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dc.contributor.authorBond, J.
dc.contributor.authorTinney, C.G.
dc.contributor.authorButler, R.P.
dc.contributor.authorJones, H.R.A.
dc.contributor.authorMarcy, G.W.
dc.contributor.authorPenny, A.J.
dc.contributor.authorCarter, B.D.
dc.date.accessioned2007-08-20T13:41:43Z
dc.date.available2007-08-20T13:41:43Z
dc.date.issued2006
dc.identifier.citationBond , J , Tinney , C G , Butler , R P , Jones , H R A , Marcy , G W , Penny , A J & Carter , B D 2006 , ' The abundance distribution of stars with planets ' , Monthly Notices of the Royal Astronomical Society , vol. 370 , no. 1 , pp. 163-173 . https://doi.org/10.1111/j.1365-2966.2006.10459.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 167469
dc.identifier.otherPURE UUID: 82b65413-32f5-49ef-b124-73000e5dae2b
dc.identifier.otherdspace: 2299/483
dc.identifier.otherScopus: 33746078404
dc.identifier.urihttp://hdl.handle.net/2299/483
dc.descriptionThe definitive version is available at www.blackwell-synergy.com--Copyright Blackwell Publishing DOI : 10.1111/j.1365-2966.2006.10459.x
dc.description.abstractWe present the results of a uniform, high-precision spectroscopic metallicity study of 136 G-type stars from the Anglo-Australian Planet Search, 20 of which are known to harbour extrasolar planets (as at July 2005). Abundances in Fe, C, Na, Al, Si, Ca, Ti and Ni are presented, along with StrÄomgen photometric metallicities. This study is one of several recent studies examining the metallicities of a sample of planet-host and non- planet-host stars that were obtained from a single sample, and analysed in an identical manner, providing an unbiased estimate of the metallicity trends for planet bearing stars. We find that non-parametric tests of the distribution of metallicities for planet- host and non-planet-host stars are significantly different at a level of 99.4% confidence. We confirm the previously observed trend for planet-host stars to have higher mean metallicities than non-planet-host stars, with a mean metallicity for planet-host stars of [Fe/H]=0.06§0.03 dex compared with [Fe/H]=¡0.09§0.01 dex for non-host-stars in our sample. This enrichment is also seen in the other elements studied. Based on our findings, we suggest that this observed enhancement is more likely a relic of the original gas cloud from which the star and its planets formed, rather than being due to "pollution" of the stellar photosphere.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleThe abundance distribution of stars with planetsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2006.10459.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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