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dc.contributor.authorPavlenko, Ya V.
dc.contributor.authorJenkins, J. S.
dc.contributor.authorIvanyuk, O. M.
dc.contributor.authorJones, Hugh
dc.contributor.authorKaminsky, B. M.
dc.contributor.authorLyubchik, Yu. P.
dc.contributor.authorYakovina, L. A.
dc.date.accessioned2018-06-06T17:07:33Z
dc.date.available2018-06-06T17:07:33Z
dc.date.issued2018-03-20
dc.identifier.citationPavlenko , Y V , Jenkins , J S , Ivanyuk , O M , Jones , H , Kaminsky , B M , Lyubchik , Y P & Yakovina , L A 2018 , ' A detailed study of Lithium in 107 CHEPS dwarf stars ' , Astronomy & Astrophysics , vol. 611 , A27 . https://doi.org/10.1051/0004-6361/201731547
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 12613340
dc.identifier.otherPURE UUID: c6ae65e8-6fe2-431a-92f0-0849976b3e5c
dc.identifier.otherScopus: 85044258294
dc.identifier.urihttp://hdl.handle.net/2299/20137
dc.descriptionReproduced with permission from Astronomy & Astrophysics, © ESO 2018.
dc.description.abstractContext. We report results from lithium abundance determinations using high resolution spectral analysis of the 107 metal-rich stars from the Calan-Hertfordshire Extrasolar Planet Search programme. Aims. We aim to set out to understand the lithium distribution of the population of stars taken from this survey. Methods. The lithium abundance taking account of non-local thermodynamical equilibrium effects was determined from the fits to the Li I 6708 Å resonance doublet profiles in the observed spectra. Results. We find that a) fast rotators tend to have higher lithium abundances; b) log N(Li) is higher in more massive and hot stars; c) log N(Li) is higher in stars of lower log g; d) stars with the metallicities >0.25 dex do not show the lithium lines in their spectra; e) most of our planet hosts rotate slower; and f) a lower limit of lithium isotopic ratio is 7Li/ 6Li > 10 in the atmospheres of two stars with planets (SWP) and two non-SWP stars. Conclusions. Measurable lithium abundances were found in the atmospheres of 45 stars located at distances of 20-170 pc from the Sun, for the other 62 stars the upper limits of log N(Li) were computed. We found well defined dependences of lithium abundances on T eff, V sin i, and less pronounced for the log g. In case of V sin i we see two sequences of stars: with measurable lithium and with the upper limit of log N(Li). About 10% of our targets are known to host planets. Only two SWP have notable lithium abundances, so we found a lower proportion of stars with detectable Li among known planet hosts than among stars without planets. However, given the small sample size of our planet-host sample, our analysis does not show any statistically significant differences in the lithium abundance between SWP and stars without known planets.en
dc.format.extent16
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysics
dc.rightsOpen
dc.subjectPlanetary systems
dc.subjectStars: abundances
dc.subjectStars: atmospheres
dc.subjectStars: rotation
dc.subjectStars: solar-type
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleA detailed study of Lithium in 107 CHEPS dwarf starsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionCentre of Data Innovation Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85044258294&partnerID=8YFLogxK
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2018-03-20
rioxxterms.versionP
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201731547
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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