2017MNRAS.469L.118J

We present the analysis of 29.77 d of K2 space photometry of the well-detached massive 4.6 d O+B binary HD 165246 (V = 7.6) obtained during Campaign 9b. This analysis reveals intrinsic variability in the residual light curve after subtraction of the binary model, in the frequency range [0, 10] d^–1. This makes HD 165246 only the second O+B eclipsing binary with asteroseismic potential. While some of the frequencies are connected with the rotation of the primary, others are interpreted as due to oscillations with periodicities of order days. The frequency resolution of the current data set does not allow us to distinguish between frequencies due to standing coherent oscillation modes or travelling waves. Future time-resolved high-precision spectroscopy covering several binary orbits will reveal whether HD 165246 is a Rosetta stone for synergistic binary and seismic modelling of an O-type star.