Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement
Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement
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DOI：
10.3847/1538-4357/ac09e8
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发表时间：
2020-08
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通讯作者：
D. Anglés-Alcázar;E. Quataert;P. Hopkins;R. Somerville;C. Hayward;C. Faucher-Giguère;G. Bryan;D. Keres̆;L. Hernquist;J. Stone
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作者：
D. Anglés-Alcázar;E. Quataert;P. Hopkins;R. Somerville;C. Hayward;C. Faucher-Giguère;G. Bryan;D. Keres̆;L. Hernquist;J. Stone
我们提出了宇宙学流体动力学模拟的类星体质量晕（M晕<$1012.5 M在z = 2），第一次解决气体运输到内部0.1 pc周围的中央大质量黑洞。我们模拟一个多相的星际介质，包括恒星反馈超新星，恒星风和辐射，和超拉格朗日细化技术，增加动态接近黑洞的分辨率。我们不包括黑洞反馈。我们发现，亚pc流入速率（1）在核气体密度峰值（z = 2）的时期，在稳定状态下可以达到大约1.6兆兆年，足以为发光类星体提供动力，（2）在前类星体阶段是高度时变的，在百万年时间尺度上跨越0.001-10兆年，（3）由于形成了一个热的中心空腔，它只限于短的（1.2亿年）活跃期（0.01-0.1百万年），然后在较低的核气体密度和较晚的时间（z = 1）有较长的不活跃期。流入的气体主要是冷的，旋转支撑在湍流和热压中占主导地位，星星的形成可以消耗与1 pc-10 kpc流入气体一样多的气体。来自多尺度恒星非轴对称的引力矩主导了气体自扭和压力梯度的角动量输运，吸积弱依赖于黑洞质量。亚pc流入速率与核（但与全球）星星的形成相关，并且可以超过爱丁顿速率×10。黑洞可以从银河系中心移动100万秒。吸积气体形成pc尺度的、旋转支撑的、模糊的结构，这些结构经常与星系尺度的盘不对齐。这些模拟为研究黑洞-星系的共同演化开辟了一条新的途径。
We present cosmological hydrodynamic simulations of a quasar-mass halo (M halo ≈ 1012.5 M ⊙ at z = 2) that for the first time resolve gas transport down to the inner 0.1 pc surrounding the central massive black hole. We model a multiphase interstellar medium including stellar feedback by supernovae, stellar winds, and radiation, and a hyper-Lagrangian refinement technique increasing the resolution dynamically approaching the black hole. We do not include black hole feedback. We show that the subpc inflow rate (1) can reach ∼6 M ⊙ yr−1 roughly in steady state during the epoch of peak nuclear gas density (z ∼ 2), sufficient to power a luminous quasar, (2) is highly time variable in the pre-quasar phase, spanning 0.001–10 M ⊙ yr−1 on Myr timescales, and (3) is limited to short (∼2 Myr) active phases (0.01–0.1 M ⊙ yr−1) followed by longer periods of inactivity at lower nuclear gas density and late times (z ∼ 1), owing to the formation of a hot central cavity. Inflowing gas is primarily cool, rotational support dominates over turbulence and thermal pressure, and star formation can consume as much gas as provided by inflows across 1 pc–10 kpc. Gravitational torques from multiscale stellar non-axisymmetries dominate angular momentum transport over gas self-torquing and pressure gradients, with accretion weakly dependent on black hole mass. Subpc inflow rates correlate with nuclear (but decouple from global) star formation and can exceed the Eddington rate by ×10. The black hole can move ∼10 pc from the galaxy center on ∼0.1 Myr. Accreting gas forms pc-scale, rotationally supported, obscuring structures often misaligned with the galaxy-scale disk. These simulations open a new avenue to investigate black hole–galaxy coevolution.