Hostname: page-component-76fb5796d-zzh7m Total loading time: 0 Render date: 2024-04-25T16:42:05.548Z Has data issue: false hasContentIssue false
  • English
  • Français

Interaction between the Be star and the compact companion in TeV γ-ray binaries

Published online by Cambridge University Press:  12 July 2011

Atsuo T. Okazaki ,
Shigehiro Nagataki ,
Tsuguya Naito ,
Akiko Kawachi ,
Kimitake Hayasaki ,
Stanley P. Owocki  and
Jumpei Takata
Atsuo T. Okazaki
Affiliation:
Faculty of Engineering, Hokkai-Gakuen University, Toyohira-ku, Sapporo 062-8605, Japan email: okazaki@elsa.hokkai-s-u.ac.jp
Shigehiro Nagataki
Affiliation:
Yukawa Institute for Theoretical Physics, Sakyo-ku, Kyoto 606-8502, Japan email: nagataki@yukawa.kyoto-u.ac.jp
Tsuguya Naito
Affiliation:
Faculty of Management Information, Yamanashi Gakuin University, Kofu, Yamanashi 400-8575, Japan email: tsuguya@ygu.ac.jp
Akiko Kawachi
Affiliation:
Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan email: kawachi@icrr.u-tokyo.ac.jp
Kimitake Hayasaki
Affiliation:
Department Astronomy, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan email: kimi@kusastro.kyoto-u.ac.jp
Stanley P. Owocki
Affiliation:
Bartol Research Institute, University of Delaware, Newark, DE 19716, USA email: owocki@bartol.udel.edu
Jumpei Takata
Affiliation:
Department of Physics, University of Hong Kong, Pokfulam Road, Hong Kong, China email: takata@hku.hk
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We report on the results from 3-D SPH simulations of TeV binaries with Be stars. Since there is only one TeV binary (B 1259-63) where the nature of the compact companion has been established, we mainly focus on this Be-pulsar system. From simulations of B 1259-63 around periastron, we find that the pulsar wind dominates the Be-star wind and strips off an outer part of the Be-star disk, causing a strongly asymmetric, phase-dependent structure of the circumstellar material around the Be star. Such a large modulation may be detected by optical, IR, and/or UV observations at phases near periastron. We also discuss the results from simulations of another TeV binary LS I+61 303, for which the nature of the compact object is not yet known.

Keywords

gamma rays: theorystars: emission-lineBestars: windsoutflowsstars: individual (B 1259-63, LS I+61 303)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 628 - 629
Copyright
Copyright © International Astronomical Union 2011

References

Dubus, G. 2006, A&A, 456, 801Google Scholar
Romero, G. E., Okazaki, A. T., Orellana, M., & Owocki, S. P. 2007, A&A, 474, 15Google Scholar