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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 03981naa a2200529 4500 | |
| 001 | oai:research.chalmers.se:55432fb7-5cf8-451f-bea7-44820e0beca5 | |
| 003 | SwePub | |
| 008 | 171007s2012 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://doi.org/10.1051/0004-6361/2011187102 DOI |
| 024 | 7 | a https://research.chalmers.se/publication/1628692 URI |
| 040 | a (SwePub)cth | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a art2 swepub-publicationtype |
| 072 | 7 | a ref2 swepub-contenttype |
| 100 | 1 | a Alves, F. O.u Universität Bonn,University of Bonn4 aut |
| 245 | 1 0 | a The magnetic field of IRAS 16293-2422 as traced by shock-induced H2O masers |
| 264 | c 2012-05-25 | |
| 264 | 1 | b EDP Sciences,c 2012 |
| 338 | a electronic2 rdacarrier | |
| 520 | a Context. Shock-induced H2O masers are important magnetic field tracers of very high density gas. Water masers are found in both high-and low-mass star-forming regions, and are a powerful tool for comparing magnetic field morphologies in both mass regimes. Aims. We present one of the first magnetic field determinations for the low-mass protostellar core IRAS 16293-2422 at volume densities as high as 10(8-10) cm(-3). Our goal is to determine wether the collapsing regime of this source is controlled by magnetic fields or other factors such as turbulence. Methods. We used the Very Large Array (VLA) to carry out spectropolarimetric observations of the 22 GHz Zeeman emission from H2O masers. From the Stokes V line profile, we are then able to estimate the magnetic field strength in the dense regions around the protostar. Results. A blend of at least three maser features can be inferred from our relatively high spatial resolution data set (similar to 0.1 ''), which is reproduced as a clear non-Gaussian line profile. The emission is very stable in terms of polarization fraction and position angle across the channels. The maser spots are aligned with some components of the complex outflow configuration of IRAS 16293-2422, and are excited in zones of compressed gas produced by shocks. The post-shock particle density is in the range of 1-3 x 10(9) cm(-3), consistent with typical water-maser pumping densities. Zeeman emission is produced by a very strong line-of-sight magnetic field (B similar to 113 mG). Conclusions. The magnetic field pressure derived from our data is comparable to the ram pressure of the outflow dynamics. This indicates that the magnetic field is energetically important to the dynamical evolution of IRAS 16293-2422. | |
| 650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
| 653 | a stars: formation | |
| 653 | a ISM: individual objects: IRAS 16293-2422 | |
| 653 | a water masers | |
| 653 | a polarization | |
| 653 | a submillimeter array | |
| 653 | a iras-16293-2422 | |
| 653 | a ISM: magnetic fields | |
| 653 | a kinematics | |
| 653 | a polarization | |
| 653 | a masers | |
| 653 | a dark clouds | |
| 653 | a low-mass stars | |
| 653 | a hot core | |
| 653 | a infrared polarimetry | |
| 653 | a star-forming regions | |
| 700 | 1 | a Vlemmings, Wouter,d 1974u Chalmers tekniska högskola,Chalmers University of Technology4 aut0 (Swepub:cth)wouterv |
| 700 | 1 | a Girart, J. M.u Universitat Autonoma de Barcelona (UAB)4 aut |
| 700 | 1 | a Torrelles, J. M.u Universitat de Barcelona,University of Barcelona4 aut |
| 710 | 2 | a Universität Bonnb Chalmers tekniska högskola4 org |
| 773 | 0 | t Astronomy and Astrophysicsd : EDP Sciencesg 542q 542x 0004-6361x 1432-0746 |
| 856 | 4 | u http://publications.lib.chalmers.se/records/fulltext/162869/local_162869.pdfx primaryx freey FULLTEXT |
| 856 | 4 | u https://www.aanda.org/articles/aa/pdf/2012/06/aa18710-11.pdf |
| 856 | 4 8 | u https://doi.org/10.1051/0004-6361/201118710 |
| 856 | 4 8 | u https://research.chalmers.se/publication/162869 |
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