发表机构
Leiden Observatory, Leiden University; Mullard Space Science Laboratory, University College London; Max-Planck-Institut für Astronomie; Centre for Astrophysics and Supercomputing (CAS), Swinburne University of Technology; School of Physics and Astronomy, University of Leeds（莱顿天文台，莱顿大学; 穆拉德空间科学实验室，伦敦大学学院; 马克斯·普朗克天文学研究所; 天体物理学与超级计算中心，斯威本科技大学; 利兹大学物理与天文学学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过ALMA和VLA的多波段观测结合建模，发现DoAr25存在尘埃陷阱、CY Tau演化由径向漂移主导，揭示了尘埃演化过程对原行星盘形态和粒径分布的塑造作用。
AI 中文摘要
背景：原行星盘是行星的诞生地，理解其中尘埃的分布与演化对于追踪行星形成的早期阶段至关重要。目标：在DSHARP巡天之后，我们旨在限制CY Tau和DoAr25原行星盘中尘埃表面密度的径向分布以及最大发射粒径，并评估尘埃捕获和径向漂移在塑造盘内尘埃种群方面的相对重要性。方法：我们呈现CY Tau和DoAr25的多波段连续谱观测，包括ALMA在2.4毫米和1.25毫米的观测，以及VLA存档的8.8毫米数据。将这些观测与尘埃连续谱正向建模相结合，我们试图推断这两个系统的尘埃表面密度和最大发射粒径的径向轮廓。结果：对于DoAr25，结果显示在111天文单位处存在一个显著的尘埃环，并有大尺寸（厘米级）尘埃延伸至外盘的证据。相比之下，CY Tau表现出更致密、更平滑的结构，其尘埃表面密度和粒径均随半径单调递减。在20-40天文单位之间的径向轮廓中存在一个初步的肩部特征，可能指向一个微弱的亚结构，或许是一个较弱的尘埃陷阱。结论：DoAr25存在能够阻止向内漂移的尘埃陷阱的证据，而CY Tau则表现出与径向漂移主导演化一致的行为。这些结果共同凸显了尘埃演化过程如何塑造盘的形态和粒径分布，即便在低质量恒星区域亦是如此。
英文摘要
Context. Protoplanetary disks are the birthplaces of planets, and understanding the distribution and evolution of dust within them is essential for tracing the early stages of planet formation. Aims. Following the DSHARP survey, we aim to constrain the radial distribution of the dust surface density and the maximum emitting grain size in the disks of CY Tau and DoAr 25 and assess the relative importance of dust trapping and radial drift in shaping the dust population in disks. Methods. We present multiwavelength continuum observations of CY Tau and DoAr 25 from ALMA at 2.4 and 1.25 mm and archival VLA data at 8.8 mm. Combining the observations with dust continuum forward modeling, we sought to infer a radial profile of the two systems of the dust surface density and maximum emitting grain size. Results. For DoAr 25, the results reveal a prominent dust ring at 111 AU and evidence for large (centimeter-sized) grains extending to the outer disk. In contrast, CY Tau exhibits a more compact and smoother structure, with both the dust surface density and grain size decreasing monotonically with radius. A tentative shoulder feature in the radial profiles, located between 20-40 AU, may point to a marginal substructure, possibly a weak dust trap. Conclusions. DoAr 25 shows evidence for a dust trap capable of halting inward drift, while CY Tau exhibits behavior consistent with evolution dominated by radial drift. Together, these results highlight how dust evolution processes shape the disk morphology and grain-size distributions, even in the low-mass stellar regime.
DOI：10.1051/0004-6361/202661293
