High-angular resolution observations at sub-millimeter/millimeter wavelengths of disks surrounding young stars have shown that their morphology is made of azimuthally-symmetric or point-symmetric substructures, in some cases with spiral arms, localized spur- or crescent-shaped features. The majority of theoretical studies with the aim of interpreting the observational results have focused on disk models with planets, under the assumption that the disk substructures are due to the disk-planet interaction. However, so far only in very few cases exoplanets have been detected in these systems. Furthermore, some substructures are expected to appear \textit{before} planets form, as they are necessary to drive the concentration of small solids which can lead to the formation of planetesimals. In this work we present observational predictions from high-resolution 3D radiative hydrodynamical models which follow the evolution of gas and solids in a protoplanetary disk. We focus on substructures in the distribution of millimeter-sized and smaller solid particles produced by the vertical shear instability. We show that their characteristics are compatible with some of the shallow gaps detected in recent observations at sub-mm/mm wavelengths, and present predictions for future observations with better sensitivity and angular resolution with ALMA and a Next Generation Very Large Array.
The ALMA survey to Resolve exoKuiper belt Substructures (ARKS) III: The vertical structure of debris disks
Universidad de La Laguna（拉古纳大学）；The University of Tokyo（东京大学）；Large Binocular Telescope Observatory, The University of Arizona（亚利桑那大学大型双筒望远镜天文台）；University of Warwick（华威大学）；Max-Planck-Insitut für Astronomie（马克斯·普朗克天文学研究所）；ELTE Eötvös Loránd University（罗兰大学）；Universidad de Santiago（圣地亚哥大学）
A tension between dust and gas radii: the role of substructures and external photoevaporation in protoplanetary disks
Ludwig-Maximilians-Universität München（慕尼黑大学）；Università degli Studi di Milano（米兰大学）；European Southern Observatory（欧洲南方天文台）；INAF, Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；University of Chicago（芝加哥大学）
Late-infall-induced formation of giant planets, multigenerational planetesimals, and disk substructures
Max Planck Institute for Solar System Research（马克斯·普朗克太阳系研究所）；University of Chicago（芝加哥大学）；Ludwig-Maximilians-Universität München（慕尼黑大学）；Exzellenzcluster ORIGINS（ORIGINS卓越集群）
The ALMA survey to Resolve exoKuiper belt Substructures (ARKS) I: Motivation, sample, data reduction, and results overview
University of Warwick（华威大学）；Universidad de La Laguna（拉古纳大学）；Millennium Nucleus on Young Exoplanets and their Moons (YEMS)（年轻系外行星及其卫星千年核）；Center for Interdisciplinary Research in Astrophysics Space Exploration (CIRAS), Universidad de Santiago, Chile（智利圣地亚哥大学天体物理学空间探索跨学科研究中心）；University of Victoria（维多利亚大学）；Institute for Astronomy (IfA), University of Vienna（维也纳大学天体物理研究所）；Institute of Physics and Astronomy, ELTE Eötvös Loránd University（罗兰·厄特沃什大学物理与天文学研究所）；Department of Astronomy, Graduate School of Science, The University of Tokyo（东京大学理学研究科天文学系）；Large Binocular Telescope Observatory, The University of Arizona（亚利桑那大学大双筒望远镜天文台）
Early Planet Formation in Embedded Disks (eDisk). XXV. Inclination-Induced Minor-Axis Brightness Asymmetries Reveal Limited Dust Settling in Embedded Protostellar Disks
University of Virginia（弗吉尼亚大学）；Virginia Institute of Theoretical Astronomy, University of Virginia（弗吉尼亚大学理论天文研究所）；National Radio Astronomy Observatory（国家射电天文台）；Kagoshima University（鹿儿岛大学）
Substructure evolution from protoplanetary to debris disks driven by mutually gravitating planetesimals and implications on Kepler resonances and free-floating planets
California Institute of Technology（加州理工学院）；University of Hawai’i（夏威夷大学）
Diverse dust vertical height and settling strength conditions in protoplanetary discs
Mullard Space Science Laboratory, University College London（穆拉德太空科学实验室，伦敦大学学院）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；School of Astronomy and Space Science, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）；Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学，法国国家科学研究中心，IPAG）；School of Physical Science and Technology, Southwest Jiaotong University（西南交通大学物理科学与技术学院）；School of Natural Sciences, Center for Astronomy, University of Galway（戈尔韦大学自然科学与天文学中心）；Max-Planck Institute for Astronomy (MPIA)（马克斯·普朗克天文学研究所）
Dust segregation in Hall-dominated turbulent protoplanetary disks
从附近原恒星周围的圆盘发出的尘埃连续体的成像揭示了不同的子结构。近年来，理论上的努力已经加强，以调查多远的内在动力学的原行星盘（PPD）可以导致这些功能。在非理想磁流体力学（MHD）领域的湍流是一个候选人，解释产生的纬向流，可以导致当地的尘埃增强。采用径向变化的圆柱盘模型，考虑初始净磁通的垂直和方位组合，对湍流PPDs中由霍尔效应引起的自组织进行了三维非理想MHD模拟。为此，NIRVANA-III和FARGO 3D MHD代码中加入了新的模块。此外，我们还包括尘埃颗粒，在流体近似处理，以研究它们的演变受到新兴的纬向流。在一个占主导地位的霍尔效应的制度，我们稳健地获得大规模的组织浓度的垂直磁场，保持稳定的数百个轨道。对于磁盘与垂直初始净通量单独，我们确认的纬向流和涡的存在下，引入超开普勒气体流的区域。包括一个中等强度的净方位磁通量可以显着改变的动态，部分地防止自组织的纬向流。当等离子体β参数小于50时，在垂直方向的磁通量中会出现大尺度的近轴对称结构。在所有情况下，我们表明，新兴的功能是能够积累的斯托克斯数范围内的尘埃颗粒。
exoALMA XX: Tomographic Detection of Embedded Planets in Protoplanetary Disks
University of Florida（佛罗里达大学）；Leiden University（莱顿大学）；Università degli Studi di Milano（米兰大学）；Max-Planck Institut für Extraterrestrische Physik (MPE)（马克斯·普朗克地外物理学研究所）；Massachusetts Institute of Technology（麻省理工学院）；Max-Planck Institute for Astronomy (MPIA)（马克斯·普朗克天文学研究所）；Université Côte d’Azur（蔚蓝海岸大学）；Observatoire de la Côte d’Azur（蔚蓝海岸天文台）；European Southern Observatory（欧洲南方天文台）
Spirals and Vertical Motions in the Planet-Forming Disk around HD 100546. A multi-line study of its gas kinematics
Massachusetts Institute of Technology（麻省理工学院）；Leiden University（莱顿大学）；University of Florida（佛罗里达大学）；European Southern Observatory（欧洲南方天文台）；University of Michigan（密歇根大学）；Joint ALMA Observatory（ALMA联合观测站）
