原行星盘的辐射热化学模型I。静液压盘结构及内轮辋
Radiation thermo-chemical models of protoplanetary disks I. Hydrostatic disk structure and inner rim
摘要：
本文介绍了一个新的磁盘代码，称为ProDiMo，计算原行星盘的热化学结构和解释气体发射谱线从UV到sub-mm。我们结合频率相关的二维尘埃连续辐射转移，动力学气相和UV光化学，冰的形成，和详细的非LTE加热和冷却平衡与流体静力盘结构的一致性计算。我们包括FeII和CO振转线加热/冷却相关的高密度气体接近恒星，并应用修改后的逃逸概率处理。模型的特点是各种物理，化学和辐射过程之间的高度一致性，其中相互反馈迭代求解。在应用于从0.5天文单位延伸到500天文单位的金牛座T盘时，这些模型的特点是有一个膨胀的内缘，并且表明致密、屏蔽和冷的中平面（z/r<0.1，Tg~Td）被一层热的（5000 K）和薄的（10^7 ~ 10^8 cm^-3）原子气体所包围，该原子气体径向延伸到大约10天文单位，垂直延伸到z/r~0.5。这一层主要由恒星紫外线加热（例如PAH加热），并通过FeII半禁戒和OI 630 nm光学线发射冷却。在这个“光环”中的尘埃颗粒将恒星光散射回圆盘上，从而影响光化学。较远的区域的特征在于较冷的扩口结构。在100 AU以上，即使在中平面，Tgas也从Tdust开始下降，并达到约Tg~ 2 Td的值。我们的模型表明，气体能量平衡是理解垂直盘结构的关键。用假设Tg=Td计算的模型显示出更平坦的盘结构。
英文摘要：
This paper introduces a new disk code, called ProDiMo, to calculate the thermo-chemical structure of protoplanetary disks and to interpret gas emission lines from UV to sub-mm. We combine frequency-dependent 2D dust continuum radiative transfer, kinetic gas-phase and UV photo-chemistry, ice formation, and detailed non-LTE heating & cooling balance with the consistent calculation of the hydrostatic disk structure. We include FeII and CO ro-vibrational line heating/cooling relevant for the high-density gas close to the star, and apply a modified escape probability treatment. The models are characterized by a high degree of consistency between the various physical, chemical and radiative processes, where the mutual feedbacks are solved iteratively. In application to a T Tauri disk extending from 0.5AU to 500AU, the models are featured by a puffed-up inner rim and show that the dense, shielded and cold midplane (z/r<0.1, Tg~Td) is surrounded by a layer of hot (5000K) and thin (10^7 to 10^8 cm^-3) atomic gas which extends radially to about 10AU, and vertically up to z/r~0.5. This layer is predominantly heated by the stellar UV (e.g. PAH-heating) and cools via FeII semi-forbidden and OI 630nm optical line emission. The dust grains in this "halo" scatter the star light back onto the disk which impacts the photo-chemistry. The more distant regions are characterized by a cooler flaring structure. Beyond 100AU, Tgas decouples from Tdust even in the midplane and reaches values of about Tg~2Td. Our models show that the gas energy balance is the key to understand the vertical disk structure. Models calculated with the assumption Tg=Td show a much flatter disk structure.
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