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Paper: B[e] Star CI Cam: Eighteen Years of Research
Volume: 508, The B[e] Phenomenom: Forty Years of Studies
Page: 307
Authors: Goranskij, V. P.; Barsukova, E. A.; Bjorkman, K. S.; Burenkov, A. N.; Klochkova, V. G.; Manset, N.; Metlova, N. V.; Miroshnichenko, A. S.; Panchuk, V. E.; Yushkin, M. V.; Zharikov, S. V.
Abstract: We present the results of extensive spectroscopic and photometric observations of CI Cam performed after its outburst in April 1998. The outburst was interpreted as a thermonuclear runaway of hydrogen on the surface of a white dwarf (WD). We detected variations of both the brightness and the He II 4686 Å line radial velocity with a period of 19d.400±0d.015 due to orbital motion of the WD. The rapid brightness variations on a timescale of hours is explained by pulsations of a B4 IIIV[e] star. In 2012, the system entered an active state with the stronger He II line and with the brightness increased by 0.4 mag. We observed a slow low-amplitude drift in the velocity of Fe II and [N II] emission lines which we explained by the orbital motion of the B[e] star + WD system along with all its gaseous environment around a third companion invisible in the spectra. The active phase of the B[e] star might have been initiated by a close approach of the binary and the third companion in 2007.
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