Long-period optical variability of the CYG X-1 system

Details Long-period optical variability of the CYG X-1 system Long-period optical variability of the CYG X-1 system

Apr 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987azh....64..326k&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 64, Mar.-Apr. 1987, p. 326-344. In Russian.

Astronomy and Astrophysics

Astronomy

9

Electrophotometry, Light Curve, Optical Properties, Periodic Variations, X Ray Binaries, Accretion Disks, Black Holes (Astronomy), Fourier Analysis, Orbital Elements

Scientific paper

Analysis of long-term photoelectric observations of V1357 Cyg = Cyg X-1 confirmed the long-period optical variation of this X-ray binary system with the period of 294d revealed by Kemp et al. (1983). This periodicity is most strongly pronounced at the orbital period phases, when the optical star is in front of the X-ray source. Variations of the mean level of Cyg X-1 and of the light curve form with the phase of the period 294d agree well with the model of a precessing accretion disc which radiates in the optical range mainly by scattering and processing of the optical star's radiation. The direction of the disc precession coincides with the one of the orbital motion, and it is hard to understand this fact in the models with forced precession. The triple system model is less probable. The supposed mass of the third body is 1 - 2 M_sun;.These results do not influence the conclusion on the large mass of the X-ray source and its identification with a black hole. The question about the presence of periods 39d or 78d in the brightness variations of Cyg X-1 remains open.

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