Volume 607, November 2017
|Number of page(s)||6|
|Published online||15 November 2017|
ALMA discovery of a rotating SO/SO2 flow in HH212
A possible MHD disk wind?
1 LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Université, UPMC Univ. Paris 06, 75014 Paris, France
2 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
3 INAF, Osservatorio Astrofisico di Arceti, Largo E. Fermi 5, 50125 Firenze, Italy
4 Università degli Studi di Firenze, Dipartimento di Fisica e Astronomia, via G. Sansone 1, 50019 Sesto Fiorentino, Italy
5 Institut d’Astrophysique Spatiale, CNRS UMR 8617, Université Paris-Sud, 91405 Orsay, France
6 Institut de Radioastronomie Millimétrique, 38406 Saint-Martin d’ Hères, France
7 OASU/LAB-UMR5804, CNRS, Université Bordeaux, 33615 Pessac, France
Received: 1 August 2017
Accepted: 29 September 2017
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 ~ 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 C34S 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 ~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%.
Key words: stars: formation / ISM: jets and outflows / ISM: individual objects: HH212
© ESO, 2017
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