J/PASP/124/401ivo://CDS.VizieR/J/PASP/124/401doi:10.26093/cds/vizier.61240401CDSKim C.Yushchenko A.V.Kim S.-L.Jeon Y.-B.Kim C.-H.2025-09-09T14:14:20Z2013-04-26T13:26:51ZCDS support team

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

cds-question@unistra.frvariable-starschemical-abundancesHigh-resolution spectroscopic observation was carried out to find the chemical composition of BE Lyn. The abundances of 25 chemical elements from carbon to neodymium were found. The deficiency of iron appeared to be equal to {DELTA}logN(Fe)=-0.26+/-0.08 with respect to the solar metallicity, and the abundances of other elements were mainly undersolar. Only nitrogen, sodium, aluminium, and sulfur showed overabundances near 0.2-0.3dex. The abundance pattern showed no clear signs of accretion or mass transfer events. It is not possible to exclude the classification of BE Lyn as a SX Phe-type star with slightly undersolar abundances of chemical elements. In addition, new differential time-series observations of BE Lyn were secured using V filters, and seven new times of light maximum were identified. We collected 162 times of light maximum from the literature, unpublished data, and an open database, and we proceeded to investigate the pulsational properties of BE Lyn. All five harmonic frequencies were identified using the Fourier decomposition method.2012PASP..124..401Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/PASP/124/401CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/PASP/124/401https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/PASP/124/401http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/PASP/124/401https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/PASP/124/401https://vizier.iucaa.in/viz-bin/votable?-source=J/PASP/124/401http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/PASP/124/401GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/PASP/124/401/table1Iron Lines in Spectrum of BE LynrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelength0.1nmem.wldoubleIonIon (Fe I or Fe II)phys.atmol.ionStagecharloggfOscillator strengthphys.atmol.oscStrengthfloatElowEnergy of low leveleVphys.energy;phys.atmol.levelfloatEWEquivalent width (in m{AA})0.1pmspect.line.eqWidthintlogNIron abundance (in the scale of logN(H)=12)phys.abundfloatJ/PASP/124/401/table2Lines of chemical elements in spectrum of BE Lyn (except iron)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonIon numerial code (FeI=26.00)phys.atmol.ionStagefloatlambdaWavelength0.1nmem.wldoubleloggfOscillator strengthphys.atmol.oscStrengthfloatr_loggfReference for loggf, in refs.dat filemeta.ref;pos.frameintElowExcitation potentialeVphys.atmol.excitationfloatDlogNDifferential abundance, Be Lyn - Sun (in the scale of logN(H)=12)phys.abundfloatlogN*BE Lyn abundance (in the scale of logN(H)=12)phys.abundfloatlogNS? Sun abundance (in the scale of logN(H)=12)phys.abundfloatnullableBl*? Be Lyn level of blending of the line in the synthetic spectra (1 = clean line, 0.0 = strong blended line)meta.codefloatnullablen_Bl*[h] h for hfs: hyperfine splittingmeta.notecharBlS? Sun level blending of the line in the synthetic spectra (1 = clean line, 0.0 = strong blended line)meta.codefloatnullablen_BlS[h] h for hfs: hyperfine splittingmeta.notecharD*BE Lyn depth of the line in synthetic spectraphot.flux.density;arith.ratiofloatDS? Sun depth of the line in synthetic spectraphot.flux.density;arith.ratiofloatnullabledA(T)Correction for abundance, by an effective temperature decrease of 200Karith.factorfloatdA(g)Correction for abundance, by a gravity increase of 0.3dexarith.factorfloatdA(vt)Correction for abundance, by a microturbulent velocity increase of 0.5km/sarith.factorfloatDDepth of the line in convoluted synthetic spectraphot.flux.density;arith.ratiofloatdD1Correction to the best depth of the line in the synthetic spectrum found by changing the abundance of the investigated chemical element by -0.5dexarith.factorfloatdD2Correction to the best depth of the line in the synthetic spectrum found by changing the abundance of the investigated chemical element by +0.5dexarith.factorfloatJ/PASP/124/401/refsReferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference numbermeta.id;meta.mainintComReferencemeta.ref;pos.framecharJ/PASP/124/401/table3Mean abundances of chemical elements in atmosphere of BE LynrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintZAtomic numbermeta.id;meta.mainintIonIonphys.atmol.ionStagecharnNumber of line usedmeta.numberintDlogNRelative abundance in BL Lyn atmosphere, best valuephys.abundfloate_DlogN? rms uncertainty on DlogNstat.errorfloatnullableDlogN1Relative abundance in BL Lyn atmosphere, effective temperature increased by 100Kphys.abundfloate_DlogN1? rms uncertainty on DlogN1stat.errorfloatnullableDlogN2Relative abundance in BL Lyn atmosphere, surface gravity decreased by 0.3dexphys.abundfloate_DlogN2? rms uncertainty on DlogN2stat.errorfloatnullableDlogN3Relative abundance in BL Lyn atmosphere, microturbulent velocity increased by 0.5km/sphys.abundfloate_DlogN3? rms uncertainty on DlogN3stat.errorfloatnullablelogNAbsolute abundance in BL Lyn atmosphere, best valuephys.abundfloate_logN? rms uncertainty on logNstat.errorfloatnullablelogN1Absolute abundance in BL Lyn atmosphere, effective temperature increased by 100Kphys.abundfloate_logN1? rms uncertainty on logN1stat.errorfloatnullablelogN2Absolute abundance in BL Lyn atmosphere, surface gravity decreased by 0.3dexphys.abundfloate_logN2? rms uncertainty on logN2stat.errorfloatnullablelogN3Absolute abundance in BL Lyn atmosphere, microturbulent velocity increased by 0.5km/sphys.abundfloate_logN3? rms uncertainty on logN3stat.errorfloatnullable