Optical light curves and masses of X-ray binaries

Details Optical light curves and masses of X-ray binaries Optical light curves and masses of X-ray binaries

Oct 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975nyasa.262..376a&link_type=abstract

(AAS, American Physical Society, and New York Academy of Sciences, Texas Symposium on Relativistic Astrophysics, 7th, Dallas, Te

Astronomy and Astrophysics

Astronomy

Binary Stars, Light Curve, Stellar Mass, X Ray Astronomy, X Ray Binaries, X Ray Stars, Astronomical Models, B Stars, Eclipses, Heating, Main Sequence Stars, Mass Ratios, O Stars

Scientific paper

The optical light curves of three X-ray binaries were analyzed to determine the possible range of masses of their components. The primary was allowed to be in its Roche mode. Heating effects and uncertainties in the data were considered, and departures from corotation were investigated. The analysis of Cyg X-1-HdE 226868 showed that the optical data cannot distinguish between a black hole and a normal OB main-sequence star. If the secondary is a black hole, its mass is not less than 9 solar masses and the ellipsoidal variations of the primary are the only contribution to the optical light curve. The mass is the same if it is an OB main-sequence star, but the light curve has contributions from the ellipsoidal variations of both stars and the two reflection effects. The inclusion of heating effects in the analysis of SMC X-1-SK 160 reduces the derived mass ratio to a value consistent with the radial velocity; values of the mass ratio derived with tidal lobe geometry differ by 20% from those derived with Roche geometry. In the case of CEN X-3 Krzeminski's star, the constraints imposed on the mass of the secondary from the light curve and eclipse duration were investigated.

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