Japan Geoscience Union Meeting 2018

Presentation information

[JJ] Oral

P (Space and Planetary Sciences) » P-CG Complex & General

[P-CG22] New Developments of Planetary Sciences with ALMA

Wed. May 23, 2018 9:00 AM - 10:30 AM A02 (Tokyo Bay Makuhari Hall)

convener:Takayuki Muto(Division of Liberal Arts, Kogakuin University), Munetake Momose(The College of Science, Ibaraki University), Hideo Sagawa(京都産業大学理学部, 共同), Masumi Shimojo(National Astronomical Observatory of Japan), Chairperson:Muto Takayuki

9:00 AM - 9:15 AM

[PCG22-01] A Spatially Resolved AU-scale Inner Disk around DM Tau with ALMA

*Jun Hashimoto1, Hauyu Liu7, Ruobing Dong6, Mihoko Konishi2, Takayuki Muto3, Yasuhiro Hasegawa4, Takashi Tsukagoshi5, Tomoyuki Kudo2 (1.The National Institutes of Natural Sciences, Astrobiology center, 2.The National Institutes of Natural Sciences, National Astronomical Observatory of Japan, 3.Kogakuin University, 4.NASA Jet Propulsion Laboratory, 5.Ibaraki University, 6.Arizona University, 7.Max Planck Institute for Astronomy)

Keywords:protoplanetary disk, ALMA, transitional disk

We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the dust continuum at 1.3 mm and 12CO (2-1) line of the transitional disk around DM Tau. DM Tau exhibits no near-infrared (NIR) excess in its spectral energy distribution (SED), which means the inner cavity is well depleted. However we found a spatially resolved inner disk at about r =3 AU in the dust continuum image. Assuming the inner disk's temperature of 200 K, a dust mass of the inner disk is about 0.2 Mjup. The brightness structures in both the dust continuum and the 12CO (2-1) are marginally asymmetric: 1.15 +- 0.08 and 1.47 +- 0.16 times brighter in the northwest part in the inner disk, respectively. We also performed a simple analytic modeling of the disk's brightness profile, and derived physical disk parameters by fitting the observed visibilities. Our modeling efforts found DM Tau's dust disk consists of three components: an inner disk, an outer disk, and an extended structure. In the presentation, we will discuss possible origins of the multi-ring structure around DM Tau.