Spiral Structure and Differential Dust Size Distribution in the LkHa 330 Disk
E. Akiyama, J. Hashimoto, H. B. Liu, J. I -H. Li, M. Bonnefoy, R. Dong, Y. Hasegawa, T. Henning, M. L. Sitko, M. Janson, M. Feldt, J. Wisniewski, T. Kudo, N. Ku… 展开作者
E. Akiyama, J. Hashimoto, H. B. Liu, J. I -H. Li, M. Bonnefoy, R. Dong, Y. Hasegawa, T. Henning, M. L. Sitko, M. Janson, M. Feldt, J. Wisniewski, T. Kudo, N. Kusakabe, T. Tsukagoshi, M. Momose, T. Muto, T. Taki, M. Kuzuhara, S. Mayama, M. Takami, N. Ohashi, C. A. Grady, J. Kwon, C. Thalmann, L. Abe, W. Brandner, T. D. Brandt, J. C. Carson, S. Egner, M. Goto, O. Guyon, Y. Hayano, M. Hayashi, S. S. Hayashi, K. W. Hodapp, M. Ishii, M. Iye, G. R. Knapp, R. Kandori, T. Matsuo, M. W. McElwain, S. Miyama, J. -I. Morino, A. Moro-Martin, T. Nishimura, T. -S. Pyo, E. Serabyn, T. Suenaga, H. Suto, R. Suzuki, Y. H. Takahashi, N. Takato, H. Terada, D. Tomono, E. L. Turner, M. Watanabe, T. Yamada, H. Takami, T. Usuda, M. Tamura
Dust trapping accelerates the coagulation of dust particles, and thus it represents an initial step toward the formation of planetesimals. We report $H$-band (1.6 um) linear polarimetric observations and 0.87 mm interferometric continuum observations toward a transitional disk around LkHa 330. As results, a pair of spiral arms were detected in the $H$-band emission and an asymmetric (potentially arm-like) structure was detected in the 0.87 mm continuum emission. We discuss the origin of the spiral arm and the asymmetric structure, and suggest that a massive unseen planet is the most plausible explanation. The possibility of dust trapping and grain growth causing the asymmetric structure was also investigated through the opacity index (beta) by plotting the observed SED slope between 0.87 mm from our SMA observation and 1.3 mm from literature. The results imply that grains are indistinguishable from ISM-like dust in the east side ($beta = 2.0 pm 0.5$), but much smaller in the west side $beta = 0.7^{+0.5}_{-0.4}$, indicating differential dust size distribution between the two sides of the disk. Combining the results of near-infrared and submillimeter observations, we conjecture that the spiral arms exist at the upper surface and an asymmetric structure resides in the disk interior. Future observations at centimeter wavelengths and differential polarization imaging in other bands (Y to K) with extreme AO imagers are required to understand how large dust grains form and to further explore the dust distribution in the disk.
Evolution of dust in a protoplanetary disc driven by stellar flybys: implications for the streaming instability
Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）；Graduate Institute of Astrophysics, National Taiwan University（國立台灣大學天文研究所）；Homer L. Dodge Department of Physics and Astronomy, The University of Oklahoma（歐克拉荷馬大學霍默·L·道奇物理與天文學系）；Department of Physics and Astronomy, The University of Alabama（阿拉巴馬大學物理與天文學系）；Univ. Grenoble Alpes, CNRS, IPAG（格勒諾布爾阿爾卑斯大學、法國國家科學研究中心、IPAG）
From spirals to rings: dust dynamics in gravitoturbulent protoplanetary discs after late infall
IRAP, Université de Toulouse, CNRS, CNES（图卢兹大学 IRAP）；Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦莱布尼茨天体物理研究所）；IPAG, Université Grenoble Alpes, CNRS（格勒诺布尔阿尔卑斯大学 IPAG）；Departamento de Física, Universidad de Santiago de Chile（圣地亚哥智利大学物理系）；Department of Physics and Astronomy, University of Nevada, Las Vegas（内华达大学拉斯维加斯分校物理与天文系）；Max Planck Institut für Astronomie（马克斯·普朗克天文学研究所）；Department of Physics, University of Warwick（沃里克大学物理系）；Université Claude Bernard Lyon 1, ENS de Lyon, CNRS, CRAL（里昂第一大学、里昂高等师范学校 CRAL）；School of Physics and Astronomy, University of Leicester（莱斯特大学物理与天文学院）
Axisymmetric Modeling of DSHARP Dusty Disks: Asymmetric Structures and Inner-Disk Dispersal
College of Science, Ibaraki University（茨城大学理学部）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交通大学李政道研究所）；RIKEN Cluster for Pioneering Research（理化学院先锋研究集群）；Division of Liberal Arts, Kogakuin University（工学院大学人文学部）；National Astronomical Observatory of Japan（日本国立天文台）
Multi-band ALMA Polarization Observations of BHB07-11 Reveal Aligned Dust Grains in Complex Spiral Arm Structures
University of Illinois（伊利诺伊大学）；Carnegie Institution for Science（卡内基科学研究所）；University of Virginia（弗吉尼亚大学）；National Radio Astronomy Observatory（美国国家射电天文台）；Worcester State University（伍斯特州立大学）；Instituto Argentino de Radioastronomía, CCT-La Plata (CONICET)（阿根廷射电天文研究所，拉普拉塔中心（阿根廷科学研究委员会））；Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata（拉普拉塔国立大学天文与地球物理学院）；Zhejiang University（浙江大学）；Seoul National University（首尔大学）
Gravitational instability, spiral substructure, and modest grain growth in a typical protostellar disk: Modeling multi-wavelength dust continuum observation of TMC1A
