@Article{AlmeidaJablRodr:2013:TwPoCi,
               author = "Almeida, Leonardo Andrade de and Jablonski, Francisco Jose and 
                         Rodrigues, Cl{\'a}udia Vilega",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Instituto Nacional de 
                         Pesquisas Espaciais (INPE)}",
                title = "Two possible circumbinary planets in the eclipsing post-common 
                         envelope system nsvs 14256825",
              journal = "Astrophysical Journal",
                 year = "2013",
               volume = "766",
               number = "1",
                pages = "11",
                month = "Mar.",
                 note = "arXiv:1210.3055 and arXiv:1210.3055v2",
             keywords = "estrelas bin{\'a}rias, exoplanetas, close binaries, eclipsing 
                         binaries, planetary systems, individual stars (NSVS 14256825), 
                         subdwarfs.",
             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 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.",
                  doi = "10.1088/0004-637X/766/1/11",
                  url = "http://dx.doi.org/10.1088/0004-637X/766/1/11",
                 issn = "0004-637X and 1538-4357",
                label = "lattes: 5605590098640584 2 AlmeidaJablRodrRodr:2013:TWPOCI",
             language = "en",
           targetfile = "1210.3055v2.pdf",
        urlaccessdate = "28 abr. 2024"
}