TWO POSSIBLE CIRCUMBINARY PLANETS IN THE ECLIPSING POST-COMMON ENVELOPE SYSTEM NSVS 14256825

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 newmid-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 similar to 3.5 years and P-d similar to 6.9 years. The corresponding projected semi-major axes would be a(c) sin i(c) similar to 1.9AU and a(d) sin i(d) similar to 2.9AU. The masses of the external bodies would be M-c similar to 2.9M(Jupiter) and M-d similar to 8.1M(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.