Astronomy Reports

, Volume 50, Issue 8, pp 664–678 | Cite as

Photometry and spectroscopy of CI camelpardalis from 1998–2005

  • E. A. Barsukova
  • N. V. Borisov
  • A. N. Burenkov
  • V. P. Goranskii
  • V. G. Klochkova
  • N. V. Metlova


Our long-time monitoring of the B[e] star and transient X-ray source CI Cam during quiescence following the 1998 outburst demonstrates that the complex, stratified circumstellar envelope has tended to stabilize after this structure was perturbed by the passage of a shock wave from the outburst. The star’s U BV R brightness shows slow, possibly cyclic, variations with an amplitude of about 0.2m. We determined the spectral type of the primary, B4III-V, based on the widths of the absorption wings of high-numbered Balmer lines. A Doppler shift of 460 km/s was detected for the Hell λ4686 Å emission line. The shifts in this line yield an orbital period of 19.41 days, which is also manifested itself in the photometric data as a wave with a V amplitude of 0.034m. The orbit is elliptical, with an eccentricity of 0.62. It is most likely that the secondary is a white dwarf surrounded by an accretion disk. The primary’s mass exceeds 12 M . The system may be at a late stage of its evolution, after the stage of mass exchange.

PACS numbers

97.30.Eh 97.80.Jp 


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Copyright information

© Pleiades Publishing, Inc. 2006

Authors and Affiliations

  • E. A. Barsukova
    • 1
  • N. V. Borisov
    • 1
  • A. N. Burenkov
    • 1
  • V. P. Goranskii
    • 2
  • V. G. Klochkova
    • 1
  • N. V. Metlova
    • 2
  1. 1.Special Astrophysical ObservatoryRussian Academy of SciencesKarachaĭ-Cherkessian RepublicRussia
  2. 2.Steinberg Astronomical InstituteMoscowRussia

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