JpGU-AGU Joint Meeting 2017

Presentation information

[EJ] Poster

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

[P-PS04] [EJ] New developments of planetary sciences with ALMA

Wed. May 24, 2017 3:30 PM - 5:00 PM Poster Hall (International Exhibition Hall HALL7)

convener:Munetake Momose(The College of Science, Ibaraki University), Hiroshi Kobayashi(Department of Physics, Nagoya University), Masumi Shimojo(National Astronomical Observatory of Japan), Hideko Nomura(Department of Earth and Planetary Sciences, Tokyo Institute of Technology)

[PPS04-P04] Observations of dust continuum emission at 1.3mm from the protoplanetary disk around DG Tau

*Munetake Momose1, Takashi Tsukagoshi1, Kang-Lou Soon1, Aya Higuchi2, Takayuki Muto3, Satoshi Okuzumi4, Misato Fukagawa5, Hidekazu Tanaka6 (1.The College of Science, Ibaraki University, 2.RIKEN, 3.Division of Liberal Arts, Kogakuin University, 4.Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 5.Graduate School of Science, Nagoya University, 6.Astronomical Institute, Tohoku University)

Keywords:protoplanetary disk, radio astronomy

We report the ALMA long-baseline observations of dust continuum emission at 1.3mm from the protoplanetary disk around DG Tau. DG Tau is a young T Tauri star in Taurus molecular clouds. It exhibits features such as a circumstellar envelope ~1000au in size, ionized jets, and vigorous mass accretion (> 10-6 Msun /yr ) onto the star. These are common to HL Tau whose protoplanetary disk was nicely imaged in the long-baseline campaign, making DG Tau an ideal object for examining the origin and universality of the ring-like features found in the HL Tau's disk. Based on the jet kinematics and gas rotation in r < 400au, the inclination and stellar mass were estimated to be 38deg and 0.67Msun. Our present observations at the wavelength of 1.3mm have provided us with a image of dust continuum emission at the beam size of ~36 milli-arcseconds, or 5au. The overall structure of the disk is axisymmetric, and the surface brightness distribution is radially smooth, approximately following power-laws of r-0.55 in r< 12.5au and r-1.22 in 12.5au < r < 50au, respectively, with steep tapering beyond r = 50au. Though the inner regions (r< 12.5au) seems optically thick at 1.3mm, the surface density distribution in r > 15au suggested from these results agrees with a classical accretion disk model. Other intriguing features are several gaps seen in 12.5au < r < 50au, with their relative decrements of ~ 7% from the power-law distribution. These are reminiscent of spectacular concentric rings around HL Tau, and their nature should be explored further by multi-band observations with ALMA in near future.