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阿塔卡马大型毫米/亚毫米波阵列（ALMA）对HL Tau星系盘内天文单位区域水的观测结果。

Resolved ALMA observations of water in the inner astronomical units of the HL Tau disk.

作者信息

Facchini Stefano, Testi Leonardo, Humphreys Elizabeth, Vander Donckt Mathieu, Isella Andrea, Wrzosek Ramon, Baudry Alain, Gray Malcom D, Richards Anita M S, Vlemmings Wouter

机构信息

Dipartimento di Fisica, Università degli Studi di Milano, Milano, Italy.

Dipartimento di Fisica e Astronomia 'Augusto Righi', Università di Bologna, Bologna, Italy.

出版信息

Nat Astron. 2024;8(5):587-595. doi: 10.1038/s41550-024-02207-w. Epub 2024 Feb 29.

DOI:10.1038/s41550-024-02207-w
PMID:39282476
原文链接:https://pmc.ncbi.nlm.nih.gov/articles/PMC11399093/
Abstract

The water molecule is a key ingredient in the formation of planetary systems, with the water snowline being a favourable location for the growth of massive planetary cores. Here we present Atacama Large Millimeter/submillimeter Array data of the ringed protoplanetary disk orbiting the young star HL Tauri that show centrally peaked, bright emission arising from three distinct transitions of the main water isotopologue ( ). The spatially and spectrally resolved water content probes gas in a thermal range down to the water sublimation temperature. Our analysis implies a stringent lower limit of 3.7 Earth oceans of water vapour available within the inner 17 astronomical units of the system. We show that our observations are limited to probing the water content in the atmosphere of the disk, due to the high dust column density and absorption, and indicate that the main water isotopologue is the best tracer to spatially resolve water vapour in protoplanetary disks.

摘要

水分子是行星系统形成的关键要素，水雪线是巨大行星核心生长的有利位置。在此，我们展示了阿塔卡马大型毫米波/亚毫米波阵列对环绕年轻恒星HL Tau的环状原行星盘的观测数据，这些数据显示，主要水同位素分子（ ）的三个不同跃迁产生了中心峰值明亮发射。空间和光谱分辨的水含量探测了直至水升华温度的热范围内的气体。我们的分析表明，在该系统内17天文单位的范围内，水蒸气的下限严格为3.7个地球海洋的水量。我们表明，由于高尘埃柱密度和吸收，我们的观测仅限于探测盘大气层中的水含量，并指出主要水同位素分子是在原行星盘中对水蒸气进行空间分辨的最佳示踪剂。

https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/86f836d23d85/41550_2024_2207_Fig8_ESM.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/977aaf0a0b20/41550_2024_2207_Fig1_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/a69fdd2e41c1/41550_2024_2207_Fig2_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/869b803614a5/41550_2024_2207_Fig3_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/b09e7178448c/41550_2024_2207_Fig4_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/a76336c2b43e/41550_2024_2207_Fig5_ESM.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/22fbb735bf74/41550_2024_2207_Fig6_ESM.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/d0704154e819/41550_2024_2207_Fig7_ESM.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/86f836d23d85/41550_2024_2207_Fig8_ESM.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/977aaf0a0b20/41550_2024_2207_Fig1_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/a69fdd2e41c1/41550_2024_2207_Fig2_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/869b803614a5/41550_2024_2207_Fig3_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/b09e7178448c/41550_2024_2207_Fig4_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/a76336c2b43e/41550_2024_2207_Fig5_ESM.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/22fbb735bf74/41550_2024_2207_Fig6_ESM.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/d0704154e819/41550_2024_2207_Fig7_ESM.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/b2cb/11399093/86f836d23d85/41550_2024_2207_Fig8_ESM.jpg

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