Radiative Stellar Feedback in Galaxy Formation: Methods and Physics
Radiative Stellar Feedback in Galaxy Formation: Methods and Physics
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星系形成中的辐射恒星反馈：方法和物理学
DOI：
10.1093/mnras/stz3129
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发表时间：
2020
影响因子：
4.8
通讯作者：
Butcher, Nathan
中科院分区：
文献类型：
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作者：
Hopkins, Philip F;Grudić, Michael Y;Wetzel, Andrew;Kereš, Dušan;Faucher-Giguère, Claude-André;Ma, Xiangcheng;Murray, Norman;Butcher, Nathan
来自恒星的辐射反馈（RFB）在星系中起着关键作用，但仍然知之甚少。我们探索这一点，使用高分辨率，多频辐射流体动力学（RHD）模拟在现实环境中的反馈（FIRE）项目。我们通过银河系质量尺度研究超暗矮星，包括H+He光电离;光电，莱曼沃纳，康普顿和尘埃加热;和单次+多次散射辐射压力（RP）。我们比较了不同的数值算法：基于光线的LEBRON（光学薄时精确）和基于矩的M1（光学厚时精确）。星系尺度上最重要的RFB通道是光电离加热和单散射RP：在所有星系中，大多数电离/远紫外光度（寿命积分测辐射热的1/2）被吸收。在矮星中，最重要的作用是来自抑制吸积的紫外背景的光电离加热。在MW质量星系中，超星系背景的影响可以忽略不计，但局部光电离和单次散射RP有助于调节星系星星形成效率和降低中心密度。如果没有一些RFB（或其他“快速”FB），解析的GMC转换成恒星的效率太高，使星系由高密度的束缚星星团主导。这使得星星的形成更加暴力和“突发”时，SNe爆炸在这些超集群的对象：因此，包括RFB“平滑”SFH。这些结论对RHD方法是稳健的，但M1产生更强的影响。像以前的FIRE模拟一样，红外多重散射是罕见的（在矮星中可以忽略不计，在大质量星系中的RP）：吸收主要发生在AV = 1的“正常”GMC中。
Radiative feedback (RFB) from stars plays a key role in galaxies, but remains poorly understood. We explore this using high-resolution, multifrequency radiation-hydrodynamics (RHD) simulations from the Feedback In Realistic Environments (FIRE) project. We study ultrafaint dwarf through Milky Way mass scales, including H+He photoionization; photoelectric, Lyman Werner, Compton, and dust heating; and single+multiple scattering radiation pressure (RP). We compare distinct numerical algorithms: ray-based LEBRON (exact when optically thin) and moments-based M1 (exact when optically thick). The most important RFB channels on galaxy scales are photoionization heating and single-scattering RP: in all galaxies, most ionizing/far-UV luminosity (∼1/2 of lifetime-integrated bolometric) is absorbed. In dwarfs, the most important effect is photoionization heating from the UV background suppressing accretion. In MW-mass galaxies, metagalactic backgrounds have negligible effects; but local photoionization and single-scattering RP contribute to regulating the galactic star formation efficiency and lowering central densities. Without some RFB (or other ‘rapid’ FB), resolved GMCs convert too-efficiently into stars, making galaxies dominated by hyperdense, bound star clusters. This makes star formation more violent and ‘bursty’ when SNe explode in these hyperclustered objects: thus, including RFB ‘smoothes’ SFHs. These conclusions are robust to RHD methods, but M1 produces somewhat stronger effects. Like in previous FIRE simulations, IR multiple-scattering is rare (negligible in dwarfs,of RP in massive galaxies): absorption occurs primarily in ‘normal’ GMCs withAV∼ 1.