CALIMA：辐射-水动力学星系形成模拟中的实时尘埃和PAH演化
CALIMA: On-the-fly dust and PAH evolution for radiation-hydrodynamics galaxy formation simulations
AI总结：
CALIMA通过实时尘埃和PAH演化，改进辐射-水动力学模拟，以更准确地解释尘埃和PAH的观测数据及尘埃反馈在星系形成中的作用。
摘要：
尘埃颗粒和多环芳香烃（PAHs）积极地影响星际介质（ISM）的热力学、化学和辐射状态，但大多数ISM模型和星系模拟要么完全排除它们，要么采用简化的处理。我们提出了CALIMA，这是一个新的模块，用于RAMSES辐射-水动力学模拟中的尘埃和PAH形成与演化，旨在自洽地耦合尘埃物理到辐射转移和非平衡热化学，在多相ISM中。该模型采用双大小、双组成尘埃框架，具有对数正态粒径分布，明确地演进恒星尘埃注入、湍流导向的气体相吸附、破碎、凝聚、热和非热溅射以及冲击破坏，同时PAHs作为独立组件具有各自的发展。演化的尘埃群体和辐射场决定了局部、波长依赖的不透明度、光电加热效率、尘埃辅助重组、尘埃-气体碰撞加热/冷却以及氢分子在尘埃和PAHs上的形成。对热溅射和碰撞冷却的更新处理，包括有限的尘埃尺寸和现代离子-固体物理，降低了高温下的溅射速率，并扩展了尘埃显著冷却热气体的范围。单区ISM测试显示，尘埃和PAH演化修改了经典热相图和碳承载化学，而孤立盘星系模拟揭示了环境依赖的尘埃-金属比、小到大粒径比、PAH分数和星际辐射场强度的变化，驱动了红外发射、紫外透明度和氢分子形成中的非平凡结构。CALIMA提供了一个物理动机的框架，用于解释基于尘埃和PAH的观测数据，并评估尘埃介导的反馈在星系形成中的跨宇宙时间影响。
英文摘要：
Dust grains and polycyclic aromatic hydrocarbons (PAHs) actively contribute to the thermodynamics, chemistry, and radiative state of the interstellar medium (ISM), yet most ISM models and galaxy simulations either exclude them altogether or adopt simplified treatments. We present CALIMA, a new module for dust and PAH formation and evolution in radiation-hydrodynamics simulations for RAMSES, designed to self-consistently couple dust physics to radiative transfer and non-equilibrium thermochemistry in a multiphase ISM. The model employs a two-size, two-composition dust framework with log-normal grain populations, explicitly evolving stellar dust injection, turbulence-informed gas-phase accretion, shattering, coagulation, thermal and non-thermal sputtering, and shock destruction, while PAHs are separate components with their own evolution. The evolving dust populations and radiation field determine local, wavelength-dependent opacities, photoelectric heating efficiencies, grain-assisted recombination, dust-gas collisional heating/cooling, and H$_2$ formation on both grains and PAHs. Updated treatments of thermal sputtering and collisional cooling that include finite grain sizes and modern ion-solid physics reduce sputtering rates at high temperatures and extend the regime where dust significantly cools hot gas. One-zone ISM tests show that dust and PAH evolution modifies classical thermal phase diagrams and C-bearing chemistry, while isolated disc galaxy simulations reveal environment-dependent variations in dust-to-metal ratio, small-to-large grain ratio, PAH fraction, and interstellar radiation field intensity that drive non-trivial structure in infrared emission, UV transparency, and H$_2$ formation. CALIMA provides a physically motivated framework to interpret dust- and PAH-based observables and to assess dust-mediated feedback in galaxy formation across cosmic time.
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