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Magnetic Field in The Isolated Massive Dense Clump IRAS 20126+4104

Shinnaga, Hiroko and Novak, Giles and Vaillancourt, John E. and Machida, Masahiro N. and Kataoka, Akimasa and Tomisaka, Kohji and Davidson, Jacqueline A. and Phillips, Thomas G. and Dowell, C. Darren and Leeuw, Lerothodi and Houde, Martin (2012) Magnetic Field in The Isolated Massive Dense Clump IRAS 20126+4104. . (Submitted)

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We measured polarized dust emission at 350µm towards the high-mass star forming massive dense clump IRAS 20126+4104 using the SHARC II Polarimeter, SHARP, at the Caltech Submillimeter Observatory. Most of the observed magnetic field vectors agree well with magnetic field vectors obtained from a numerical simulation for the case when the global magnetic field lines are inclined with respect to the rotation axis of the dense clump. The results of the numerical simulation show that rotation plays an important role on the evolution of the massive dense clump and its magnetic field. The direction of the cold CO 1-0 bipolar outflow is parallel to the observed magnetic field within the dense clump as well as the global magnetic field, as inferred from optical polarimetry data, indicating that the magnetic field also plays a critical role in an early stage of massive star formation. The large-scale Keplerian disk of the massive (proto)star rotates in almost opposite sense to the clump's envelope. The observed magnetic field morphology and the counter-rotating feature of the massive dense clump system provide hints to constrain the role of magnetic fields in the process of high mass star formation.

Item Type:Report or Paper (Working Paper)
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URLURL TypeDescription
Novak, Giles0000-0003-1288-2656
Additional Information:This research has been supported by NSF grant AST-0540882 and AST-0838261 to the CSO. SHARP has been supported by NSF grants AST 02-41356, AST 05-05230, and AST-0909030 to Northwestern University and grant AST 05-05124 to the University of Chicago. Numerical computations were carried out on NEC SX-9 and the general-purpose PC farm at Center for Computational Astrophysics of National Astronomical Observatory of Japan. This work was supported by a Grants-in-Aid from MEXT (21740136, 21244021). Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. HS thanks Hua-bai Li, Roger Hildebrand, and Fumitaka Nakamura for helpful comments, and Shu-ichiro Inutsuka for valuable discussions. Facilities: CSO.
Funding AgencyGrant Number
NSFAST 02-41356
NSFAST 05-05230
NSFAST 05-05124
MEXT Grants-in-Aid21740136
MEXT Grants-in-Aid21244021
Subject Keywords:polarization — techniques: polarimetric — stars: formation — ISM: clouds — ISM: magnetic fields — submillimeter: ISM
Record Number:CaltechAUTHORS:20120409-085648496
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:30034
Deposited By: Tony Diaz
Deposited On:25 Apr 2012 17:39
Last Modified:09 Mar 2020 13:19

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