Photometric Modelling of Close Binary Star CN And

Details Photometric Modelling of Close Binary Star CN And Photometric Modelling of Close Binary Star CN And

Mar 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006japa...27...47j&link_type=abstract

Journal of Astrophysics and Astronomy, Vol. 27, Issue 1, p.47

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

The results of two color photometry of active close binary CN And are presented and analyzed. The light curves of the system are obviously asymmetric, with the primary maximum brighter than the sec-ondary maximum, which is known as the O'Conell effect. The most plau-sible explanation of the asymmetry is expected to be due to spot activity of the primary component. For the determination of physical and geometrical parameters, the most new version of W--D code was used, but the presence of asymmetry prevented the convergence of the method when the whole light curves were used. The solutions were obtained by applying mode 3 of W--D code to the first half of the light curves, assuming synchronous rota-tion and zero eccentricity. Absolute parameters of the system were obtained from combining the photometric solution with spectroscopic data obtained from radial velocity curve analysis. The results indicate the poor thermal contact of the components and transit primary minimum. Finally the O--C diagram was analyzed. It was found that the orbital period of the system is changing with a rate of dP/dt =-2 2 6-10??? 10 which corresponds to mass transfer from more massive component to less massive with the rate of dM/dt ?4 82-10??? 8 M sun year.

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