Disk Dynamics Collaboration, Philip J. Armitage, Jaehan Bae, Myriam Benisty, Edwin A. Bergin, Simon Casassus, Ian Czekala, Stefano Facchini, Jeffrey Fung, Cassa… 展开作者
Disk Dynamics Collaboration, Philip J. Armitage, Jaehan Bae, Myriam Benisty, Edwin A. Bergin, Simon Casassus, Ian Czekala, Stefano Facchini, Jeffrey Fung, Cassandra Hall, John D. Ilee, Miriam Keppler, Aleksandra Kuznetsova, Romane Le Gal, Ryan A. Loomis, Wladimir Lyra, Natascha Manger, Sebastian Perez, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Judit Szulagyi, Kamber Schwarz, Jacob B. Simon, Richard Teague, Ke Zhang
A stunning range of substructures in the dust of protoplanetary disks is routinely observed across a range of wavelengths. These gaps, rings and spirals are highly indicative of a population of unseen planets, hinting at the possibility of current observational facilities being able to capture planet-formation in action. Over the last decade, our understanding of the influence of a young planet on the dynamical structure of its parental disk has progressed significantly, revealing a host of potentially observable features which would betray the presence of a deeply embedded planet. In concert, recent observations have shown that subtle perturbations in the kinematic structure of protoplanetary disks are found in multiple sources, potentially the characteristic disturbances associated with embedded planets. In this work, we review the theoretical background of planet-disk interactions, focusing on the kinematical features, and the current methodologies used to observe these interactions in spatially and spectrally resolved observations. We discuss the potential pit falls of such kinematical detections of planets, providing best-practices for imaging and analysing interferometric data, along with a set of criteria to use as a benchmark for any claimed detection of embedded planets. We finish with a discussion on the current state of simulations in regard to planet-disk interactions, highlighting areas of particular interest and future directions which will provide the most significant impact in our search for embedded planets. This work is the culmination of the 'Visualizing the Kinematics of Planet Formation' workshop, held in October 2019 at the Center for Computational Astrophysics at the Flatiron Institute in New York City.
Planetary gas gaps and kinematic signatures in the planet forming disk around WISPIT 2
Leiden University（莱顿大学）；European Southern Observatory（欧洲南方天文台）；University of Florida（佛罗里达大学）；Peking University（北京大学）；University College Cork（科克大学）；Trinity College Dublin, The University of Dublin（都柏林三一学院，都柏林大学）；University of Galway（高威大学）
Planets Across Space and Time (PAST). I. Characterizing the Memberships of Galactic Components and Stellar Ages: Revisiting the Kinematic Methods and Applying to Planet Host Stars
Kinematic evidence for an embedded planet in the IM Lupi disc
我们测试的假设，一个嵌入式的巨行星在IM卢皮原恒星盘可以产生速度扭结在CO线观测，以及在散射光和连续辐射看到的螺旋臂。我们将行星注入到IM Lupi的三维流体动力学模拟中，使用Monte Carlo辐射转移生成合成观测。我们发现，嵌入式行星的2-3倍的木星质量可以重现非开普勒速度扰动，或“扭结”，在12 CO J=2-1通道地图。这样的行星也可以解释在1.25毫米尘埃连续辐射和1.6微米散射光图像中看到的螺旋臂。我们发现，可以跟踪观察到的峰值速度图，这似乎密切遵循我们的模拟和行星盘相互作用的分析模型预期的形态的行星的尾流。
Kinematic and thermal signatures of the directly imaged protoplanet candidate around Elias 2-24
我们报告与直接成像的原行星候选人在埃利亚斯2-24光盘的运动学和热签名。使用DSHARP ALMA观测的$^{12}$ CO J=2-1线，我们表明，光盘运动学扰动，与分离的CO发射点的位置的行星候选人和痕迹的螺旋尾迹，也是所观察到的CO发射强度需要本地加热。虽然前景灭绝隐藏了与行星相关的速度通道，阻止了行星质量的估计，但CO排放所暗示的气体加热水平表明存在一颗温暖的嵌入式巨行星。与模型的比较显示，这可能是一颗$\gtrsim 5$ M $_\mathrm{Jup}$，也可能是一颗质量较低但正在吸积的原行星（$\gtrsim 2$ M $_\mathrm{Jup}$）。
Chemical abundances and kinematics of 257 G-, K-type field giants. Setting a base for further analysis of giant-planet properties orbiting evolved stars
A new planet candidate detected in a dust gap of the disc around HD 163296 through localised kinematic signatures. An observational validation of the Discminer
Planets Across Space and Time (PAST) IV: The Occurrence and Architecture of Kepler Planetary Systems as a Function of Kinematic Age Revealed by the LAMOST-Gaia-Kepler Sample
Kinematic Evidence of an Embedded Protoplanet in HD 142666 Identified by Machine Learning
The University of Georgia（佐治亚大学）；University of California, San Francisco（加州大学旧金山分校）；Cardiovascular Research Institute（心血管研究所）；The University of Alabama（阿拉巴马大学）
Galactic Kinematics and Observed Flare Rates of a Volume-Complete Sample of Mid-to-Late M-dwarfs: Constraints on the History of the Stellar Radiation Environment of Planets Orbiting Low-mass Stars
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）
