Evolution of protoplanetary disks from their taxonomy in scattered light: spirals, rings, cavities, and shadows
Antonio Garufi, Myriam Benisty, Paola Pinilla, Marco Tazzari, Carsten Dominik, Christian Ginski, Thomas Henning, Quentin Kral, Maud Langlois, Francois Menard, T… 展开作者
Antonio Garufi, Myriam Benisty, Paola Pinilla, Marco Tazzari, Carsten Dominik, Christian Ginski, Thomas Henning, Quentin Kral, Maud Langlois, Francois Menard, Tomas Stolker, Judit Szulagyi, Marion Villenave, Gerrit van der Plas
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16 pages, 8 figures, accepted for publication by A&A
The variety of observed protoplanetary disks in polarimetric light motivates a taxonomical study to constrain their evolution and establish the current framework of this type of observations. We classified 58 disks with available polarimetric observations into six major categories (Ring, Spiral, Giant, Rim, Faint, and Small disks) based on their appearance in scattered light. We re-calculated the stellar and disk properties from the newly available GAIA DR2 and related these properties with the disk categories. More than a half of our sample shows disk sub-structures. For the remaining sources, the absence of detected features is due to their faintness, to their small size, or to the disk geometry. Faint disks are typically found around young stars and typically host no cavity. There is a possible dichotomy in the near-IR excess of sources with spiral-disks (high) and ring-disks (low). Like spirals, shadows are associated with a high near-IR excess. If we account for the pre-main sequence evolutionary timescale of stars with different mass, spiral arms are likely associated to old disks. We also found a loose, shallow declining trend for the disk dust mass with time. Protoplanetary disks may form sub-structures like rings very early in their evolution but their detectability in scattered light is limited to relatively old sources (more than 5 Myr) where the recurrently detected disk cavities allow to illuminate the outer disk. The shallow decrease of disk mass with time might be due to a selection effect, where disks observed thus far in scattered light are typically massive, bright transition disks with longer lifetime than most disks. Our study points toward spirals and shadows being generated by planets of fraction-to-few Jupiter masses that leave their (observed) imprint on both the inner disk near the star and the outer disk cavity.
Observational signatures of eccentric Jupiters inside gas cavities in protoplanetary discs
预测一颗年轻行星如何塑造其母行星盘的气体和尘埃排放是限制原行星盘观测中不可见行星存在的关键。我们调查的情况下，2木星质量的行星，成为偏心后，迁移到一个低密度的气体空腔在其母盘。进行二维流体动力学模拟，并通过三维辐射转移计算进行后处理。在我们的圆盘模型中，行星偏心率达到~0.25，这导致空腔内气体密度的强烈不对称。这些不对称性通过光解离而增强，并且在12 CO J=3-2积分强度图中形成大尺度不对称性。它们被证明是可检测的角分辨率和噪声水平类似的ALMA观测中实现的。此外，行星的偏心率使空腔内的气体偏心，这表现为12 CO J=3-2的速度图中的等速度线变窄，拉伸和扭曲。然而，行星的偏心率并没有引起可检测的签名，在13 CO和C18 O J=3-2内的腔，因为低柱密度。在腔外，气体保持近圆形轨道，垂直延伸的光学厚CO发射在圆盘倾角> 30度的积分强度图中显示出四瓣图案。在我们的模型中，空腔内缺乏大小尘埃，这进一步意味着当行星在空腔内偏心或仍然是圆形时，亚毫米连续辐射的合成图像和近红外偏振散射光的合成图像不会显示出显着差异。
Astrometric view of companions in the inner dust cavities of protoplanetary disks
European Southern Observatory（欧洲南方天文台）；School of Physics and Astronomy, University of Leeds（利兹大学物理与天文学学院）；Dipartimento di Fisica, Università degli Studi di Milano（米兰大学物理系）；Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理学研究所）；Max-Planck-Institut für Astronomie (MPIA)（马克斯·普朗克天文学研究所）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；INAF - Istituto di Radioastronomia（意大利国家天体物理研究所射电天文研究所）；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家研究委员会-国家航空航天技术研究所天体生物学中心）；Astronomy Unit, School of Physics and Astronomy, Queen Mary University of London（伦敦大学玛丽女王学院物理与天文学学院天文学单元）
Correlation between accretion rate and free-free emission in protoplanetary disks -- A multi-wavelength analysis of central mm/cm emission in transition disks
The Disk Substructures at High Angular Resolution Project (DSHARP): III. Spiral Structures in the Millimeter Continuum of the Elias 27, IM Lup, and WaOph 6 Disks
