A 100 au Wide Bipolar Rotating Shell Emanating from the HH 212 Protostellar Disk: A Disk Wind?

HH 212 is a Class 0 protostellar system found to host a "hamburger"-shaped dusty disk with a rotating disk atmosphere and a collimated SiO jet at a distance of ∼400 pc. Recently, a compact rotating outflow has been detected in SO and SO2 toward the center along the jet axis at ∼52 au (0 13...

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Bibliographic Details
Published in:The Astrophysical journal 2018-03, Vol.856 (1), p.14
Main Authors: Lee, Chin-Fei, Li, Zhi-Yun, Codella, Claudio, Ho, Paul T. P., Podio, Linda, Hirano, Naomi, Shang, Hsien, Turner, Neal J., Zhang, Qizhou
Format: Article
Language:English
Subjects:
accretion, accretion disks
Angular momentum
Astrophysics
Atmosphere
Atmospheric models
Collimation
ISM: individual objects (HH 212)
ISM: jets and outflows
Kinematics
Outflow
Protostars
Rotating disks
Rotation
stars: formation
Sulfur dioxide
Wind
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Summary:HH 212 is a Class 0 protostellar system found to host a "hamburger"-shaped dusty disk with a rotating disk atmosphere and a collimated SiO jet at a distance of ∼400 pc. Recently, a compact rotating outflow has been detected in SO and SO2 toward the center along the jet axis at ∼52 au (0 13) resolution. Here we resolve the compact outflow into a small-scale wide-opening rotating outflow shell and a collimated jet, with the observations in the same S-bearing molecules at ∼16 au (0 04) resolution. The collimated jet is aligned with the SiO jet, tracing the shock interactions in the jet. The wide-opening outflow shell is seen extending out from the inner disk around the SiO jet and has a width of ∼100 au. It is not only expanding away from the center, but also rotating around the jet axis. The specific angular momentum of the outflow shell is ∼40 au km s−1. Simple modeling of the observed kinematics suggests that the rotating outflow shell can trace either a disk wind or disk material pushed away by an unseen wind from the inner disk or protostar. We also resolve the disk atmosphere in the same S-bearing molecules, confirming the Keplerian rotation there.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aaae6d