2009/11/02 by S.‐B. Qian, S.-B. Qian, Z.-B. Dai +6 · 55 citations
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Binary number #Binary star #Brown dwarf #Cataclysmic variable star #Eclipse #Exoplanet #Light curve #Mass ratio #Orbital period #Physics #Planet #Stars #Stellar, planetary, and galactic studies #White dwarf
paper · pdf · doi:10.1088/0004-637x/706/1/l96
published in The Astrophysical Journal 706(1), L96-L99 (IOP Publishing)
openalex publication_date 2009/11/02 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/01
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 (0 00031) 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 3 sin i ' = 0.0107(±0.0017) M ☉ when a total mass of 0.646 M ☉ for NN Ser is adopted. For orbital inclinations i ' ⩾ 49 56, 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.