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dc.contributor.authorMacIejewski, G.-
dc.contributor.authorDimitrov, D.-
dc.contributor.authorFernández, Matilde-
dc.contributor.authorSota Ballano, Alfredo-
dc.contributor.authorNowak, G.-
dc.contributor.authorOhlert, J.-
dc.contributor.authorNikolov, G.-
dc.contributor.authorBukowiecki, L.-
dc.contributor.authorHinse, T.C.-
dc.contributor.authorPallé, E.-
dc.contributor.authorTingley, B.-
dc.contributor.authorKjurkchieva, D.-
dc.contributor.authorLee, J.W.-
dc.contributor.authorLee, C.U.-
dc.date.accessioned2016-06-21T08:27:22Z-
dc.date.available2016-06-21T08:27:22Z-
dc.date.issued2016-
dc.identifierdoi: 10.1051/0004-6361/201628312-
dc.identifierissn: 1432-0746-
dc.identifier.citationAstronomy and Astrophysics 588 (2016)-
dc.identifier.urihttp://hdl.handle.net/10261/133801-
dc.description.abstractAims. Most hot Jupiters are expected to spiral in toward their host stars because the angular momentum of the orbital motion is transferred to the stellar spin. Their orbits can also precess as a result of planet-star interactions. Calculations show that both effects might be detected for the very-hot exoplanet WASP-12 b using the method of precise transit-timing over a time span of about 10 yr. Methods. We acquired new precise light curves for 29 transits of WASP-12 b, spannning four observing seasons from November 2012 to February 2016. New mid-transit times, together with those from the literature, were used to refine the transit ephemeris and analyze the timing residuals. Results. We find that the transit times of WASP-12 b do not follow a linear ephemeris with a 5σ confidence level. They may be approximated with a quadratic ephemeris that gives a change rate in the orbital period of (-2.56 ± 0.40) × 10 s yr. The tidal quality parameter of the host star was found to be equal to 2.5 × 10, which is similar to theoretical predictions for Sun-like stars. We also considered a model in which the observed timing residuals are interpreted as a result of the apsidal precession. We find, however, that this model is statistically less probable than the orbital decay.-
dc.description.sponsorshipG.M. acknowledges funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement number RG226604 (OPTICON). G.M. and G.N. acknowledge the financial support from the Polish Ministry of Science and Higher Education through the Iuventus Plus grant and IP2011 031971. MF was supported by the Spanish grant AYA2014-54348-C3-1-R. T.C.H., J.W.L. & C.U.L. acknowledge travel support from KASI grant number 2013-9-400-00 and astronomical observations were carried out during a KRCF Young Scientist Research Fellowship Program. D.K. acknowledges the financial support from Shumen University, project RD 08-81. A part of this paper is the result of the exchange and joint research project Spectral and photometric studies of variable stars between the Polish and Bulgarian Academies of Sciences. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA.-
dc.publisherEDP Sciences-
dc.relationMINECO/ICTI2013-2016/AYA2014-54348-C3-1-R-
dc.relation.isversionofPublisher's version-
dc.rightsopenAccess-
dc.subjectPlanet-star interactions-
dc.subjectPlanets and satellites: individual: WASP-12 b-
dc.subjectStars: individual: WASP-12-
dc.titleDeparture from the constant-period ephemeris for the transiting exoplanet WASP-12 b-
dc.typeartículo-
dc.identifier.doi10.1051/0004-6361/201628312-
dc.date.updated2016-06-21T08:27:23Z-
dc.description.versionPeer Reviewed-
dc.language.rfc3066eng-
dc.contributor.funderMinistry of Science and Higher Education (Poland)-
dc.contributor.funderKorea Research Council of Fundamental Science and Technology-
dc.contributor.funderShumen University-
dc.contributor.funderEuropean Commission-
dc.contributor.funderMinisterio de Economía y Competitividad (España)-
dc.contributor.funderKorea Astronomy and Space Science Institute-
dc.relation.csic-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003714es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000780es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003717es_ES
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