%0 Journal Article
%4 dpi.inpe.br/plutao/2013/05.31.18.49
%2 dpi.inpe.br/plutao/2013/05.31.18.49.18
%@doi 10.1088/0004-637X/766/1/11
%@issn 0004-637X
%@issn 1538-4357
%F lattes: 5605590098640584 2 AlmeidaJablRodrRodr:2013:TWPOCI
%T Two possible circumbinary planets in the eclipsing post-common envelope system nsvs 14256825
%D 2013
%8 Mar.
%9 journal article
%A Almeida, Leonardo Andrade de,
%A Jablonski, Francisco Jose,
%A Rodrigues, Cláudia Vilega,
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@electronicmailaddress leonardodealmeida.andrade@gmail.com
%@electronicmailaddress chico@das.inpe.br
%@electronicmailaddress claudiavilega@gmail.com
%B Astrophysical Journal
%V 766
%N 1
%P 11
%K estrelas binárias, exoplanetas, close binaries, eclipsing binaries, planetary systems, individual stars (NSVS 14256825), subdwarfs.
%X 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 Pc ~3.5 years and Pd ~6.9 years. The corresponding projected semi-major axes would be a_c sin i_c ~1.9AU and a_d sin i_d ~ 2.9AU. The masses of the external bodies would be Mc ~2.9M_Jupiter and Md ~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.
%@language en
%3 1210.3055v2.pdf
%O arXiv:1210.3055
%O arXiv:1210.3055v2