1. Photometry and spectroscopy of CI camelpardalis from 1998–2005
- Author
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N. V. Metlova, E. A. Barsukova, V. G. Klochkova, V. P. Goranskii, A. N. Burenkov, and N. V. Borisov
- Subjects
Physics ,Astrophysics::High Energy Astrophysical Phenomena ,Astronomy ,Balmer series ,White dwarf ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Circumstellar envelope ,Orbital period ,Photometry (optics) ,symbols.namesake ,Amplitude ,Intermediate polar ,Space and Planetary Science ,symbols ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Emission spectrum ,Astrophysics::Galaxy Astrophysics - Abstract
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 A 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.
- Published
- 2006