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The Ejection of Runaway Massive Binaries

Published online by Cambridge University Press:  12 July 2007

M. Virginia McSwain
Affiliation:
NSF Astronomy and Astrophysics Postdoctoral Fellow; Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520-8101, USA, email: mcswain@astro.yale.edu
Scott M. Ransom
Affiliation:
National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA, email: sransom@nrao.edu
Tabetha S. Boyajian
Affiliation:
Department of Physics and Astronomy, Georgia State University, P.O. Box 4106, Atlanta, GA 30302-4106, USA, email: tabetha@chara.gsu.edu, erika@chara.gsu.edu, gies@chara.gsu.edu
Erika D. Grundstrom
Affiliation:
Department of Physics and Astronomy, Georgia State University, P.O. Box 4106, Atlanta, GA 30302-4106, USA, email: tabetha@chara.gsu.edu, erika@chara.gsu.edu, gies@chara.gsu.edu
Mallory S.E. Roberts
Affiliation:
Eureka Scientific, Inc., 2452 Delmer Street Suite 100, Oakland, CA 94602-3017, USA, email: malloryr@gmail.com
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Abstract

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The runaway O-type stars HD 14633 and HD 15137 are both SB1 systems that were probably ejected from the open cluster NGC 654. Were these stars dynamically ejected by close gravitational encounters in the dense cluster, or did the binaries each receive a kick from a supernova in one member? We present new results from our investigation of the optical, X-ray, and radio properties of these binary systems to discuss the probable ejection scenarios. We argue that these binaries may have been ejected via dynamical interactions in the dense cluster environment.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2007

References

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