MAGNETIC FIELD STRUCTURE IN THE FLATTENED ENVELOPE AND JET IN THE YOUNG PROTOSTELLAR SYSTEM HH 211

Journal Article · Wed Dec 10 00:00:00 EST 2014 · Astrophysical Journal Letters

DOI:https://doi.org/10.1088/2041-8205/797/1/L9· OSTI ID:22364875

Lee, Chin-Fei; Rao, Ramprasad; Hirano, Naomi; Ho, Paul T. P.; Hwang, Hsiang-Chih ^[1]; Ching, Tao-Chung; Lai, Shih-Ping ^[2]

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1. Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 106, Taiwan (China)
2. Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu 30013, Taiwan (China)

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 the 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 a 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.

• OSTI ID: 22364875
• Journal Information: Astrophysical Journal Letters, Vol. 797, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
COSMIC DUST
EMISSION SPECTRA
GHZ RANGE
GRAVITATIONAL COLLAPSE
JETS
MAGNETIC FIELDS
MORPHOLOGY
ORIENTATION
POLARIZATION
PROTOSTARS
SENSITIVITY
SILICON OXIDES
STARS