Japan Geoscience Union Meeting 2016

Presentation information


Symbol P (Space and Planetary Sciences) » P-PS Planetary Sciences

[P-PS15] New developments of planetary sciences with ALMA

Sun. May 22, 2016 3:30 PM - 5:00 PM A02 (APA HOTEL&RESORT TOKYO BAY MAKUHARI)

Convener:*Munetake Momose(The College of Science, Ibaraki University), Satoshi Okuzumi(Graduate School of Science, Tokyo Institute of Technology), Hiroshi Kobayashi(Department of Physics, Nagoya University), Hideo Sagawa(Faculty of Science, Kyoto Sangyo University), Tetsuo Hasegawa(National Astronomical Observatory of Japan, National Institutes of Natural Sciences), Chair:Satoshi Okuzumi(Graduate School of Science, Tokyo Institute of Technology)

4:15 PM - 4:30 PM

[PPS15-04] ALMA Observations of a Gap and a Ring in the Protoplanetary Disk around TW Hya

*Hideko Nomura1, Takashi Tsukagoshi2, Ryohei Kawabe3, Daiki Ishimoto4,1, Satoshi Okuzumi1, Takayuki Muto5, Kazuhiro Kanagawa6, Shigeru Ida7, Catherine Walsh8, Tom J Millar9, Bai Xue-Ning10 (1.Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 2.College of Science, Ibaraki University, 3.National Astronomical Observatory of Japan, 4.Department of Astronomy, Graduate School of Science, Kyoto University, 5.Division of Liberal Arts, Kogakuin University, 6.University of Szczecin, 7.Earth-Life Science Institute, Tokyo Institute of Technology, 8.Leiden Observatory, Leiden University, 9.Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, 10.Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics)

Keywords:protoplanetary disks, dust continuum emission, gap and ring

We report the first detection of a gap and a ring in 336GHz dust continuum emission from the protoplanetary disk around TW Hya, using the Atacama Large Millimeter/Submillimeter Array (ALMA). The gap and ring are located at around 25 and 41 AU from the central star, respectively, and are associated with the CO snowline at ~ 30AU. The gap has a radial width of less than 15AU and a mass deficit of more than 23%, taking into account that the observations are limited to an angular resolution of ~ 15AU. The observed gap could be caused by gravitational interaction between the disk gas and a planet with a mass less than super-Neptune (2MNeptune), or result from destruction of large dust aggregates due to the sintering of CO ice.