Magnetic activity, flares and asynchronous spot modulation, in the detached eclipsing binary KOI 6832

We present a photometric study of the poorly investigated eclipsing binary KOI 6832 using 1459.49 d of long cadence Kepler observations. The Wilson–Devinney light curve solution favours a detached configuration composed of two cool late type components. With T 1 = 4573 K fixed, the adopted solution gives T 2 = 4501 K, q = 0.92 , i = 87.47 ° , and mean fractional radii of 〈 r 1 〉 = 0.0374 and 〈 r 2 〉 = 0.0464 . The calibration dependent absolute parameters are M 1 = 0.71 M ⊙ , M 2 = 0.66 M ⊙ , R 1 = 0.61 R ⊙ , and R 2 = 0.76 R ⊙ , although radial velocities are required for dynamical values. The secondary eclipse occurs near phase 0.49; after adopting Δ E = 0.49 , no significant timing variation requiring apsidal motion or a light time effect is detected. The eclipse cleaned light curve shows a dominant modulation at ν 1 = 0.1355 d − 1 , corresponding to P rot = 7.3805 d, different from P orb = 6.490663 d and consistent with asynchronous or latitude dependent spot modulation. We detect 59 flares, with N 1 = 0.001684 h − 1 and N 2 = 9.190 × 1 0 − 6 . The OPEA model gives a Plateau value of 1.724 ± 0.1739 and a half time of 6853.42 s. We conclude that KOI 6832 is a magnetically active detached binary showing flare activity, spot modulation, and non-synchronous surface rotation.