Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing Protoplanetary Disk Structure within 20 au-猫眼课题宝

DOI：

10.3847/1538-4365/ac1433

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：

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

限制气体和尘埃在原行星盘内部20 Au的分布是困难的。同时，这个区域被认为是大多数行星形成的原因，特别是在3-10 Au的水冰线周围。在Keplerian盘的假设下，我们利用分子的灵敏度和行星形成尺度（MAPS）阿尔马大型程序阿尔马，利用线速度剖面，对CO同位素J = 2-1谱线构造了有效分辨率为100 ~ 3 Au的径向表面亮度剖面。IM Lup揭示了13 CO和C18 O的中心低压，这归因于内部20 Au中堆积了约500 M Au的尘埃，导致气尘比约为10），并且尘埃间隙中的气体足够丰富，具有光学厚度的C18 O。本文是《天体物理学杂志增刊》MAPS特刊的一部分。

Constraining the distribution of gas and dust in the inner 20 au of protoplanetary disks is difficult. At the same time, this region is thought to be responsible for most planet formation, especially around the water ice line at 3–10 au. Under the assumption that the gas is in a Keplerian disk, we use the exquisite sensitivity of the Molecules with ALMA at Planet-forming Scales (MAPS) ALMA large program to construct radial surface brightness profiles with a ∼3 au effective resolution for the CO isotopologue J = 2–1 lines using the line velocity profile. IM Lup reveals a central depression in 13CO and C18O that is ascribed to a pileup of ∼500 M ⊕ of dust in the inner 20 au, leading to a gas-to-dust ratio of around 10) and that the dust gap is gas-rich enough to have optically thick C18O. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement.

Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing Protoplanetary Disk Structure within 20 au

文献摘要

相似文献