论文标题
金牛座（ALMA-DOT）磁盘流源源的Alma化学调查III：DG TAU的原星磁盘中气体与灰尘之间的相互作用
ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT) III: The interplay between gas and dust in the protoplanetary disk of DG Tau
论文作者
论文摘要
行星形成了原星盘并继承其化学成分。因此，了解磁盘分子含量至关重要。我们旨在表征分子在DG TAU磁盘中的分布和丰度。在金牛座（Alma-dot）中磁盘流源的Alma化学调查中，我们分析了H2CO 3（1,2）-2（1,1），CS 5-4和CN 2-1在〜0.15英寸的Alma观察到DG Tau的磁盘，即在121 pc. H2co和c的unimant and contim and contim and and contim and contim and contim。 CS对H2CO进行探测（分别在〜70和〜60 au处峰值），CN来自最外层的磁盘/信封区域。密度为〜2.4-8.6e13 cm-2（H2CO），〜1.7-2.5e13 cm-2（cs），〜1.9-4.7e13 cm-2（CN）（CN）揭示了在〜40 au时的灰尘发射的环，即在〜40 au中，即snecy sne Snowline（〜30 au）。链接。在1.3mm连续的边缘观察到的分子发射可能是由于内部磁盘中的粉尘不透明度和/或连续的过度提取，以及在MM涂圈的边缘上增加了紫外线的渗透和/或温度倒置。发射也与0.87mm的线性极化的变化相吻合，这表明在CO雪线之外，灰尘特性可能会改变连续体的强度（以及极化的变化）和分子发射。
Planets form in protoplanetary disks and inherit their chemical composition. It is therefore crucial to understand the disks molecular content. We aim to characterize the distribution and abundance of molecules in the disk of DG Tau. In the context of the ALMA chemical survey of Disk-Outflow sources in Taurus (ALMA-DOT) we analyse ALMA observations of the disk of DG Tau in H2CO 3(1,2)-2(1,1), CS 5-4, and CN 2-1 at ~0.15", i.e. ~18 au at 121 pc. H2CO and CS originate from a disk ring at the edge of the 1.3mm dust continuum, with CS probing an outer disk region with respect to H2CO (peaking at ~70 and ~60 au, respectively). CN originates from an outermost disk/envelope region peaking at ~80 au. H2CO is dominated by disk emission, while CS probes also two streams of material possibly accreting onto the disk with a peak of emission where the stream connects to the disk. The ring- and disk-height- averaged column densities are ~2.4-8.6e13 cm-2 (H2CO), ~1.7-2.5e13 cm-2 (CS), and ~1.9-4.7e13 cm-2 (CN). Unsharp masking reveals a ring of enhanced dust emission at ~40 au, i.e. just outside the CO snowline (~30 au). CS and H2CO emissions are co-spatial suggesting that they are chemically linked. The observed rings of molecular emission at the edge of the 1.3mm continuum may be due to dust opacity effects and/or continnum over-subtraction in the inner disk; as well as to increased UV penetration and/or temperature inversion at the edge of the mm-dust which would cause an enhanced gas-phase formation and desorption of these molecules. Moreover, H2CO and CS originate from outside the ring of enhanced dust emission, which also coincides with a change of the linear polarization at 0.87mm. This suggests that outside the CO snowline there could be a change of the dust properties which would reflect in the increase of the intensity (and change of polarization) of continuum, and of molecular emission.
