By Alvaro Giménez; et al
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Extra info for Close binaries in the 21st century : new opportunities and challenges
3 × 10−13 ) × E 2 . Figure 1a shows the O–C diagram constructed with the light elements given above; it is clear that V839 Oph has an increasing period which can be explained with a mass exchange/loss mechanism in the system. 44 × 10−12 ) day/cycle. 86 × 10−7 M yr−1 . Residuals from the parabolic ﬁt indicates a continuous oscillatory behaviour covering three minima and three maxima. The visual timings in general show a large amount of scatter and not considered during the further anal- ysis. The cyclic variation could be produced by the light-time effect due to a third body in the system or magnetic activity cycle of the primary component.
0010M . 022 M . 014. For magnetic activity cycle we used the amplitude and period of the cyclic variation and calculated the concerning parameters with Applegate (1992)’s formulation as in Table 1 assuming that the primary component is the active one. 1 rd Springer Astrophys Space Sci (2006) 304:33–35 3. Conclusions An O–C analysis for V839 Oph based on all available eclipse timings together with newly determined ones is presented. The orbital period of the binary star shows cyclic variation superimposed on a quadratic variation.
ACT 2611, Australia 2. Results from the light curve modelling S. Zola ( ) Astronomical Observatory of the Jagiellonian University, ul. Orla 171, 30-244 Cracow, Poland; Mt. Suhora Observatory, Pedagogical University, ul. Podchorazych 2, 30-084 Cracow, Poland In order to obtain the physical parameters of each system we used the W-D code (Wilson, 1979) supplemented with the Monte Carlo search procedure. The theoretical values of both albedo and gravity darkening coefﬁcients were used. Keywords Binaries: eclipsing, Binaries: close, Binaries: contact, Stars: Fundamental parameters 1.
Close binaries in the 21st century : new opportunities and challenges by Alvaro Giménez; et al