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Double eclipsing binary system KIC 3832716

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In this paper we analyzed the light curve of the object KIC 3832716 observed during Kepler K1 mission. We showed that this previously known eclipsing binary is in fact quadruple system, in double eclipsing binary configuration on a long period orbit with the mass ratio of eclipsing binaries \(0.7 \pm 0.3\). The system consists of eclipsing binary A with the orbital period of \(P_{A} \sim 1.1419~\mbox{d}\). Eclipsing binary A contains larger but less luminous secondary component in the post main sequence stage of its evolution consistent with an “Algol paradox” which can explain parameters of the components by mass transfer from secondary component after leaving the main sequence. Inspection of the light curve and eclipse time variations of the eclipsing binary A also indicates the presence of spots on the surface of secondary component with 57 d period of activity probably induced by longitudinal motion of the spots. The second eclipsing binary B with orbital period \(P_{B} \sim 2.1703~\mbox{d}\) contains very dim secondary component with luminosity below \(0.09~L_{\odot}\).

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This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. This work was supported by the Slovak Research and Development Agency under the contract No. APVV-15-0458. The research of M.F. was supported by the internal grant No. VVGS-PF-2018-758 of the Faculty of Science, P.J. Šafárik University in Košice. The author would like to thank E. Paunzen and M. Lach for constructive criticism of the manuscript.

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Correspondence to M. Fedurco.

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Fedurco, M., Parimucha, Š. Double eclipsing binary system KIC 3832716. Astrophys Space Sci 363, 267 (2018).

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