The failure of stellar feedback, magnetic fields, conduction, and morphological quenching in maintaining red galaxies
The failure of stellar feedback, magnetic fields, conduction, and morphological quenching in maintaining red galaxies
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DOI：
10.1093/mnras/stz1494
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发表时间：
2018-09
影响因子：
4.8
通讯作者：
Kung-Yi Su;P. Hopkins;C. Hayward;Xiangcheng Ma;C. Faucher-Giguère;D. Kerevs;Matthew E. Orr;V. Robles
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文献类型：
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作者：
Kung-Yi Su;P. Hopkins;C. Hayward;Xiangcheng Ma;C. Faucher-Giguère;D. Kerevs;Matthew E. Orr;V. Robles
在从银河系质量穿过星系团的星系中，猝灭“维持”和相关的“冷却流动”问题是很重要的。我们用FIRE-2(在现实环境中的反馈)恒星反馈模型的非宇宙学高分辨率流体动力学模拟，在质量为∼$10^{12}--10^{14}，{rM}_我们特别关注没有AGN的物理存在，并表明文献中提出的各种“非AGN”解决机制，包括Ia型超新星、激波AGB风、其他形式的恒星反馈(例如宇宙射线)、磁场、Spitzer-Braginskii传导或“形态猝灭”不会停止或大幅减少冷却流动，也不会在这个质量范围内维持“猝灭”的星系。我们发现，恒星反馈(包括来自SNE的宇宙射线)改变了冷/暖气体的平衡和星系内冷却气体变成恒星的速度，但不改变重子净流入。如果说有什么不同的话，那就是流出的金属和稠密的气体促进了额外的冷却。不出所料，只有在质量最大的晕中，传导才是重要的，但即使在∼$10^{14}，流入也只减少了一个因子∼2(由于饱和效应和各向异性抑制)。改变星系的形态只会轻微改变它们的Toomre-Q参数，对冷却没有影响(正如预期的那样)，因此基本上不会对冷却流动或保持猝灭产生任何影响。这一切都支持这样一种观点，即额外的物理，例如活动星系核反馈，在大质量星系中肯定是重要的。
The quenching ‘maintenance’ and related ‘cooling flow’ problems are important in galaxies from Milky Way mass through clusters. We investigate this in haloes with masses ∼$10^{12}\!-\!10^{14}\, {\rm M}_{\odot }$, using non-cosmological high-resolution hydrodynamic simulations with the FIRE-2 (Feedback In Realistic Environments) stellar feedback model. We specifically focus on physics present without AGN, and show that various proposed ‘non-AGN’ solution mechanisms in the literature, including Type Ia supernovae, shocked AGB winds, other forms of stellar feedback (e.g. cosmic rays), magnetic fields, Spitzer–Braginskii conduction, or ‘morphological quenching’ do not halt or substantially reduce cooling flows nor maintain ‘quenched’ galaxies in this mass range. We show that stellar feedback (including cosmic rays from SNe) alters the balance of cold/warm gas and the rate at which the cooled gas within the galaxy turns into stars, but not the net baryonic inflow. If anything, outflowing metals and dense gas promote additional cooling. Conduction is important only in the most massive haloes, as expected, but even at ∼$10^{14}\, {\rm M}_{\odot }$ reduces inflow only by a factor ∼2 (owing to saturation effects and anisotropic suppression). Changing the morphology of the galaxies only slightly alters their Toomre-Q parameter, and has no effect on cooling (as expected), so has essentially no effect on cooling flows or maintaining quenching. This all supports the idea that additional physics, e.g. AGN feedback, must be important in massive galaxies.