The Anatomy of an Unusual Edge-on Protoplanetary Disk. II. Gas Temperature and a Warm Outer Region
The Anatomy of an Unusual Edge-on Protoplanetary Disk. II. Gas Temperature and a Warm Outer Region
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DOI：
10.3847/1538-3881/abeb1e
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发表时间：
2021-03
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影响因子：
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通讯作者：
Christian Flores;G. Duchêne;S. Wolff;M. Villenave;K. Stapelfeldt;Jonathan P. Williams;C. Pinte;D. Padgett;M. Connelley;G. V. D. Plas;F. Menard;M. Perrin
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文献类型：
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作者：
Christian Flores;G. Duchêne;S. Wolff;M. Villenave;K. Stapelfeldt;Jonathan P. Williams;C. Pinte;D. Padgett;M. Connelley;G. V. D. Plas;F. Menard;M. Perrin
我们提出了高分辨率的12 CO和13 CO 2-1阿尔马观测，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，我们得到的源是一致的1.2 M的星星推断从阿尔马的意见。尽管它有巨大的拱星盘，我们几乎没有发现星星正在吸积的证据。CO图显示了一个磁盘，是非常紧凑的沿着垂直方向，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等人提出的断层重建分布方法的修改版本。推导出磁盘的温度结构。当R = 200 Au时，CO发光层和中平面的温度分别为33 K和20 K，盘的中平面温度上升到30 K，并具有近似垂直的等温分布。CO温度的转变与磁盘的亚微米和亚毫米辐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。
We present high-resolution 12CO and 13CO 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 1.2 M ⊙ 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 tomographically reconstructed distribution method presented by Dutrey et al. to derive the temperature structure of the disk. We find a temperature in the CO-emitting layers and the midplane of ∼33 K and ∼20 K at R 200 au, the disk’s midplane temperature increases to ∼30 K, with a nearly vertically isothermal profile. The transition in CO temperature coincides with a dramatic reduction in the submicron and submillimeter emission from the disk. We interpret this as interstellar UV radiation providing an additional source of heating to the outer part of the disk.