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arXiv 2103.02666astro-ph.SRastro-ph.EP
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一个不寻常的边缘上的原行星盘的解剖。II。气体温度和温暖的外部区域

The Anatomy of an Unusual Edge-on Protoplanetary Disk. II. Gas temperature and a warm outer region

Christian Flores, Gaspard Duchene, Schuyler Wolff, Marion Villenave, Karl Stapelfeldt, Jonathan P. Williams, Christophe Pinte, Deborah Padgett, Michael S. Conne… 展开作者

Christian Flores, Gaspard Duchene, Schuyler Wolff, Marion Villenave, Karl Stapelfeldt, Jonathan P. Williams, Christophe Pinte, Deborah Padgett, Michael S. Connelley, Gerrit van der Plas, Francois Menard, Marshall D. Perrin

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27 pages, 18 figures, 1 table
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摘要：

我们提出了高分辨率$^{12}$ CO和$^{13}$ CO 2 - 1 ALMA观测，以及光学和近红外光谱，高度倾斜的原行星盘周围的SSTC 2D J163131.2 - 242627。光谱类型，我们得到的来源是一致的$\rm 1.2 \, M_{\odot}$明星推断ALMA的意见。尽管它有巨大的拱星盘，但我们几乎没有发现恒星上正在进行吸积的证据。CO地图揭示了一个磁盘，是异常紧凑的垂直方向，其外观在散射光图像一致。气体盘延伸的距离大约是亚毫米连续谱和光学散射光的两倍。从由中平面区域分离的两个表面层检测到CO，在中平面区域中，CO排放被抑制，如从冷中平面中的冻结所预期的。我们应用Dutrey等人2017年提出的地形重建分布方法的修改版本来推导圆盘的温度结构。我们发现，在CO发光层和$\sim$ 33 K和$\sim$ 20 K的中平面的温度在$\rm R<200$金，分别。在$\rm R>200$ Au之外，盘的中平面温度增加到$\sim$ 30 K，具有几乎垂直的等温轮廓。CO温度的转变与圆盘的亚微米和亚毫米发射的急剧减少相吻合。我们将其解释为星际紫外线辐射为圆盘的外部提供了额外的热源。

英文摘要：

We present high-resolution $^{12}$CO and $^{13}$CO 2-1 ALMA observations, as well as optical and near-infrared spectroscopy, of the highly-inclined protoplanetary disk around SSTC2D J163131.2-242627. The spectral type we derive for the source is consistent with a $\rm 1.2 \, M_{\odot}$ star inferred from the ALMA observations. Despite its massive circumstellar disk, we find little to no evidence for ongoing accretion on the star. The CO maps reveal a disk that is unusually compact along the vertical direction, consistent with its appearance in scattered light images. The gas disk extends about twice as far away as both the submillimeter continuum and the optical scattered light. CO is detected from two surface layers separated by a midplane region in which CO emission is suppressed, as expected from freeze-out in the cold midplane. We apply a modified version of the Topographically Reconstructed Distribution method presented by Dutrey et al. 2017 to derive the temperature structure of the disk. We find a temperature in the CO-emitting layers and the midplane of $\sim$33 K and $\sim$20 K at $\rm R<200$ au, respectively. Outside of $\rm R>200$ au, the disk's midplane temperature increases to $\sim$30 K, with a nearly vertically isothermal profile. The transition in CO temperature coincides with a dramatic reduction in the sub-micron and sub-millimeter emission from the disk. We interpret this as interstellar UV radiation providing an additional source of heating to the outer part of the disk.

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