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Accretion Flows in High-Mass Star Formation

Published online by Cambridge University Press:  12 April 2016

Eric Keto
Eric Keto*
Affiliation:
Lawrence Livermore National Laboratory Institute of Geophysics and Planetary Physics

Abstract

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We compare observed and simulated images of the accretion flows associated with high mass star formation in the regions G10.6-0.4 and DR21. We describe, as a result of the comparison, the temperature, density, and velocity fields. Our results indicate that the G10.6-0.4 cloud core is strongly condensed and has approximately equal velocities in rotation and infall at its current evolutionary state. The rapid collapse and lack of rotational support suggests that significant angular momentum transfer is occuring over scales at least as large as those observed (0.5 pc). A milligauss magnetic field would have sufficient energy to supply the required braking torque of 1047 ergs. The DR21 core shows approximately spherically symmetric radial accretion with no detectable rotation. Unlike the G10.6-0.4 core, the DR21 core does not contain an embedded HII region. Thus this core may represent a molecular cloud condensation undergoing gravitational collapse and accretion just prior to the formation of massive stars.

Type
I. Molecular Clouds, Star Formation And HII Regions
Information
International Astronomical Union Colloquium , Volume 120: Structure and Dynamics of the Interstellar Medium , 1989 , pp. 122 - 127
Copyright
Copyright © Springer-Verlag 1989

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