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Paper: Study of theMagnetic Activity Cycles of CG Cygni
Volume: 370, Solar and Stellar Physics Through Eclipses
Page: 353
Authors: Tsantilas, S.; Rovithis-Livaniou, H.
Abstract: The RS CVn-type eclipsing binary CG Cyg is known to exhibit orbital period variations, which have been attributed to the light-time effect and/or to magnetic activity cycles. The latter seems to be more possible, as neither the spectroscopic data nor the periodogram of these variations confirmed the presence of a third body in the system. Thus, assuming that the observed period changes of CG Cyg are due only to the magnetic activity of its components, we find their magnetic field variation by applying the new method we proposed recently, (ASPC 335, 147, 2005). Our analysis shows that the magnetic field of the primary component of CG Cyg varies from 7 to 9.8 kG with a minimum around 1980, which coincides with the systemís maximum luminosity. On the other hand, and although the secondary star of CG Cyg is capable to sustain magnetic activity, this hypothesis requires a ΔL/L ≈ 0.2–0.8, which is 20 to 80 times larger than that predicted by magnetic activity. Thus, we conclude that the period modulation should probably assigned mostly to the magnetic activity of the primary component of CG Cygni.
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