Please use this identifier to cite or link to this item:
|Title:||Velocity and magnetic fields within 1000 AU of a massive YSO||Authors:||SANNA, ALBERTO
Vlemmings, W. H. T.
Caratti o Garatti, A.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||583||First Page:||L3||Abstract:||<BR /> Aims: We study the velocity and magnetic field morphology in the vicinity (<1000 AU) of a massive young stellar object (YSO) at very high spatial resolution (10-100 AU). <BR /> Methods: We performed milliarcsecond polarimetric observations of the strong CH<SUB>3</SUB>OH maser emission observed in the vicinity of an O-type YSO in G023.01-00.41. We combined this information with the velocity field of the CH<SUB>3</SUB>OH masing gas previously measured at the same angular resolution. We analyzed the velocity and magnetic fields in the reference system defined by the direction of the molecular outflow and the equatorial plane of the hot molecular core at its base, as recently observed on subarcsecond scales. <BR /> Results: We provide a first detailed picture of the gas dynamics and magnetic field configuration within a radius of 2000 AU of a massive YSO. We have been able to reproduce the magnetic field lines for the outer regions (>600 AU) of the molecular envelope, where the magnetic field orientation shows a smooth change with the maser cloudlets position (0.2° AU<SUP>-1</SUP>). Overall, the velocity field vectors accommodate the local magnetic field direction well, but still show an average misalignment of 30°. We interpret this finding as the contribution of a turbulent velocity field of about 3.5 km s<SUP>-1</SUP>, which would be responsible for breaking up the alignment between the velocity and magnetic field vectors. We do resolve different gas flows that develop both along the outflow axis and across the disk plane and that have an average speed of 7 km s<SUP>-1</SUP>. In the direction of the outflow axis, we establish a collimation of the gas flow at a distance of about 1000 AU from the disk plane. In the disk region, gas appears to stream outward along the disk plane for radii greater than 500-600 AU and inward for shorter radii. <P />Table 1 is available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201526806/olm">http://www.aanda.org</A>||Acknowledgments:||Financial support by the Deutsche Forschungsgemeinschaft (DFG) Priority Program 1573 is gratefully acknowledged. W.V. acknowledges financial support from the European Research Council through ERC consolidator grant 614264. A.C.G. was supported by the Science Foundation of Ireland, grant 13/ERC/I2907. A.S. thanks S. Leurini for helpful discussions in preparation.||URI:||http://hdl.handle.net/20.500.12386/23267||URL:||https://www.aanda.org/articles/aa/abs/2015/11/aa26806-15/aa26806-15.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201526806||Bibcode ADS:||2015A&A...583L...3S||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
Show full item record
checked on Sep 24, 2020
checked on Sep 24, 2020
Items in DSpace are published in Open Access, unless otherwise indicated.