Ionized gas emission in protoplanetary disks with the SKAO
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，天体物理学与行星学研究所）；School of Physics and Astronomy, University of Leeds（利兹大学物理与天文学学院）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；School of Physics and Astronomy, University of Leicester（莱斯特大学物理与天文学学院）
Greta Guidi, Christian Rab, Barbara Ercolano, Michael L. Weber, Claudio Codella, Izaskun Jiménez-Serra, Evgenia Koumpia, John D. Ilee, Enrique Macías, Elena Vis… 展开作者
Greta Guidi, Christian Rab, Barbara Ercolano, Michael L. Weber, Claudio Codella, Izaskun Jiménez-Serra, Evgenia Koumpia, John D. Ilee, Enrique Macías, Elena Viscardi, Yinhao Wu, Francesca Bacciotti, Asmita Bhandare, Eleonora Bianchi, Tyler Bourke, Luca Cacciapuoti, Antonio Garufi, Geoffroy Lesur, Vincent Piétu, Linda Podio, Giovanni Sabatini, Leonardo Testi, Claudia Toci
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Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Guidi01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopes
Protoplanetary disks represent a crucial stage in the evolution of Young Stellar Objects towards the formation of fully formed planetary systems. While substantial progress has been made in the last decades in the characterization of the dust and molecular gas in these systems, the ionized component remains poorly understood. Ionized gas traces important processes such as photoevaporation, accretion, disk winds, and jets, and therefore is key to studying disk dynamics, evolution, and ultimately planet formation. In this paper, we investigate the capabilities of the forthcoming SKA telescope to probe this component in protoplanetary disks within nearby star forming regions. We present state-of-the-art simulations of photoevaporative, magneto-thermal, and magnetohydrodynamic winds, and generate theoretical predictions and synthetic SKAO observations to assess its potential in detecting and characterizing free-free emission and Hydrogen recombination lines. Finally, we discuss synergies with complementary facilities and how they will provide a comprehensive, multi-scale view of disk winds and offer critical insights on the mechanisms driving disk evolution and the onset of planet formation.
Correlation between accretion rate and free-free emission in protoplanetary disks -- A multi-wavelength analysis of central mm/cm emission in transition disks
Unveiling Complex Chemistry in Planet-forming Disks with the SKAO
University of Leeds（利兹大学）；Univ Toulouse, CNES, CNRS, IRAP（图卢兹大学，法国国家空间研究中心，法国国家科学研究中心，天体物理研究所）；Academia Sinica Institute of Astronomy and Astrophysics（中央研究院天文及天文物理研究所）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Tata Institute of Fundamental Research（塔塔基础研究所）；Institute for Research in Fundamental Sciences（伊朗基础科学研究院）；United Kingdom Astronomy Technology Centre（英国天文学技术研究中心）；National Institute of Science Education and Research（国家科学教育与研究学院）；Homi Bhabha National Institute（霍米·巴哈国立学院）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Monash University（蒙纳士大学）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；University of Leicester（莱斯特大学）
Perspectives for the study of gas in protoplanetary disks and accretion/ejection phenomena in young stars with the near-IR spectrograph SPIROU at the CFHT
Probing Protoplanetary Disk Winds with C II Absorption
我们提出了一个分析的风吸收的C II $λ1335$双峰对40个经典的金牛座T星档案远紫外（FUV）光谱的哈勃太空望远镜。在我们的样本中，通常检测到由快速或慢速风产生的吸收特征（40个目标中的36个）。快风的风速随着圆盘倾角的减小而减小，这与准直射流的预期一致。慢风吸收检测主要是在磁盘与中间或高的倾斜，没有一个显着的依赖于磁盘倾斜的风速。在中性或单电离原子的FUV谱线中，快速和慢速风吸收都被优先探测到。Mg II $λλ2796,2804$谱线显示风吸收与C II谱线中的吸收一致。我们开发了简化的半解析圆盘/风模型来解释观测的圆盘风吸收。快风和慢风都与热磁化盘风模型的预期一致，并且通常与纯热风不一致。这两个模型和观测分析表明，风的吸收发生优先从内部磁盘，提供了一个风诊断补充光学禁止线发射，跟踪风在更大的体积。
Mapping Molecular Ion Distributions in a Diverse Sample of Protoplanetary Disks
University of Virginia（弗吉尼亚大学）；University of Minnesota（明尼苏达大学）；University of Michigan（密歇根大学）；U.S. Naval Academy（美国海军学院）；Harvard-Smithsonian Center for Astrophysics（哈佛-史密森天体物理中心）；Columbia University（哥伦比亚大学）；Wesleyan University（卫斯理安大学）；Boston University（波士顿大学）
Beyond the $α$ model: scaling the wind-driven accretion rate in protoplanetary disks using systematic non-ideal magnetohydrodynamical simulations
Department of Earth and Planetary Sciences, Institute of Science Tokyo（东京科学地球与行星科学系）；Institute for Advanced Study and Department of Astronomy, Tsinghua University（清华大学高等研究院天文学系）
JWST/MIRI Detection of Molecular H$_2$ Winds from an Edge-on Class II Source HV Tau C
Tata Institute of Fundamental Research（塔塔基础研究所）；Max-Planck-Institut für Astronomie (MPIA)（马克斯·普朗克天文学研究所）；Kapteyn Astronomical Institute, Rijksuniversiteit Groningen（格罗宁根大学卡佩因天文研究所）；INAF – Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）
研究利用JWST/MIRI-MRS数据分析近边缘取向的II类盘HV Tau C分子氢发射特性，探测到广角双锥分子风，估计其质量损失率等，发现分子H₂风对盘演化等仍重要，吸积率或因边缘取向被低估。
VLA cm-wave survey of young stellar objects in the Oph A cluster: constraining extreme UV- and X-ray-driven disk photo-evaporation -- A pathfinder for Square Kilometre Array studies
