EPIC 201160323

This faint star shows rapid apsidal motion. The period measured from the times of primary and secondary eclipse in the K2 light curve are $P_{\rm pri}
=22.272$d and $P_{\rm sec} = 22.300$d, respectively. We therefore included the rate of change of the longitude of periastron in the light curve model as a free parameter and hence obtained the value $\frac{d\omega}{dt} =
-0.10^{\circ} \pm 0.01^{\circ}$ per anomalistic period. This corresponds to an apsidal motion period of approximately 220 years if this rate is assumed to be constant.

![image](Figs/EPIC201160323_lcfit-eps-converted-to.pdf){width="99.00000%"}

Our best-fit model is shown in Fig. \[201160323\_lcfit\], where the drift in eclipse times relative to a single linear ephemeris calculated with the average period can be clearly seen. There are no nearby stars listed in the GAIA DR1 catalogue that might explain the large value for the third light parameter derived from the light curve analysis ($\ell_3 = 0.43 \pm 0.05$). This suggests that EPIC 201160323 is a triple or multiple star system in which the gravitational interaction between the eclipsing binary and an additional body or bodies is causing the rapid change in the orientation of its orbit.

This star is listed in the K2 Variable Catalogue as an 