engleski

Toward a model of the strongly interacting binary w crucis with genetic algorithm

The long-period eclipsing binary W Crucis belongs to a rare group of the strongly interacting binaries of the W Serpentis class. It is belived that these binaries to which famous Beta Lyrae also belongs, is in the phase of rapid mass transfer between the components. In spite of its long period of about 200 days it attracked skilled photometrists and a several sets of light-curves of W Crucis have been published in the last decade including Stroemgren photometry in the Long-Term Photometry of Variables Project at ESO. We modelled this interacting binary system with a computer code that incorporates the influence of an accretion disk which surrounds a mass-gaining component. Genetic algorithm searches paramter space using the simplified version of the biological evolutionary process. We obtain a new mass ratio for the system of 0.13 and inclination close to 88 deg. The masses for the invisible afn a giant (mass-losing) star estimated at 7.5 and 1.0 Msun, respectively. We would also present radiative and geometrical properties of its accretion disk which has completely hidden massive component, and compare our optimal parameters with Zola results which are based on another code and another optimization procedure.

interacting binary stars; accretion disk; genetic algorithm

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