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Massive Star Formation: Radiation Transfer Modeling and Multiwavelength Observation

Published online by Cambridge University Press:  21 March 2013

Yichen Zhang ,
Jonathan Tan ,
Chris McKee  and
James De Buizer
Yichen Zhang
Affiliation:
Department of Astronomy, University of Florida, Gainesville, Florida 32611, USA email: yczhang@astro.ufl.edu
Jonathan Tan
Affiliation:
Department of Astronomy, University of Florida, Gainesville, Florida 32611, USA email: yczhang@astro.ufl.edu Departments of Physics, University of Florida, Gainesville, Florida 32611, USA
Chris McKee
Affiliation:
Departments of Astronomy & Astrophysics and Physics, University of California, Berkeley, California 94720, USA
James De Buizer
Affiliation:
SOFIA-USRA, NASA Ames Research Center, MSN211-3, Moffett Field, CA94035, USA
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Abstract

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We present a radiation transfer model consistently developed for a core in high pressure environment forming a massive star through core accretion. We compare this model to the massive protostar G35.2-0.74N, including SOFIA observations at 30 and 40μm. Good agreement is achieved, showing that a ~30M⊙ protostar is forming from a high surface density core via relatively ordered collapse and accretion, driving powerful outflows. This result supports the Core Accretion theory which predicts that massive stars form similarly to low-mass stars.

Keywords

stars: formation — ISM: clouds — ISM: jets and outflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S292: Molecular Gas, Dust, and Star Formation in Galaxies , August 2012 , pp. 67
Copyright
Copyright © International Astronomical Union 2013

References

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Zhang, Y. & Tan, J. C., 2011, ApJ, 733, 55CrossRefGoogle Scholar
Zhang, Y., Tan, J. C., & McKee, C. F., 2012, ApJ, submittedGoogle Scholar