Magnetic field structure in the Flattened Envelope and Jet in the young protostellar system HH 211

Abstract

HH 211 is a young Class 0 protostellar system, with a flattened envelope, a possible rotating disk, and a collimated jet. We have mapped it with the Submillimeter Array in 341.6 GHz continuum and SiO J=8-7 at ~ 0.6 resolution. The continuum traces the thermal dust emission in the flattened envelope and the possible disk. Linear polarization is detected in the continuum in the flattened envelope. The field lines implied from the polarization have different orientations, but they are not incompatible with current gravitational collapse models, which predict different orientation depending on the region/distance. Also, we might have detected for the first time polarized SiO line emission in the jet due to the Goldreich-Kylafis effect. Observations at higher sensitivity are needed to determine the field morphology in the jet.

5 pages, 2 figures

References in corpus (3)

• Magnetic Fields in the Formation of Sun-Like Stars
• A Magnetized Jet from a Massive Protostar
• Submillimeter arcsecond-resolution mapping of the highly collimated protostellar jet HH 211

Cited by in corpus (4)

• Interferometric observations of magnetic fields in forming stars
• Jet Motion, Internal Working Surfaces, and Nested Shells in the Protostellar System HH 212
• A Pseudodisk Threaded with a Toroidal and Pinched Poloidal Magnetic Field Morphology in the HH 211 Protostellar System
• Low Level Carbon Monoxide Line Polarization in two Protoplanetary Disks: HD 142527 and IM Lup