2013ApJ...766...11A

We present an analysis of eclipse timings of the post-common envelope binary NSVS 14256825, which is composed of an sdOB star and a dM star in a close orbit (P_orb= 0.110374 days). High-speed photometry of this system was performed between 2010 July and 2012 August. Ten new mid-eclipse times were analyzed together with all available eclipse times in the literature. We revisited the (O - C) diagram using a linear ephemeris and verified a clear orbital period variation. On the assumption that these orbital period variations are caused by light travel time effects, the (O - C) diagram can be explained by the presence of two circumbinary bodies, even though this explanation requires a longer baseline of observations to be fully tested. The orbital periods of the best solution would be P_c∼ 3.5 years and P_d ∼ 6.9 years. The corresponding projected semi-major axes would be a_csin i_c∼ 1.9 AU and a_d sin i_d∼ 2.9 AU. The masses of the external bodies would be M_c∼ 2.9 M_Jupiter and M_d∼ 8.1 M_Jupiter, if we assume their orbits are coplanar with the close binary. Therefore NSVS 14256825 might be composed of a close binary with two circumbinary planets, though the orbital period variations is still open to other interpretations.