Context: Gaps, cavities and rings in circumstellar disks are signposts of disk evolution and planet-disk interactions. We follow the recent suggestion that Herbig Ae/Be disks with a flared disk harbour a cavity, and investigate the disk around HD~97048.
Aims: We aim to resolve the 34$\pm$ 4 au central cavity predicted by Maaskant et al. (2013) and to investigate the structure of the disk.
Methods: We image the disk around HD~97048 using ALMA at 0.85~mm and 2.94~mm, and ATCA (multiple frequencies) observations. Our observations also include the 12CO J=1-0, 12CO J=3-2 and HCO+ J=4-3 emission lines.
Results: A central cavity in the disk around HD~97048 is resolved with a 40-46 au radius. Additional radial structure present in the surface brightness profile can be accounted for either by an opacity gap at ~90 au or by an extra emitting ring at ~150 au. The continuum emission tracing the dust in the disk is detected out to 355 au. The 12CO J=3-2 disk is detected 2.4 times farther out. The 12CO emission can be traced down to $\approx$ 10 au scales. Non-Keplerian kinematics are detected inside the cavity via the HCO+ J=4-3 velocity map. The mm spectral index measured from ATCA observations suggests that grain growth has occurred in the HD~97048 disk. Finally, we resolve a highly inclined disk out to 150 au around the nearby 0.5~$M_{\odot}$ binary ISO-ChaI 126.
Conclusions: The data presented here reveal a cavity in the disk of HD 97048, and prominent radial structure in the surface brightness. The cavity size varies for different continuum frequencies and gas tracers. The gas inside the cavity follows non-Keplerian kinematics seen in HCO+ emission. The variable cavity size along with the kinematical signature suggests the presence of a substellar companion or massive planet inside the cavity.
Validating a Non-conventional Method for Expansion of Coronal Mass Ejections (CMEs) and Investigating the Evolution of a CME Substructures Using Solar Orbiter and Wind Observations
University of Reading（雷丁大学）；Austrian Space Weather Office, GeoSphere Austria（奥地利空间天气办公室，地球系统奥地利）；Indian Institute of Astrophysics（印度天体物理研究所）；Pondicherry University（本地治里大学）
The ALMA survey to Resolve exoKuiper belt Substructures (ARKS) XI: Gas-dust interactions and radial offsets between micron and millimetre-sized grains
The University of Tokyo（东京大学）；Universidad de La Laguna（拉各拉纳加大学）；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（圣地亚哥大学天体物理与空间探索跨学科研究中心）；European Southern Observatory（欧洲南方天文台）；Institute of Physics Belgrade, University of Belgrade（贝尔格莱德大学物理研究所）；Department of Physics and Astronomy, University of Exeter（埃克塞特大学物理与天文学系）；Astrophysikalisches Institut und Universitätssternwarte, Friedrich-Schiller-Universität Jena（耶拿弗里德里希·席勒大学天体物理研究所及大学天文台）；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）；National Astronomical Observatory of Japan（日本国立天文台）
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）
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
The Disk Substructures at High Angular Resolution Project (DSHARP) VI: Dust trapping in thin-ringed protoplanetary disks
ALMA观测到的大部分原行星盘在连续体中显示出多个定义明确且近乎完美的圆环，在许多情况下具有显著的峰谷对比度。DSHARP活动表明，这些环中有几个在径向范围内非常狭窄。在本文中，我们测试的假设，这些尘埃环是由尘埃捕获在径向压力颠簸，如果得到证实，把约束的物理尘埃捕获机制。我们在1D模型分析这个过程，假设轴对称。通过与观测数据的比较，我们发现所有的星环都与尘埃捕获相一致。基于一个合理的尘埃温度模型，我们发现几个环比压力标度的高度更窄，为尘埃捕获提供了强有力的证据。环具有在0.2和0.5之间的范围内的峰值吸收光学深度。储存在每个环中的尘埃质量大约是地球质量的几十倍，尽管由于尘埃不透明度的不确定性，仍然存在许多模糊性。尘埃环的密度足以潜在地触发流动的不稳定性，但我们的分析无法证明这种机制实际上在起作用。然而，我们的结果表明，本文所< 5e-4 and very large grains a_grain >研究的所有环的数据都可以排除非常低的α_turb < > 0.1 cm的组合。
The Ophiuchus DIsk Survey Employing ALMA (ODISEA): A Unified Evolutionary Sequence of Planet-Driven Substructures Explaining the Diversity of Disk Morphologies
