Discovery of Line Pressure Broadening and Direct Constraint on Gas Surface Density in a Protoplanetary Disk

The gas surface density profile of protoplanetary disks is one of the most fundamental physical properties to understanding planet formation. However, it is challenging to determine the surface density profile observationally, because the H 2 emission cannot be observed in low-temperature regions. W...

Full description

Saved in:
Bibliographic Details
Published in:Astrophysical journal. Letters 2022-09, Vol.937 (1), p.L14
Main Authors: Yoshida, Tomohiro C., Nomura, Hideko, Tsukagoshi, Takashi, Furuya, Kenji, Ueda, Takahiro
Format: Article
Language:English
Subjects:
Accretion disks
Astrochemistry
Carbon monoxide
Emission analysis
Extrasolar planets
Gas density
Gas giant planets
Jupiter
Low temperature
Magnetic fields
Physical properties
Planet formation
Planets
Pressure broadening
Protoplanetary disks
Radio telescopes
Snow line
Temperature regions
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:The gas surface density profile of protoplanetary disks is one of the most fundamental physical properties to understanding planet formation. However, it is challenging to determine the surface density profile observationally, because the H 2 emission cannot be observed in low-temperature regions. We analyzed the Atacama Large Millimeter/submillimeter Array (ALMA) archival data of the 12 CO J = 3 − 2 line toward the protoplanetary disk around TW Hya and discovered extremely broad line wings due to the pressure broadening. In conjunction with a previously reported optically thin CO isotopologue line, the pressure broadened line wings enabled us to directly determine the midplane gas density for the first time. The gas surface density at ∼5 au from the central star reaches ∼10 3 g cm −2 , which suggests that the inner region of the disk has enough mass to form a Jupiter-mass planet. Additionally, the gas surface density drops at the inner cavity by ∼2 orders of magnitude compared to outside the cavity. We also found a low CO abundance of ∼10 −6 with respect to H 2 , even inside the CO snow line, which suggests conversion of CO to less volatile species. Combining our results with previous studies, the gas surface density jumps at r ∼ 20 au, suggesting that the inner region (3 < r < 20 au) might be the magnetorotational instability dead zone. This study sheds light on the direct gas surface density constraint without assuming the CO/H 2 ratio using ALMA.
ISSN:2041-8205
2041-8213
DOI:10.3847/2041-8213/ac903a