Hostname: page-component-848d4c4894-v5vhk Total loading time: 0 Render date: 2024-06-26T19:48:40.279Z Has data issue: false hasContentIssue false
  • English
  • Français

Investigation of X-ray transient CI Cam as an unique star with the B[e]phenomenon

Published online by Cambridge University Press:  12 July 2011

Elena A. Barsukova ,
Alexandr N. Burenkov ,
Valentina G. Klochkova ,
Vitalij P. Goranskij ,
Nataly V. Metlova ,
Peter Kroll  and
Anatoly S. Miroshnichenko
Elena A. Barsukova
Affiliation:
Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnij Arkhyz, Karachai-Cherkesia, 369167, Russia; email: bars@sao.ru, ban@sao.ru, valenta@sao.ru
Alexandr N. Burenkov
Affiliation:
Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnij Arkhyz, Karachai-Cherkesia, 369167, Russia; email: bars@sao.ru, ban@sao.ru, valenta@sao.ru
Valentina G. Klochkova
Affiliation:
Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnij Arkhyz, Karachai-Cherkesia, 369167, Russia; email: bars@sao.ru, ban@sao.ru, valenta@sao.ru
Vitalij P. Goranskij
Affiliation:
Sternberg Astronomical Institute, Moscow University, Universitetskii pr. 13, Moscow, 119991, Russia; email: goray@sai.msu.ru, nm@sai.crimea.ua
Nataly V. Metlova
Affiliation:
Sternberg Astronomical Institute, Moscow University, Universitetskii pr. 13, Moscow, 119991, Russia; email: goray@sai.msu.ru, nm@sai.crimea.ua
Peter Kroll
Affiliation:
Sternwarte Sonneberg, Sternwartestrasse, 32, Sonneberg, D-96515, Germany email: pk@4pisysteme.de
Anatoly S. Miroshnichenko
Affiliation:
University of North Carolina at Greensboro, USA; email: a_mirosh@uncg.edu
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.

Double mode pulsations of the B4 component in the system of CI Cam were detected. The photometric 19.4 day orbital period of CI Cam was confirmed with the plates of the Sonneberg collection for a long period of time before the unique 1998 outburst. The amplitude of the periodic component of 0.08 mag before the outburst was larger than that of 0.03 mag after the outburst.

Keywords

binaries: generalnovaecataclysmic variablesstars: oscillations (including pulsations)circumstellar matter
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. 602 - 603
Copyright
Copyright © International Astronomical Union 2011

References

De Cat, P. 2002, in: Aerts, C., Bedding, T. R., & Christensen-Dalsgaard, J. (eds.), IAU Colloq. 185: Radial and Nonradial Pulsationsn as Probes of Stellar Physics, ASP-CS 259, p. 196Google Scholar
Barsukova, E. A., Borisov, N. V., Burenkov, A. N., Goranskii, V. P. et al. 2006, Astron. Rep., 50, 664Google Scholar
Barsukova, E.A., Klochkova, V.G., Panchuk, V.E., Yushkin, M. V. et al. 2007, ATel, 1036Google Scholar
Goranskij, V. P. & Barsukova, E. A. 2009, Astrophysical Bulletin, 64, 50Google Scholar