期刊
ASTRONOMY & ASTROPHYSICS
卷 607, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201731691
关键词
stars: formation; ISM: jets and outflows; ISM: individual objects: HH212
资金
- Programme National Physique et Chimie du Milieu Interstellaire (PCMI) of CNRS/INSU
- INC/INP
- CNES
- Conseil Scientifique of Observatoire de Paris
We wish to constrain the possible contribution of a magnetohydrodynamic disk wind (DW) to the HH212 molecular jet. We mapped the flow base with ALMA Cycle 4 at 0 ''.13 similar to 60 au resolution and compared these observations with synthetic DW predictions. We identified, in SO/SO2, a rotating flow that is wider and slower than the axial SiO jet. The broad outflow cavity seen in (CS)-S-34 is not carved by a fast wide-angle wind but by this slower agent. Rotation signatures may be fitted by a DW of a moderate lever arm launched out to similar to 40 au with SiO tracing dust-free streamlines from 0.05-0.3 au. Such a DW could limit the core-to-star efficiency to <= 50%.
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