ABSTRACT. NN Ser is a short-period (P = 3.12 hr) close binary containing a very hot white dwarf primary with a mass of 0.535 M and a fully convective secondary with a mass of 0.111 M . The changes in the orbital period of the eclipsing binary were analyzed based on our five newly determined eclipse times together with those compiled from the literature. A small-amplitude (000031) cyclic period variation with a period of 7.56 years was discovered to be superimposed on a possible long-term decrease. The periodic change was plausibly explained as the light-travel time effect via the presence of a tertiary companion. The mass of the tertiary companion is determined to be M ₃sin i' = 0.0107(±0.0017) M when a total mass of 0.646 M for NN Ser is adopted. For orbital inclinations i' ≥ 4956, the mass of the tertiary component was calculated to be M ₃ ≤ 0.014 M ; thus it would be an extrasolar planet. The third body is orbiting the white dwarf-red dwarf eclipsing binary at a distance shorter than 3.29 AU. Since the observed decrease rate of the orbital period is about two orders larger than that caused by gravitational radiation, it can be plausibly interpreted by magnetic braking of the fully convective component, which is driving this binary to evolve into a normal cataclysmic variable.

Key words: binaries: close; binaries: eclipsing; stars: individual (NN Ser); stars: low-mass, brown dwarfs; white dwarfs

Print publication: Issue 1 (2009 November 20)
Received 2009 June 25, accepted for publication 2009 October 15
Published 2009 November 2