae in simulations of star and galaxy formation
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DOI：
10.1093/mnras/sty674
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发表时间：
2017-07
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. Hayward;K. El-Badry
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文献类型：
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作者：
P. Hopkins;A. Wetzel;D. Keres̆;C. Faucher-Giguère;E. Quataert;M. Boylan-Kolchin;N. Murray;C. Hayward;K. El-Badry
作者：Hopkins， PF；吉姆,一个;凯瑞斯语,D;faucher - giguere CA;Quataert E;Boylan-Kolchin, M;穆雷,N;海沃德,CC;摘要：©2018作者。牛津大学出版社代表皇家天文学会出版。在现实环境反馈（FIRE）项目中，我们研究了超新星（SNe）和恒星质量损失在星系模拟中的机械反馈的实现。我们提出了耦合力学反馈的FIRE-2算法，该算法可以应用于任何流体力学方法（如固定网格、移动网格和无网格方法），以及黑洞和恒星反馈。该算法确保了质量、能量和动量的明显守恒，并避免在弹射物上留下“首选方向”的印记。我们表明，以一种自一致的方式结合机械喷射的动量和热能是至关重要的，当它们不被解决时，考虑到SNe冷却半径。通过对单个SN爆炸的理想化模拟，我们证明了FIRE-2算法在不受分辨率影响的情况下，可以再现能量和动量的收敛解。相比之下，文献中常见的“全热”（能量堆积）或“全动能”（粒子踢动）方案强烈依赖于分辨率：当应用于质量分辨率≥100M⊙时，它们与收敛解相差数量级。在星系形成模拟中，这种差异会导致星系属性的数量级差异，除非这些模型以分辨率相关的方式进行调整。我们表明，所有单独的时间分辨SNe模型都以足够高的分辨率（1 100M⊙）收敛到FIRE-2解决方案。然而，在理想的单sn模拟和宇宙学星系形成模拟中，FIRE-2算法在不重新调整参数的情况下比其他子网格模型收敛得快得多。
Author(s): Hopkins, PF; Wetzel, A; Keres, D; Faucher-Giguere, CA; Quataert, E; Boylan-Kolchin, M; Murray, N; Hayward, CC; El-Badry, K | Abstract: © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. We study the implementation of mechanical feedback from supernovae (SNe) and stellar mass loss in galaxy simulations, within the Feedback In Realistic Environments (FIRE) project. We present the FIRE-2 algorithm for coupling mechanical feedback, which can be applied to any hydrodynamics method (e.g. fixed-grid, moving-mesh, and mesh-less methods), and black hole as well as stellar feedback. This algorithm ensures manifest conservation of mass, energy, and momentum, and avoids imprinting 'preferred directions' on the ejecta. We show that it is critical to incorporate both momentum and thermal energy of mechanical ejecta in a self-consistent manner, accounting for SNe cooling radii when they are not resolved. Using idealized simulations of single SN explosions, we show that the FIRE-2 algorithm, independent of resolution, reproduces converged solutions in both energy and momentum. In contrast, common 'fully thermal' (energy-dump) or 'fully kinetic' (particle-kicking) schemes in the literature depend strongly on resolution: when applied at mass resolution ≳100M⊙, they diverge by orders of magnitude from the converged solution. In galaxy-formation simulations, this divergence leads to orders-of-magnitude differences in galaxy properties, unless those models are adjusted in a resolution-dependent way. We show that all models that individually time-resolve SNe converge to the FIRE-2 solution at sufficiently high resolution (l 100M⊙). However, in both idealized single-SN simulations and cosmological galaxy-formation simulations, the FIRE-2 algorithm converges much faster than other sub-grid models without re-tuning parameters.