Distribution of refractory and volatile elements in CoRoT exoplanet host stars

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dc.contributor.authorChavero, C.
dc.contributor.authorde la Reza, R.
dc.contributor.authorDomingos, R. C. [UNESP]
dc.contributor.authorDrake, N. A.
dc.contributor.authorPereira, C. B.
dc.contributor.authorWinter, O. C. [UNESP]
dc.contributor.institutionObserv Nacl
dc.contributor.institutionSt Petersburg State Univ
dc.contributor.institutionUniversidade Estadual Paulista (Unesp)
dc.date.accessioned2014-05-20T15:33:50Z
dc.date.available2014-05-20T15:33:50Z
dc.date.issued2010-07-01
dc.description.abstractThe relative distribution of abundances of refractory, intermediate, and volatile elements in stars with planets can be an important tool for investigating the internal migration of a giant planet. This migration can lead to the accretion of planetesimals and the selective enrichment of the star with these elements. We report on a spectroscopic determination of the atmospheric parameters and chemical abundances of the parent stars in transiting planets CoRoT-2b and CoRoT-4b. Adding data for CoRoT-3 and CoRoT-5 from the literature, we find a flat distribution of the relative abundances as a function of their condensation temperatures. For CoRoT-2, the relatively high lithium abundance and intensity of its LiI resonance line permit us to propose an age of 120 Myr, making this star one of the youngest stars with planets to date. We introduce a new methodology to investigate a relation between the abundances of these stars and the internal migration of their planets. By simulating the internal migration of a planet in a disk formed only by planetesimals, we are able, for the first time, to separate the stellar fractions of refractory, intermediate, and volatile rich planetesimals accreting onto the central star. Intermediate and volatile element fractions enriching the star are similar and much larger than those of pure refractory ones. This result is opposite to what has been considered in the literature for the accreting self-enrichment processes of stars with planets. We also show that these results are highly dependent on the model adopted for the disk distribution regions in terms of refractory, intermediate, and also volatile elements and other parameters considered. We note however, that this self-enrichment mechanism is only efficient during the first 20-30 Myr or later in the lifetime of the disk when the surface convection layers of the central star for the first time attain its minimum size configuration.en
dc.description.affiliationObserv Nacl, BR-20921400 Rio de Janeiro, Brazil
dc.description.affiliationSt Petersburg State Univ, Sobolev Astron Inst, St Petersburg 198504, Russia
dc.description.affiliationUniv Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, Brazil
dc.description.affiliationUnespUniv Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, Brazil
dc.description.sponsorshipCoordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)
dc.description.sponsorshipConselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)
dc.description.sponsorshipFundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)
dc.format.extent13
dc.identifierhttp://dx.doi.org/10.1051/0004-6361/200912184
dc.identifier.citationAstronomy & Astrophysics. Les Ulis Cedex A: Edp Sciences S A, v. 517, p. 13, 2010.
dc.identifier.doi10.1051/0004-6361/200912184
dc.identifier.fileWOS000280929400050.pdf
dc.identifier.issn0004-6361
dc.identifier.lattes0960024575647258
dc.identifier.lattes6652169083464327
dc.identifier.orcid0000-0002-0516-0420
dc.identifier.urihttp://hdl.handle.net/11449/42333
dc.identifier.wosWOS:000280929400050
dc.language.isoeng
dc.publisherEdp Sciences S A
dc.relation.ispartofAstronomy & Astrophysics
dc.relation.ispartofsjr2,265
dc.rights.accessRightsAcesso aberto
dc.sourceWeb of Science
dc.subjectplanetary systemsen
dc.subjectstars: abundancesen
dc.subjectstars: fundamental parametersen
dc.titleDistribution of refractory and volatile elements in CoRoT exoplanet host starsen
dc.typeArtigo
dcterms.licensehttp://www.aanda.org/index.php?option=com_content&view=article&id=100&Itemid=104
dcterms.rightsHolderEdp Sciences S A
unesp.author.lattes0960024575647258
unesp.author.lattes6652169083464327[3]
unesp.author.orcid0000-0002-0516-0420[3]
unesp.campusUniversidade Estadual Paulista (Unesp), Faculdade de Engenharia, Guaratinguetápt

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