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Is the Magnetic Field Preserved During Core Formation?

Published online by Cambridge University Press:  23 September 2016

Brenda C. Matthews ,
Shih-Ping Lai ,
Richard M. Crutcher  and
Christine D. Wilson
Brenda C. Matthews
Affiliation:
University of California at Berkeley, Radio Astronomy Laboratory, 601 Campbell Hall, Berkeley, CA, 94720, U.S.A.
Shih-Ping Lai
Affiliation:
University of Maryland, Department of Astronomy, College Park, MD, 20742, U.S.A.
Richard M. Crutcher
Affiliation:
University of Illinois, Department of Astronomy, 1002 West Green Street, Urbana, IL, 61801, U.S.A.
Christine D. Wilson
Affiliation:
McMaster University, Department of Physics & Astronomy, 1280 Main St. W., Hamilton, ON, L8S 4M1, Canada

Abstract

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We present recent JCMT and BIMA array polarimetry data of nearby star-forming regions in order to compare the core and cloud-scale magnetic field geometries in two regions of Orion. The similarity of the magnetic field geometry in these cores to that of their ambient clouds is contrasted with JCMT data toward the Barnard 1 dark cloud in Perseus, which reveal a different magnetic field orientation between the majority of the cores and the surrounding cloud; each of the cores exhibits a different mean polarization position angle. We conclude that the preservation of the magnetic field geometry is better in cores formed within clouds with ordered large scale structures. In Barnard 1, the cores may quickly exhibit a different polarization pattern if they have, for example, rotation which differs from the large scale cloud motions, or a weaker component of ordered fields. This could also explain why the cores exhibit such different geometries from each other in Barnard 1.

Type
Part 2: From Molecular Clouds to Protostellar Cores
Information
Symposium - International Astronomical Union , Volume 221: Star Formation at High Angular Resolution , 2004 , pp. 97 - 103
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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