論文

査読有り
2019年1月

The Flared Gas Structure of the Transitional Disk around Sz 91

Astrophysical Journal
  • Takashi Tsukagoshi
  • ,
  • Munetake Momose
  • ,
  • Yoshimi Kitamura
  • ,
  • Masao Saito
  • ,
  • Ryohei Kawabe
  • ,
  • Sean Andrews
  • ,
  • David Wilner
  • ,
  • Tomoyuki Kudo
  • ,
  • Jun Hashimoto
  • ,
  • Nagayoshi Ohashi
  • ,
  • Motohide Tamura

871
1
開始ページ
5
終了ページ
18
記述言語
英語
掲載種別
研究論文(学術雑誌)
DOI
10.3847/1538-4357/aaf4f1

We report $0.14&quot;$ resolution observations of the dust continuum at band 7,<br />
and the CO(3--2) and HCO$^{+}$(4--3) line emissions toward the transitional<br />
disk around Sz 91 with Atacama Large Millimeter/submillimeter Array (ALMA). The<br />
dust disk appears to be an axisymmetric ring, peaking a radius of $\sim$95~au<br />
from a Gaussian fit. The Gaussian fit widths of the dust ring are 24.6 and<br />
23.7~au for the major and the minor axes, respectively, indicating that the<br />
dust ring is not geometrically thin. The gas disk extends out to $\sim$320~au<br />
and is also detected in the inner hole of the dust ring. A twin-line pattern is<br />
found in the channel maps of CO, which can be interpreted as the emission from<br />
the front and rear of the flared gas disk. We perform the radiative transfer<br />
calculations using RADMC-3D, to check whether the twin-line pattern can be<br />
reproduced under the assumption that the flared gas disk has a power-law form<br />
for the column density and $T_\mathrm{gas}=T_\mathrm{dust}$. The thermal Monte<br />
Carlo calculation in RADMC-3D shows that the disk temperature has a gradient<br />
along the vertical direction beyond the dust ring, as it blocks the stellar<br />
radiation, and thus the twin-line pattern can be naturally explained by the<br />
flared gas disk in combination with the dust ring. In addition, no significant<br />
depletion of the CO molecules in the cold midplane achieves a reasonable<br />
agreement with the observed twin-line pattern. This result indicates that the<br />
CO emission from the rear surface must be heavily absorbed in the cold<br />
midplane.

リンク情報
DOI
https://doi.org/10.3847/1538-4357/aaf4f1
arXiv
http://arxiv.org/abs/arXiv:1811.12036
URL
http://iopscience.iop.org/article/10.3847/1538-4357/aaf4f1/meta