J/ApJ/819/19ivo://CDS.VizieR/J/ApJ/819/19doi:10.26093/cds/vizier.18190019CDSTeske J.K.Khanal S.Ramirez I.2017-01-23T22:00:00Z2016-06-15T09:13:52ZCDS support team

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

cds-question@unistra.frmultiple-starssolar-system-planetsline-intensitiesBinary stars provide an ideal laboratory for investigating the potential effects of planet formation on stellar composition. Assuming that the stars formed in the same environment/from the same material, any compositional anomalies between binary components might indicate differences in how material was sequestered in planets, or accreted by the star in the process of planet formation. We present here a study of the elemental abundance differences between WASP-94A and B, a pair of stars that each host a hot Jupiter exoplanet. The two stars are very similar in spectral type (F8 and F9), and their ~2700AU separation suggests that their protoplanetary disks were likely not influenced by stellar interactions, but WASP-94Ab's orbit --misaligned with the host star spin axis and likely retrograde-- points toward a dynamically active formation mechanism, perhaps different from that of WASP-94Bb, which is not misaligned and has a nearly circular orbit. Based on our high-quality spectra and strictly relative abundance analysis, we detect a depletion of volatiles (~-0.02dex, on average) and enhancement of refractories (~0.01dex) in WASP-94A relative to B (standard errors are ~0.005dex). This is different from every other published case of binary host star abundances, in which either no significant abundance differences are reported or there is some degree of enhancement in all elements, including volatiles. Several scenarios that may explain the abundance trend are discussed, but none can be definitively accepted or rejected. Additional high-contrast imaging observations to search for companions that may be dynamically affecting the system, as well as a larger sample of binary host star studies, are needed to better understand the curious abundance trends we observe in WASP-94A and B.2016ApJ...819...19Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/819/19CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/580/A24 : Abundances in dwarfs, subgiants, and giants (da Silva+, 2015)J/A+A/576/A69 : Li abundances in F stars (Delgado+, 2015)J/A+A/572/A49 : WASP-94AB photometry and RVs (Neveu-VanMalle+, 2014)J/A+A/562/A71 : Solar neighbourhood dwarf chemical abundances (Bensby+, 2014)J/A+A/561/A7 : Abundances for stars with planets (Ramirez+, 2014)J/ApJ/771/107 : Spectroscopy of faint KOI stars (Everett+, 2013)J/A+A/552/A6 : Abundances of F-G MS stars (Gonzalez Hernandez+, 2013)J/ApJ/743/24 : Solar models with accretion. I. (Serenelli+, 2011)J/ApJ/732/55 : Abundances of stars with planets (Schuler+, 2011)J/ApJ/720/1290 : Abundances of stars hosting planets (Ghezzi+, 2010)J/ApJ/715/1050 : Predicted abundances for extrasolar planets. I. (Bond+, 2010)J/A+A/512/A54 : Teff and Fbol from Infrared Flux Method (Casagrande+, 2010)J/A+A/508/L17 : Abundances in solar analogs (Ramirez+, 2009)J/A+A/487/373 : Spectroscopic parameters of 451 HARPS-GTO stars (Sousa+, 2008)J/A+A/465/271 : Oxygen abundances in nearby stars (Ramirez+, 2007)J/A+A/454/581 : Iron abundances of 33 wide binaries (Desidera+, 2006)J/ApJ/622/1102 : The planet-metallicity correlation. (Fischer+, 2005)J/A+A/420/683 : Equivalent widths of 23 wide binaries (Desidera+, 2004)J/A+A/415/1153 : [Fe/H] for 98 extra-solar planet-host stars (Santos+, 2004)J/A+A/377/123 : Equivalent widths of 6 binaries (Gratton+, 2001)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/819/19https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/819/19http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/819/19https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/819/19https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/819/19http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/819/19GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/819/19/table1Measured lines and equivalent widthsIonIonphys.atmol.ionStagecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[4218.7/8435.7] Wavelength in Angstroms0.1nmem.wldoubleExPot[0/9.2] Excitation potentialeVphys.atmol.excitationfloatlog(gf)[-5.5/0.6] Log of the oscillator strengthphys.atmol.oscStrengthfloatEWS[12.5/119.5]? Equivalent width of the solar spectrum1e-13mspect.line.eqWidthfloatnullableEWA-IR[3.9/169]? Equivalent width of the WASP-94A spectrum measured by Ramirez I.1e-13mspect.line.eqWidth;em.opt.IfloatnullableEWA-SK[3.6/167]? Equivalent width of the WASP-94A spectrum measured by Khanal S.1e-13mspect.line.eqWidthfloatnullableEWA-JT[3.6/166]? Equivalent width of the WASP-94A spectrum measured by Teske J.K.1e-13mspect.line.eqWidthfloatnullableEWB-IR[4/173.3]? Equivalent width of the WASP-94B spectrum measured by Ramirez I.1e-13mspect.line.eqWidth;em.opt.IfloatnullableEWB-SK[4.9/167]? Equivalent width of the WASP-94B spectrum measured by Khanal S.1e-13mspect.line.eqWidthfloatnullableEWB-JT[4.7/166]? Equivalent width of the WASP-94B spectrum measured by Teske J.K.1e-13mspect.line.eqWidthfloatnullable