发表机构
Università degli Studi di Milano; Max-Planck-Institut für Astronomie (MPIA); Università di Bologna; INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（米兰大学; 马克斯·普朗克天文学研究所; 博洛尼亚大学; 意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究提出原行星盘外边缘的辐射转移与尘埃演化耦合效应可自诱导形成边缘环，为第一代环的形成提供了无需行星参与的合理解释。
AI 中文摘要
ALMA的高角分辨率观测揭示原行星盘中普遍存在子结构，轴对称尘埃环是最常见的形态。一些观测到的原行星盘（包括年轻原行星盘）的轮廓整体光滑，在连续谱盘的外边缘附近存在局部的凹陷或凸起，表现为边缘环。尽管嵌入的行星可能对这些结构有贡献，但其物理起源仍不清楚。我们研究了这些边缘环完全源于原行星盘外边缘的辐射转移效应的可能性：盘外边缘陡峭的表面密度尘埃梯度使恒星辐射更有效地穿透到盘外，产生以“先凹陷后凸起”为特征的非单调温度分布。我们测试这种非单调温度结构能否生成并维持局部连续谱增强，通过在蒙特卡洛辐射转移代码RADMC-3D和尘埃演化代码DustPy之间迭代，耦合辐射转移与尘埃演化，该框架自洽地追踪温度、 grain生长和尘埃动力学的耦合演化。盘边缘的热力学反馈可自然生成并维持类似观测到的极年轻原行星盘中边缘环的局部尘埃增强，无需引入行星或额外动力学扰动，该机制为第一代环的形成提供了合理的解释。我们的结果强调，在模拟原行星盘时，耦合热力学与尘埃演化至关重要，表明热力学反馈可能在塑造盘子结构中发挥作用。
英文摘要
Observations with a high angular resolution by ALMA have revealed that substructures are ubiquitous in protoplanetary disks. Axisymmetric dust rings are the most common morphology. The profiles of some observed disks, including young disks, are smooth overall, with a localized dip or bump near the outer edge of the continuum disk that manifests as an edge ring. While embedded planets might contribute to these structures, their physical origin remains unclear. We investigated the possibility that these edge rings arise purely from radiative transfer effects at the outer edge of a protoplanetary disk. A steep surface density dust gradient at the outer edge of the disk allows stellar irradiation to penetrate more efficiently beyond the disk edge, producing a non-monotonic temperature profile characterized by a dip that is followed by a bump. We tested whether this non-monotonic temperature structure can generate and maintain a localized continuum enhancement. We coupled radiative transfer and dust evolution by iterating between the Monte Carlo radiative transfer code RADMC-3D and the dust evolution code DustPy. This framework self-consistently follows the coupled evolution of temperature, grain growth, and dust dynamics. Thermodynamic feedback at the disk edge can naturally generate and maintain localized dust enhancements resembling the edge rings that are observed in some extremely young disks. Without invoking planets or additional dynamical perturbations, this mechanism offers a plausible explanation for the first-generation ring formation. Our results highlight the importance of coupling thermodynamics and dust evolution when modeling protoplanetary disks, suggesting that thermodynamic feedback probably plays a role in shaping disk substructures.
Comments12 pages, 12 figures, accepted in A&A
DOI：10.1051/0004-6361/202661190
