J/A+A/614/A138ivo://CDS.VizieR/J/A+A/614/A138doi:10.26093/cds/vizier.36140138CDSLiu F.Yong D.Asplund M.Feltzing S.Mustill A.J.Melendez J.,Ramirez I.Lin J.2018-09-26T14:55:36Z2018-07-03T07:01:03ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmultiple-starssolar-system-planetsexoplanetsline-intensitiesDifferences in the elemental abundances of planet-hosting stars in binary systems can give important clues and constraints about planet formation and evolution. In this study we performed a high-precision, differential elemental abundance analysis of a wide binary system, HD 80606/80607, based on high-resolution spectra with high signal-to-noise ratio obtained with Keck/HIRES. HD 80606 is known to host a giant planet with the mass of four Jupiters, but no planet has been detected around HD 80607 so far. We determined stellar parameters as well as abundances for 23 elements for these two stars with extremely high precision. Our main results are that (i) we confirmed that the two components share very similar chemical compositions, but HD 80606 is marginally more metal-rich than HD 80607, with an average difference of +0.013+/-0.002dex ({sigma}=0.009dex); and (ii) there is no obvious trend between abundance differences and condensation temperature. Assuming that this binary formed from material with the same chemical composition, it is difficult to understand how giant planet formation could produce the present-day photospheric abundances of the elements we measure. We cannot exclude the possibility that HD 80606 might have accreted about 2.5 to 5M_Earth_ material onto its surface, possibly from a planet destabilised by the known highly eccentric giant.2018A&A...614A.138Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/614/A138CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/516/A95 : Photometry and spectroscopy of HD 80606b (Hebrard+, 2010)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/614/A138https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/614/A138http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/614/A138https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/614/A138https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/614/A138http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/614/A138GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/614/A138/tablea1Atomic line data, as well as the EW measurements, adopted for our analysisrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelength (Angstrom)0.1nmem.wldoubleSpeciesSpeciesmeta.notecharEpLower excitation potential (eV)eVphys.atmol.excitation;stat.minfloatloggfOscillator strength (loggf)phys.atmol.oscStrengthfloatEW1Equivalent widths for Vesta (m{AA})0.0001nmspect.line.eqWidthfloatEW2Equivalent widths for HD 80606 (m{AA})0.0001nmspect.line.eqWidthfloatEW3Equivalent widths for HD 80607 (m{AA})0.0001nmspect.line.eqWidthfloat