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Submillimeter Array Observations of Magnetic Fields in Star Forming Regions

Published online by Cambridge University Press:  27 April 2011

R. Rao ,
J.-M. Girart  and
D. P. Marrone
R. Rao
Affiliation:
Academia Sinica Institute of Astronomy & Astrophysics, Submillimeter Array, 645 N. Aohoku Place, Hilo, HI 96720, USA email: rrao@sma.hawaii.edu
J.-M. Girart
Affiliation:
Institut de Ciències de l'Espai (CSIC-IEEC), Campus UAB – Facultat de Ciències, Torre C5 - parell 2, 08193 Bellaterra, Catalunya, Spain
D. P. Marrone
Affiliation:
National Radio Astronomy Observatory & Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois, 60637, USA
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Abstract

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There have been a number of theoretical and computational models which state that magnetic fields play an important role in the process of star formation. Competing theories instead postulate that it is turbulence which is dominant and magnetic fields are weak. The recent installation of a polarimetry system at the Submillimeter Array (SMA) has enabled us to conduct observations that could potentially distinguish between the two theories. Some of the nearby low mass star forming regions show hour-glass shaped magnetic field structures that are consistent with theoretical models in which the magnetic field plays a dominant role. However, there are other similar regions where no significant polarization is detected. Future polarimetry observations made by the Submillimeter Array should be able to increase the sample of observed regions. These measurements will allow us to address observationally the important question of the role of magnetic fields and/or turbulence in the process of star formation.

Keywords

stars: formationISM: magnetic fieldsi ISM: dusttechniques: polarimetric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 103 - 106
Copyright
Copyright © International Astronomical Union 2011

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