| Full text | |
| Author(s): |
Total Authors: 3
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| Affiliation: | [1] Inst Nacl Pesquisas Espaciais, Div Astrofis, BR-12201 Sao Jose Dos Campos, SP - Brazil
Total Affiliations: 1
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| Document type: | Journal article |
| Source: | ASTROPHYSICAL JOURNAL; v. 766, n. 1 MAR 20 2013. |
| Web of Science Citations: | 23 |
| Abstract | |
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. (AU) | |
| FAPESP's process: | 10/01584-8 - SPARC4: simultaneous polarimeter and rapid camera in four bands |
| Grantee: | Cláudia Vilega Rodrigues |
| Support Opportunities: | Regular Research Grants |