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		<doi>10.1088/0004-637X/766/1/11</doi>
		<issn>0004-637X</issn>
		<issn>1538-4357</issn>
		<label>lattes: 5605590098640584 2 AlmeidaJablRodrRodr:2013:TWPOCI</label>
		<citationkey>AlmeidaJablRodr:2013:TwPoCi</citationkey>
		<title>Two possible circumbinary planets in the eclipsing post-common envelope system nsvs 14256825</title>
		<project>CAPES (LAA); CNPq (CVR: 308005/2009-0); FAPESP (CVR: 2010/01584-8).</project>
		<year>2013</year>
		<month>Mar.</month>
		<typeofwork>journal article</typeofwork>
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		<author>Almeida, Leonardo Andrade de,</author>
		<author>Jablonski, Francisco Jose,</author>
		<author>Rodrigues, Cláudia Vilega,</author>
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		<group>DAS-CEA-INPE-MCTI-GOV-BR</group>
		<group>DAS-CEA-INPE-MCTI-GOV-BR</group>
		<affiliation>Instituto Nacional de Pesquisas Espaciais (INPE)</affiliation>
		<affiliation>Instituto Nacional de Pesquisas Espaciais (INPE)</affiliation>
		<affiliation>Instituto Nacional de Pesquisas Espaciais (INPE)</affiliation>
		<electronicmailaddress>leonardodealmeida.andrade@gmail.com</electronicmailaddress>
		<electronicmailaddress>chico@das.inpe.br</electronicmailaddress>
		<electronicmailaddress>claudiavilega@gmail.com</electronicmailaddress>
		<e-mailaddress>chico@das.inpe.br</e-mailaddress>
		<journal>Astrophysical Journal</journal>
		<volume>766</volume>
		<number>1</number>
		<pages>11</pages>
		<secondarymark>A1 A1 A1 A2</secondarymark>
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		<contenttype>External Contribution</contenttype>
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		<keywords>estrelas binárias, exoplanetas, close binaries, eclipsing binaries, planetary systems, individual stars (NSVS 14256825), subdwarfs.</keywords>
		<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&#8722;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&#8722;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.</abstract>
		<area>CEA</area>
		<language>en</language>
		<targetfile>1210.3055v2.pdf</targetfile>
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		<notes>arXiv:1210.3055</notes>
		<notes>arXiv:1210.3055v2</notes>
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