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Massive Star Formation: Radiation Transfer Modeling and Multiwavelength Observation

Published online by Cambridge University Press:  21 March 2013

Yichen Zhang
Affiliation:
Department of Astronomy, University of Florida, Gainesville, Florida 32611, USA email: [email protected]
Jonathan Tan
Affiliation:
Department of Astronomy, University of Florida, Gainesville, Florida 32611, USA email: [email protected] 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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013

References

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