在火中锻造III：从STARFORGE中获得的星系吸积盘中的恒星质量函数
FORGE'd in FIRE III: The IMF in Quasar Accretion Disks from STARFORGE
AI总结：
研究通过STARFORGE模拟揭示了类星体吸积盘中恒星形成和IMF的形成机制，强调磁性场、辐射及反馈的重要性，并指出未解析的动力学对IMF形状的敏感影响。
摘要：
最近，我们展示了从宇宙辐射-磁流体动力学-热化学星系-恒星形成模拟中自洽地形成强磁化类星体吸积盘（QADs）。这些模拟包括之前已显示在典型星际介质条件下能产生合理恒星质量函数（IMF）的完整STARFORGE物理过程。在此，我们研究了QADs中的恒星形成和恒星IMF，研究尺度从100个天文单位到10个秒差距。我们表明，包括磁性场、辐射和（原）恒星反馈在内的物理过程是至关重要的。更靠近黑洞，恒星形成被抑制，但形成的（罕见）恒星表现出顶部偏重的IMF。恒星只能在特殊位置（例如磁场转换）形成于QAD的外围。原恒星快速吸积其胎盘核心，但随后动态解耦并与气体分离，停止吸积的时间尺度约为100年。其喷流控制初始核心吸积，但喷流被扫入更大的尺度QAD流中，没有显著的动态影响。强烈的潮汐环境强烈抑制了核心的多重性。IMF的形状对原恒星盘（PSD）的未解析动力学高度敏感，因为全球的动力学时间可以变得极其短（<<年）且潮汐场极其强大，因此PSD是否能有效传输角动量或在<<10天文单位尺度上发生灾难性碎片化，需要新的PSD模拟来正确解决。大多数解析IMF模型和类比于PSD中的行星形成均无法定性地解释模拟IMF，尽管我们讨论了其中几种可行的模型。
英文摘要：
Recently, we demonstrated self-consistent formation of strongly-magnetized quasar accretion disks (QADs) from cosmological radiation-magnetohydrodynamic-thermochemical galaxy-star formation simulations, including the full STARFORGE physics shown previously to produce a reasonable IMF under typical ISM conditions. Here we study star formation and the stellar IMF in QADs, on scales from 100 au to 10 pc from the SMBH. We show it is critical to include physics often previously neglected, including magnetic fields, radiation, and (proto)stellar feedback. Closer to the SMBH, star formation is suppressed, but the (rare) stars that do form exhibit top-heavy IMFs. Stars can form only in special locations (e.g. magnetic field switches) in the outer QAD. Protostars accrete their natal cores rapidly but then dynamically decouple from the gas and wander, ceasing accretion on timescales ~100 yr. Their jets control initial core accretion, but the ejecta are swept up into the larger-scale QAD flow without much dynamical effect. The strong tidal environment strongly suppresses common-core multiplicity. The IMF shape depends sensitively on un-resolved dynamics of protostellar disks (PSDs), as the global dynamical times can become incredibly short ($\ll$ yr) and tidal fields are incredibly strong, so whether PSDs can efficiently transport angular momentum or fragment catastrophically at $\lesssim 10$ au scales requires novel PSD simulations to properly address. Most analytic IMF models and analogies with planet formation in PSDs fail qualitatively to explain the simulation IMFs, though we discuss a couple of viable models.
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