Molecules with ALMA at Planet-forming Scales (MAPS). III. Characteristics of Radial Chemical Substructures-猫眼课题宝

DOI：

10.3847/1538-4365/ac1434

发表时间：

2021-09

期刊：

The Astrophysical Journal Supplement Series

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

C. Law;R. Loomis;R. Teague;K. Öberg;I. Czekala;S. Andrews;Jane Huang;Y. Aikawa;Felipe Alarc'on;J. Bae;E. Bergin;J. Bergner;Y. Boehler;A. Booth;A. Bosman;Jenny K. Calahan;G. Cataldi;L. Cleeves;K. Furuya;V. Guzmán;J. Ilee;R. Le Gal;Yao Liu;F. Long;F. Ménard;H. Nomura;C. Qi;K. Schwarz;A. Sierra;T. Tsukagoshi;Yoshihide Yamato;M. V. ’. van ’t Hoff;C. Walsh;D. Wilner;Kecheng Zhang

行星形成尺度上的分子ALMA （MAPS）大程序提供了与行星形成相关的空间尺度上5个原行星盘中分子线发射的详细、高分辨率（~ 10-20 au）视图。本文对imlup、GM Aur、as209、hd163296、MWC 480等18个分子系的化学亚结构进行了系统分析。我们确定了200多个化学亚结构，这些亚结构几乎在所有检测到线发射的半径上都有发现。在每个圆盘内和map样本中都观察到各种各样的径向形态，包括环状、间隙和高原。这种谱线发射谱线的多样性也存在于最内层的50 au内。总的来说，这表明行星在不同的化学环境中形成，无论是在圆盘上还是在同一圆盘内不同的半径上。在150 au以内，map盘上的大多数化学子结构在空间上与毫米连续体中的子结构一致，表明盘中部与温暖的、升高的分子发射层之间存在物理和化学联系。然而，盘内的一些化学亚结构和150 au以外的大多数化学亚结构不能直接与尘埃亚结构联系起来，这表明还有其他化学亚结构的原因，如雪线、紫外光子通量的梯度、电离和径向变化的元素比。这意味着，除了影响行星聚集的环境外，化学亚结构还可以发展成具有不同磁盘特征的强大探测器。这篇论文是《天体物理学杂志增刊》MAPS特刊的一部分。

The Molecules with ALMA at Planet-forming Scales (MAPS) Large Program provides a detailed, high-resolution (∼10–20 au) view of molecular line emission in five protoplanetary disks at spatial scales relevant for planet formation. Here we present a systematic analysis of chemical substructures in 18 molecular lines toward the MAPS sources: IM Lup, GM Aur, AS 209, HD 163296, and MWC 480. We identify more than 200 chemical substructures, which are found at nearly all radii where line emission is detected. A wide diversity of radial morphologies—including rings, gaps, and plateaus—is observed both within each disk and across the MAPS sample. This diversity in line emission profiles is also present in the innermost 50 au. Overall, this suggests that planets form in varied chemical environments both across disks and at different radii within the same disk. Interior to 150 au, the majority of chemical substructures across the MAPS disks are spatially coincident with substructures in the millimeter continuum, indicative of physical and chemical links between the disk midplane and warm, elevated molecular emission layers. Some chemical substructures in the inner disk and most chemical substructures exterior to 150 au cannot be directly linked to dust substructure, however, which indicates that there are also other causes of chemical substructures, such as snowlines, gradients in UV photon fluxes, ionization, and radially varying elemental ratios. This implies that chemical substructures could be developed into powerful probes of different disk characteristics, in addition to influencing the environments within which planets assemble. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement.

Molecules with ALMA at Planet-forming Scales (MAPS). III. Characteristics of Radial Chemical Substructures

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