Possible magnetic activity cycles in two solar-type overcontact binary stars: AD Cnc and FG Hya

Details Possible magnetic activity cycles in two solar-type overcontact binary stars: AD Cnc and FG Hya Possible magnetic activity cycles in two solar-type overcontact binary stars: AD Cnc and FG Hya

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...8e..17q&link_type=abstract

Solar and Stellar Activity Cycles, 26th meeting of the IAU, Joint Discussion 8, 17-18 August 2006, Prague, Czech Republic, JD08,

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Scientific paper

W UMa-type binary stars are overcontact systems where both components are filling the critical Roche lobes and sharing a common convictive envelope (CCE). This type of binaries offers a good chance to study the effects of the CCE on solar-type magnetic activity. Recently, two solar-type overcontact binaries, AD Cnc (Sp.=K0; P=0.2827 days) and FG Hya (Sp.=G0; P=0.3278 days), have been monitored for several years photometrically with the 1.0-m telescope in Yunnan Observatory. The light levels at both minima and both maxima in the light curves were found to be variable. An orbital period analysis of the two systems were done based on our new determined times of light minimum combined with the others compiled from the literature. After long-term period changes were removed, double cyclic period changes were discovered for the two binaries. The light curves of those sample stars have been analysed with the new version of the W-D method and the properties of dark spot on the photospheric surface were determined. The main results are as following. (1) For FG Hya, we found that both the orbital period and the depth of the primary minimum show a cyclic change with a period of 36.4 years and in the same phase. The variation of the light curve, the spotted primary component and the connection between the period change and the depth of the primary minimum all indicate that the G0-type primary component display solar-type magnetic activity cycle with a period of 36.4 years. (2) The long-term evolution of dark spot on the photospheric surface of the primary component is presented based on the analysis of the variation of the light curves. It is found that the dark spot activity may have a 17-year cycle, which is close to the period of one cyclic component of the period variations (16.2 years). This suggests that the primary component (K0-type star) may have a 17-year magnetic activity cycle.

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