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dc.contributor.authorBond, J.
dc.contributor.authorLauretta, D.S.
dc.contributor.authorTinney, C.G.
dc.contributor.authorButler, R.P.
dc.contributor.authorMarcy, G.W.
dc.contributor.authorJones, H.R.A.
dc.contributor.authorCarter, B.D.
dc.contributor.authorO'Toole, S.
dc.contributor.authorBailey, J.
dc.date.accessioned2009-01-07T09:30:47Z
dc.date.available2009-01-07T09:30:47Z
dc.date.issued2008
dc.identifier.citationBond , J , Lauretta , D S , Tinney , C G , Butler , R P , Marcy , G W , Jones , H R A , Carter , B D , O'Toole , S & Bailey , J 2008 , ' Beyond the Iron Peak: r- and s-process Elemental Abundances in Stars with Planets ' , The Astrophysical Journal , vol. 682 , pp. 1234-1247 . https://doi.org/10.1086/589236
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 151066
dc.identifier.otherPURE UUID: e2054058-d1e3-43da-98f9-ff3d4e2df32a
dc.identifier.otherdspace: 2299/2752
dc.identifier.otherScopus: 53549133394
dc.identifier.urihttp://hdl.handle.net/2299/2752
dc.descriptionOriginal article can be found at: http://www.iop.org/EJ/journal/apj Copyright American Astronomical Society DOI: 10.1086/589236 [Full text of this article is not available in the UHRA]
dc.description.abstractWe present elemental abundances of 118 stars (28 of which are known extrasolar planetary host stars) observed as part of the Anglo-Australian Planet Search. Abundances of O, Mg, Cr, Y, Zr, Ba, Nd, and Eu (along with previously published abundances for C and Si) are presented. This study is one of the first to specifically examine planetary host stars for the heavy elements produced by neutron capture reactions. We find that the abundances in host stars are chemically different from both the standard solar abundances and the abundances in non-host stars in all elements studied, with enrichments over non-host stars ranging from 0.06 dex (for O) to 0.11 dex (for Cr and Y). Such abundance trends are in agreement with other previous studies of field stars and lead us to conclude that the chemical anomalies observed in planetary host stars are the result of normal galactic chemical evolution processes. Based on this observation, we conclude that the observed chemical traits of planetary host stars are primordial in origin, coming from the original nebula and not from a "pollution" process occurring during or after formation, and that planet formation occurs naturally with the evolution of stellar material.en
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.titleBeyond the Iron Peak: r- and s-process Elemental Abundances in Stars with Planetsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1086/589236
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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