J/AJ/145/167ivo://CDS.VizieR/J/AJ/145/167doi:10.26093/cds/vizier.51450167CDSKang Y.-W.Yushchenko A.V.Hong K.Guinan E.F.Gopka V.F.2026-03-18T11:46:11Z2014-06-13T07:06:06ZCDS support team

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

cds-question@unistra.freclipsing-binary-starschemical-abundancesline-intensitiesWe present spectroscopic observations of LX Per carried out using the Korean Bohyunsan Observatory Echelle Spectrograph (BOES) with spectral resolving power R=80000. The spectrograph was attached to the 1.8m telescope. The fit of synthetic spectra to the observed spectrum of the system allowed us to find the component parameters and the abundances of chemical elements in the atmospheres of the components. The strong CaII H&K emissions are confirmed; we also found emission lines in the CaII reversals' triplet absorptions at the wavelengths of 8498, 8542, and 8662{AA} in the spectrum of the cooler component of LX Per. A unique photometric solution using the distorted light curves of three different epochs was made. The spot model light curves were fitted to the 1981, 1982, and 1983 observations successfully by adjusting only spot parameters. We could infer that the variation of spot location and size was the main reason for the changing shape of light curves. The main feature of the abundance patterns of both components was the apparent deficiency of heavy (Z>30) elements. Only elements with strong lines, namely Y and Ba, were detected. Correlations of relative abundances of chemical elements with condensation temperatures and second ionization potentials of these elements, which can be explained by the accretion of dust and gas, were found.2013AJ....145..167Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/145/167CatalogResearchIsServedByTAP VizieR generic servicerelated-toVI/69 : Atomic Spectral Line List (Hirata+ 1995)J/AJ/144/35 : Abundances of the eclipsing binary ZZ Boo (Kang+, 2012)J/ApJ/645/613 : Abundances of HD 221170 (Ivans+, 2006)J/PASP/118/636 : al. Per High res. spectral atlas at 3810-8100{AA} (Lee+, 2006)J/A+A/347/348 : Solar abundance of iron (Grevesse+, 1999)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/145/167https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/145/167http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/145/167https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/145/167https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/145/167http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/145/167GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/AJ/145/167/table1Iron lines in the spectrum of LX PerMMean abundance for this elementmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonIron line identifier (Fe I or Fe II)phys.atmol.ionStagecharlambda[4515/8946] Wavelength; in {AA}0.1nmem.wldoubleloggfLog of the oscillator strengthphys.atmol.oscStrengthfloatr_loggfReference for loggf; in refs.dat filemeta.ref;pos.framecharElowLower excitation energy leveleVphys.energy;phys.atmol.levelfloatEWh? Equivalent width of hot component (m{AA})0.1pmspect.line.eqWidthfloatnullableEWc? Equivalent width of cool component (m{AA})0.1pmspect.line.eqWidthfloatnullablelogNh? Hot component abundance (logN(H)=12)phys.abundfloatnullablelogNc? Cool component abundance (logN(H)=12)phys.abundfloatnullableJ/AJ/145/167/linesLines of non-iron elements in the spectrum of LX Per (tables 5 and 6)IonElemental line identificationphys.atmol.ionStagecharCmeta.code.multipcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[4497/9238] Line wavelength; in {AA}0.1nmem.wl;spect.linedoubleloggfLog of the oscillator strengthphys.atmol.oscStrengthfloatElowExcitation energy of lower leveleVphys.energy;phys.atmol.levelfloatlogNDerived abundance in LX Per (H=12)phys.abundfloatlogNo? Derived abundance in the Sun (H=12)phys.abundfloatnullableAbunLX Per abundance relative to the Sunlog(Sun)phys.abundfloatBl[0/1] Blending in LX Per (1=clean line)meta.notefloatBlo[0/1]? Blending in the Sun (1=clean line)meta.notefloatnullableD[0/1] LX Per depth in synthetic spectrumphot.flux.density;arith.ratiofloatDo[0/1]? Solar depth in synthetic spectrumphot.flux.density;arith.ratiofloatnullablee(g)LX Per error in abundance for a change in logg of +0.2dexstat.errorfloate(T)LX Per error in abundance for a change in effective temperature of +100Kstat.errorfloatf_loggf[h] Flag on loggf (h) (1)meta.codecharr_loggfReference for loggf; in refs.dat filemeta.ref;pos.framecharMMean abundance for this elementmeta.ref.urlcharJ/AJ/145/167/table7Mean abundances of chemical elements in the atmosphere of LX PerrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintC[ch] Component (h=hotter, c=cooler)meta.code.multipcharZ[3/56]? Atomic numbermeta.id;meta.mainintnullableIonName of ionphys.atmol.ionStagecharNL[1/72] Number of spectral lines usedmeta.numberintLinesDetails of lines observed for this elementmeta.ref.urlcharAbestBest value mean abundance (LX Per minus Solar)log(Sun)phys.abundfloate_Abest? Uncertainty in Ab-bestlog(Sun)stat.errorfloatnullableAg+0.2Mean abundance (LX Per minus Solar) with surface gravity shifted by +0.2cm/s^2^log(Sun)phys.abundfloate_Ag+0.2? Uncertainty in Ag+0.2log(Sun)stat.errorfloatnullableA+100KMean abundance (LX Per minus Solar) with effective temperature altered by +100Klog(Sun)phys.abundfloate_A+100K? Uncertainty in A+100Klog(Sun)stat.errorfloatnullableNbestBest value of LX Per absolute mean abundance log(N/H)+12phys.abundfloate_Nbest? Uncertainty in N-beststat.errorfloatnullableNg+0.2Absolute mean abundance of LX Per with surface gravity shifted by +0.2cm/s^2^phys.abundfloate_Ng+0.2? Uncertainty in N+0.2stat.errorfloatnullableN+100KAbsolute mean abundance (log(N/H)+12) of LX Per with effective temperature altered by +100Kphys.abundfloate_N+100K? Uncertainty in N+100Kstat.errorfloatnullableJ/AJ/145/167/refsReferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRef[1/27] Reference numbermeta.id;meta.mainintBibCodeBibliographic codemeta.bib.bibcodecharAutAuthors's namemeta.bib.authorcharComCommentsmeta.notechar