发表机构
Max-Planck-Institut für Astronomie; Max-Planck-Institut für Astrophysik; Universitätssternwarte München, LMU（马克斯·普朗克天文学研究所; 马克斯·普朗克天体物理研究所; 慕尼黑大学天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
针对原行星盘热力学模拟，提出PLUTO代码中一种自洽的辐射流体动力学方案，涵盖气体、辐射和多物种尘埃的能量交换，可准确再现观测特征，并适用于盘研究中的关键问题。
AI 中文摘要
原行星盘的热力学由气体、尘埃和辐射之间的复杂相互作用所控制，对其在大尺度和小尺度上的形态和动力学产生强烈影响。历史上，流体动力学模拟通常采用近似处理热力学的方法，例如局部等温假设、参数化的β冷却，以及假设气体与尘埃热平衡的辐射流体动力学。然而，一种更全面且自洽的方法能够更准确地再现观测中发现的丰富特征，而现代观测已达到前所未有的光谱、角度和垂直分辨率。基于这一动机，我们为PLUTO代码设计了一种辐射流体动力学方案，该方案通过吸收、发射和碰撞实现气体、辐射及多种尘埃物种之间的能量交换。尘埃-气体动力学通过将每种尘埃物种视为无压力、可扩散的流体来处理，确保我们的方案能够表示由颗粒沉降和捕获引起的盘照明变化。我们在多个测试问题中展示了该方案的有效性，并最后讨论了其与原行星盘研究中未解决问题相关性。
英文摘要
The thermodynamics of protoplanetary disks, governed by a complex interplay between gas, dust, and radiation, exerts a strong influence on their morphology and dynamics at both large and small scales. Historically, hydrodynamical simulations have treated thermodynamics with approximate prescriptions, such as local isothermality, parametrized $β$-cooling, and radiation hydrodynamics with gas-dust thermal equilibrium. However, a more comprehensive and self-consistent approach would more accurately reproduce the wealth of features found in observations, which in modern times have reached unprecedented spectral, angular, and vertical resolution. With this motivation, we have devised a radiation-hydrodynamics scheme for the PLUTO code with energy exchange (via absorption, emission, and collisions) for gas, radiation, and multiple species of dust. Dust-gas dynamics are handled by treating each dust species as a pressureless, diffusive fluid, ensuring that our scheme can represent changes in disk illumination caused by grain settling and trapping. We demonstrate the effectiveness of our scheme in several test problems, and conclude by discussing its relevance to open questions in protoplanetary disk studies.
Comments18 pages (+7 pages appendix), 13 figures. Accepted to Astronomy and Astrophysics; further comments and questions welcome
