Jae Woo Lee, Kyeongsoo Hong, Jae-Rim Koo, Jang-Ho Park
2016 Astrophysical Journal  
KIC 9532219 is a W UMa-type eclipsing binary with an orbital period of 0.1981549 d that is below the short-period limit (∼0.22 d) of the period distribution for contact binaries. The Kepler light curve of the system exhibits striking light changes in both eclipse depths and light maxima. Applying third-body and spot effects, the light-curve synthesis indicates that the eclipsing pair is currently in a marginal contact stage with a mass ratio of q=1.20, an orbital inclination of i=66.0 deg, a
more » ... perature difference of Δ (T_1--T_2)=172 K, and a third light of l_3=75.9 %. To understand the light variations with time, we divided up the light curve into 312 segments and separately analyzed them. The results reveal that variation of eclipse depth is primarily caused by changing amounts of contamination due to the nearby star KIC9532228 between the Kepler Quarters and that the variable O'Connell effect originates from the starspot activity on the less massive primary component. Based on our light-curve timings, a period study of KIC 9532219 indicates that the orbital period has varied as a combination of a downward parabola and a light-travel-time (LTT) effect due to a third body, with a period of 1196 d and a minimum mass of 0.0892 M_ in an eccentric orbit of 0.150. The parabolic variation could be a small part of a second LTT orbit due to a fourth component in a wider orbit, instead of either mass transfer or angular momentum loss.
doi:10.3847/0004-637x/820/1/1 fatcat:p2bpx4px2beqpnns2suu6rjta4