Japan Geoscience Union Meeting 2019

Presentation information

[J] Poster

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

[P-CG24] New Developments of Planetary Sciences with ALMA

Wed. May 29, 2019 3:30 PM - 5:00 PM Poster Hall (International Exhibition Hall8, Makuhari Messe)

convener:Takayuki Muto(Division of Liberal Arts, Kogakuin University), Munetake Momose(The College of Science, Ibaraki University), Hideo Sagawa(Faculty of Science, Kyoto Sangyo University), Masumi Shimojo(National Astronomical Observatory of Japan)

[PCG24-P02] Investigating the gas-to-dust ratio in the protoplanetary disk of HD 142527

*Soon Kang-Lou1, Munetake Momose1, Takayuki Muto2, Takashi Tsukagoshi3, Akimasa Kataoka3, Tomoyuki Hanawa4, Misato Fukagawa3, Kazuya Saigo3, Hiroshi Shibai5 (1.Ibaraki University, 2.Kogakuin University, 3.National Astronomical Observatory of Japan, 4.Chiba University, 5.Osaka University)

Keywords:HD 142527, protoplanetary disk, gas-to-dust ratio

We present the ALMA observations of the 98.5 GHz dust continuum and the 13CO J = 1 – 0 and C18O J = 1 – 0 line emission towards the protoplanetary disk of HD 142527. The 98.5 GHz continuum shows a strong azimuthal-asymmetric distribution similar to the previously reported 336 GHz continuum, and its peak emission at the dust concentrated northern region is optically thin at approximately 8 K. In every position angle, the peak brightness temperature of C18O J = 1 – 0 emission (≦ 25 K) is lower than that of the optically thick 13CO J = 3 – 2 (≈ 36 K), indicating that the C18O is optically thin. We derive the gas and dust surface densities, Σg and Σd, of the disk of HD 142527 by using the ALMA Band 3 and Band 7 observations. In the analyses we assume the local thermodynamic equilibrium and the disk temperature to be the same as the peak brightness temperature of 13CO J = 3 – 2 with continuum emission. We successfully derived the gas-to-dust ratio G/D, defined as Σgd, distribution across the disk. The ratio varies azimuthally, where it is ∼3 and ∼20 in the disk northern and southern regions, respectively. We also found that Σg varies approximately as ∝ Σd0.5, or equivalently G/D ∝ Σd-0.5. In addition, our results show that the peak Σd is located ahead of the peak Σg; if the latter correspond to a vortex of high gas pressure, the results indicate that the dust are trapped ahead of the vortex, which is predicted by theoretical studies.