J/AJ/144/35ivo://CDS.VizieR/J/AJ/144/35doi:10.26093/cds/vizier.51440035CDSKang Y.-W.Yushchenko A.Hong K.Kim S.Yushchenko V.2017-06-30T05:48:02Z2013-09-26T09:26:35ZCDS support team

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

cds-question@unistra.freclipsing-binary-starsspectroscopychemical-abundancesline-intensitieseffective-temperatureWe investigated ZZ Boo using a high-resolution (R=80000) spectrum obtained at the BOES echelle spectrograph attached to a 1.8m telescope at the Bohuynsan observatory in Korea. The atmospheric parameters of the components were found using the published photometrical observations and the abundance analysis of iron lines: the flux ratio of the components F_A_/F_B_=1.12+/-0.15, the effective temperatures of the components T_eff_=6860+/-20K and 6930+/-20K, the surface gravities log g=3.72+/-0.10 and 3.84+/-0.10, the metallicities [Fe/H]=-0.10+/-0.08 and -0.03+/-0.10, and the projected rotation velocities vsin i=11.9+/-0.4km/s and 19.3+/-0.8km/s for the primary and secondary components, respectively. The pointed errors are the formal errors of the methods used; the systematic errors of the temperatures, gravities, metallicities, and projected rotational velocities can be as high as 250-300K, 0.3dex, 0.15dex, and 4km/s, respectively. The abundances of 24 and 22 chemical elements were determined in the atmospheres of the components. The abundance pattern of the primary component shows the solar or slightly undersolar abundances of all elements. CNO abundances are close to solar values. The abundance pattern of this component resembles those of {lambda} Boo type stars. The abundances of light elements, except oxygen, in the atmosphere of the secondary component are practically solar. The abundances of barium and two detected lanthanides are close to the solar values; the overabundance of oxygen is 0.9dex. The abundances of two components are evidently different. The comparison of relative abundances with the condensation temperatures and second ionization potentials of the elements confirms the difference in abundance patterns and allows discussion of the different accretion scenarios for two components of this binary system.2012AJ....144...35Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/144/35CatalogResearchIsServedByTAP VizieR generic servicerelated-toV/130 : Geneva-Copenhagen Survey of Solar neighbourhood III (Holmberg+, 2009)VI/69 : Atomic Spectral Line List (Hirata+ 1995)J/MNRAS/415/2238 : Abundances of TX UMa (Glazunova+, 2011)J/A+A/511/A68 : Transitions of CrII (Gurell+, 2010)J/ApJS/167/292 : Laboratory transition probabilities for Gd IIJ/ApJ/645/613 : Abundances of HD 221170 (Ivans+, 2006)J/PASP/118/636 : Alpha Per High res. spectral atlas at 3810-8100{AA}J/AJ/128/846 : VRI observations of CE Leonis (Kang+, 2004)J/A+A/347/348 : Solar abundance of iron (Grevesse+, 1999)J/A+AS/126/21 : Velocities and duplicity of F-type dwarfs (Nordstroem+ 1997)J/A+A/281/161 : Radio emission from stars at 250GHz (Altenhoff+, 1994)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/144/35https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/144/35http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/144/35https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/144/35https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/144/35http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/144/35GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/AJ/144/35/table1Iron lines in the spectrum of ZZ BoorecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonIron line identifier (Fe I or Fe II)phys.atmol.ionStagecharlambda[4508/8825] Wavelength; in {AA}0.1nmem.wldoubleEW-A? Component A equivalent width; in m{AA}1e-13mspect.line.eqWidthfloatnullableEW-B? Component B equivalent width; in m{AA}1e-13mspect.line.eqWidthfloatnullablelog(gf)[-4.2/0.645] Log of the oscillatory strengthphys.atmol.collStrengthfloatr_log(gf)Reference to log(gf), in refs.dat filemeta.ref;pos.frameintElowLower energy level E_low_eVphys.energy;phys.atmol.levelfloatlogN-A? Component A abundance (where log N(H)=12)phys.abundfloatnullablelogN-B? Component B abundance (where log N(H)=12)phys.abundfloatnullableJ/AJ/144/35/linesLines of non-iron elements in therecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonElemental line identificationphys.atmol.ionStagecharlambda[3856/8695] Wavelength; in {AA}0.1nmem.wldoubleCompSimbad column added by the CDSmeta.code.multipcharlog(gf)Log of the oscillatory strengthphys.abundfloatRef[1/27]? Reference to log(gf), in refs.dat filemeta.refintnullablef_RefFlag on Ref (h) (1)meta.codecharElowLower energy level E_low_eVphys.energy;phys.atmol.levelfloatlogN[0.8/9.7] ZZ Boo abundance (log N(H)=12)phys.abundfloatlogNo[0.8/8.7]? Solar abundancephys.abundfloatnullableDlogN[-0.573/0.993] Abundance relative to the Sunlog(Sun)phys.abundfloatBl[0/1] ZZ Boo blending (1=clean line)meta.notefloatBl0[0/1]? Solar blending (1=clean line)meta.notefloatnullableD[0/1] ZZ Boo Depth in synthetic spectraphot.flux.density;arith.ratiofloatDo[0/1]? Solar depth in synthetic spectraphot.flux.density;arith.ratiofloatnullablee(T)? ZZ Boo error in abundance for a change in effective temperatures +/-100Kstat.errorfloatnullablee(g)? ZZ Boo error in abundance for a cja,ge in logg of +0.2dexstat.errorfloatnullableDC-bestZZ Boo depth in best combined synthetic spectrum of the binaryphot.flux.density;arith.ratiofloatDC-0.5ZZ Boo depth with under-abundance by 0.5dexphot.flux.density;arith.ratiofloatDC+0.5ZZ Boo depth with over-abundance by 0.5dexphot.flux.density;arith.ratiofloatJ/AJ/144/35/table5Mean abundances of chemical elements in the atmospheres of components of ZZ BooZ[6/64] Atomic numbermeta.id;meta.mainintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintCompZZ Boo component (A=primary component, B=secondary component)meta.code.multipcharIonInvestigated species identificationphys.atmol.ionStagecharNL[1/76] Number of lines usedmeta.idintAb-bestBest value abundance (ZZ Boo minus Solar)log(Sun)phys.abundfloate_Ab-best? error in Ab-bestlog(Sun)stat.errorfloatnullableAb+100KAbundance (ZZ Boo minus Solar) with effective temperature shifted by +100K)log(Sun)phys.abundfloate_Ab+100K? error in Ab+100Klog(Sun)stat.errorfloatnullableAb+0.2Abundance (ZZ Boo minus Solar) with surface gravity shifted by +0.2dex)log(Sun)phys.abundfloate_Ab+0.2? error in Ab+0.2log(Sun)stat.errorfloatnullablelogN-bestBest value of ZZ Boo absolute mean abundancephys.abundfloate_logN-best? error in logN-stat.errorfloatnullablelogN+100KAbsolute mean abundance of ZZ Boo with effective temperature shifted by +100Kphys.abundfloate_logN+100K? error in logN+100Kstat.errorfloatnullablelogN+0.2Absolute mean abundance of ZZ Boo with surface gravity shifted by +0.2cm/s^2^)phys.abundfloate_logN+0.2? error in logN-loggstat.errorfloatnullableJ/AJ/144/35/refsReferencesComCommentsmeta.notecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRef[1/27] Reference numbermeta.id;meta.mainintprimaryBibCodeBibliographic codemeta.bib.bibcodecharAutAuthors's namemeta.bib.authorchar