J/A+A/561/A7ivo://CDS.VizieR/J/A+A/561/A7doi:10.26093/cds/vizier.35610007CDSRamirez I.Melendez J.Asplund M.2017-11-06T12:23:29Z2013-12-17T11:30:06ZCDS support team

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

cds-question@unistra.frmultiple-starssolar-system-planetschemical-abundanceseffective-temperaturestellar-massesstellar-agesElemental abundance studies of solar twin stars suggest that the solar chemical composition contains signatures of the formation of terrestrial planets in the solar system, namely small but significant depletions of the refractory elements. To test this hypothesis, we study stars which, compared to solar twins, have less massive convective envelopes (therefore increasing the amplitude of the predicted effect) or are, arguably, more likely to host planets (thus increasing the frequency of signature detections). We measure relative atmospheric parameters and elemental abundances of a late-F type dwarf sample (52 stars) and a sample of metal-rich solar analogs (59 stars). We detect refractory-element depletions with amplitudes up to about 0.15dex. The distribution of depletion amplitudes for stars known to host gas giant planets is not different from that of the rest of stars. The maximum amplitude of depletion increases with effective temperature from 5650K to 5950K, while it appears to be constant for warmer stars (up to 6300K). The depletions observed in solar twin stars have a maximum amplitude that is very similar to that seen here for both of our samples. Gas giant planet formation alone cannot explain the observed distributions of refractory-element depletions, leaving the formation of rocky material as a more likely explanation of our observations. More rocky material is necessary to explain the data of solar twins than metal-rich stars, and less for warm stars. However, the sizes of the stars' convective envelopes at the time of planet formation could be regulating these amplitudes. Our results could be explained if disk lifetimes were shorter in more massive stars, as independent observations indeed seem to suggest.2014A&A...561A...7Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/561/A7CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/468/663 : Li abundances in solar-analog stars (Takeda+, 2007)J/A+A/515/A93 : Li abundances in solar-analog stars. II. (Takeda+, 2010)J/AJ/138/312 : Activity of bright solar analogs (Hall+, 2009)J/ApJ/720/1592 : Abundances of solar analogs with planets (Hernandez+, 2010)J/A+A/508/L17 : Abundances in solar analogs (Ramirez+, 2009)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/561/A7https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/561/A7http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/561/A7https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/561/A7https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/561/A7http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/561/A7GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/561/A7/stars (Sample and literature data, atmospheric parameters, mass, age, chromospheric activity data, and abundances)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/561/A7/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/561/A7/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/561/A7/stars?GETtext/xml+votable180.050000true1.5798978-49.07518940.0055555555555555566/311 4136 4634 4661 12644 12905 16519 17219 17266 17529 17730 17989 18112 18366 19391 19541 19720 20016 20072 20118 20144 20605 20746 21080 21428 21780 21906 22159 22289 22590 22654 22800 23018 23030 23201 23545 24227 25078 25978 26242 26748 27018 27143 27645 27712 28196 28763 29291 29978 30195 30218 30278 30526 30576 30707 30848 30939 31015 31494 31860 33258 33717 34479 34497 34905 35064 35362 35968 36834 36854 37716 37954 38918 39282 39364 39555 39563 39888 39915 40453 41167 41290 42248 42386 42860 42934 43577 43677 43699 43797 43813 44228 44243 44398 44740 45034 45228 45364 45457 45656 45865 46306 47550 47590 48022 48105 48182 48519 48821 49114https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/561/A7?format=asciidefaultJ/A+A/561/A7/starsSample and literature data, atmospheric parameters, mass, age, chromospheric activity data, and abundancese_d[Cu/H]Error on d[Cu/H] (4)stat.error;phys.abundfloatd[Zn/H]Differential zinc abundance (4)phys.abundfloate_d[Zn/H]Error on d[Zn/H] (4)stat.error;phys.abundfloatd[Ba/H]Differential barium abundance (4)phys.abundfloate_d[Ba/H]Error on d[Ba/H] (4)stat.error;phys.abundfloat_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHIPHipparcos numbermeta.id;meta.mainintVmagApparent visual magnitudemagphot.mag;em.opt.Vfloate_d[Al/H]Error on d[Al/H] (4)stat.error;phys.abundfloatTefflEffective temperature (1)Kphys.temperature.effectiveintlogglSurface gravity (1)log(cm.s**-2)phys.gravityfloat[Fe/H]lMetallicity (1)log(Sun)phys.abund.FefloatNlitNumber of sources of atmospheric parameters (1)meta.numberintMpl? Mass of known planet hosted (2)(1.898187x10+27kg)phys.massfloatnullableTeffEffective temperature from this workKphys.temperature.effectiveintloggSurface gravity from this worklog(cm.s**-2)phys.gravityfloat[Fe/H]Metallicity from this worklog(Sun)phys.abund.ZfloatvtMicroturbulence from this workkm/sphys.veloc.microTurbfloatdTeffDifferential effective temperature (3)Kphys.temperature.effectiveinte_dTeffError on DTeff (3)Kstat.errorintdloggDifferential surface gravity (3)log(cm.s**-2)phys.gravity;arith.difffloate_dloggError on Dlogg (3)log(cm.s**-2)stat.errorfloatd[Fe/H]Differential metallicity (3)log(Sun)phys.abund.Fefloate_d[Fe/H]Error on d[Fe/H] (3)log(Sun)stat.error;phys.abund.FefloatMassMass of starsolMassphys.massfloate_Mass2-{sigma} mass lower limitsolMassstat.error;phys.massfloatE_Mass2-{sigma} mass upper limitsolMassstat.error;stat.maxfloattauAge {tau}Gyrtime.agefloate_tau2-{sigma} age lower limitGyrstat.errorfloatE_tau2-{sigma} age upper limitGyrstat.error;stat.maxfloatActlog(R'_HK_) activity indexphot.flux;arith.ratiofloatSimbadSimbad column added by the CDSmeta.ref.urlchard[C/H]Differential carbon abundance (4)phys.abundfloate_d[C/H]Error on d[C/H] (4)stat.error;phys.abundfloatd[O/H]Differential oxygen abundance (4)phys.abundfloate_d[O/H]Error on d[O/H] (4)stat.error;phys.abundfloatd[Na/H]Differential sodium abundance (4)phys.abundfloate_d[Na/H]Error on d[Na/H] (4)stat.error;phys.abundfloatd[Mg/H]Differential magnesium abundance (4)phys.abundfloate_d[Mg/H]Error on d[Mg/H] (4)stat.error;phys.abundfloatd[Al/H]Differential aluminium abundance (4)phys.abundfloatd[Si/H]Differential silicon abundance (4)phys.abundfloate_d[Si/H]Error on d[Si/H] (4)stat.error;phys.abundfloatd[S/H]Differential sulfur abundance (4)phys.abundfloate_d[S/H]Error on d[S/H] (4)stat.error;phys.abundfloatd[Ca/H]Differential calcium abundance (4)phys.abundfloate_d[Ca/H]Error on d[Ca/H] (4)stat.error;phys.abundfloatd[Sc/H]Differential scandium abundance (4)phys.abundfloate_d[Sc/H]Error on d[Sc/H] (4)stat.error;phys.abundfloatd[Ti/H]Differential titanium abundance (4)phys.abundfloate_d[Ti/H]Error on d[Ti/H] (4)stat.error;phys.abundfloatd[V/H]Differential vanadium abundance (4)phys.abundfloate_d[V/H]Error on d[V/H] (4)stat.error;phys.abundfloatd[Cr/H]Differential chromium abundance (4)phys.abundfloate_d[Cr/H]Error on d[Cr/H] (4)stat.error;phys.abundfloatd[Mn/H]Differential manganese abundance (4)phys.abundfloate_d[Mn/H]Error on d[Mn/H] (4)stat.error;phys.abundfloatd[Co/H]Differential cobalt abundance (4)phys.abundfloate_d[Co/H]Error on d[Co/H] (4)stat.error;phys.abundfloatd[Ni/H]Differential nickel abundance (4)phys.abundfloate_d[Ni/H]Error on d[Ni/H] (4)stat.error;phys.abundfloatd[Cu/H]Differential cupper abundance (4)phys.abundfloatJ/A+A/561/A7/linelistAtomic line list including HFS parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSpeciesSpeciesmeta.notecharTcond? Condensation temperatureKphys.temperatureintnullablelambda[4491/8683] Wavelength {lambda} ({AA})0.1nmem.wldoubleEP? Excitation potentialeVphys.atmol.excitationfloatnullablelog(gf)Transition probabilityphys.atmol.oscStrengthfloat