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 July , 2010 and August , 2012 .
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 } \sim 3.5 years and P _ { d } \sim 6.9 years .
The corresponding projected semi-major axes would be a _ { c } \sin i _ { c } \sim 1.9 AU and a _ { d } \sin i _ { d } \sim 2.9 AU .
The masses of the external bodies would be M _ { c } \sim 2.9 ~ { } M _ { Jupiter } and M _ { d } \sim 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 .