J/AJ/114/341ivo://CDS.VizieR/J/AJ/114/341doi:10.26093/cds/vizier.51140341CDSGonzalez G.Lambert D.L.2023-04-06T16:50:27Z1998-03-15T15:28:31ZCDS support team

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

cds-question@unistra.frglobular-star-clustersvariable-starschemical-abundancesWe have determined the photospheric compositions of five luminous F-G variables in globular clusters: V11 in M2, V42 in M5, V84 in M5, V2 in M10, and V17 in M28, three of which are classified as RV Tau variable stars. Unlike the recent findings that the photospheres of field RV Tau variables have been altered by a gas-dust separation process, none of these stars, except possibly V2 in M10, show such signs. We suggest that either a smaller carbon abundance in the photosphere of a globular cluster RV Tau star (compared to its field analogues) might be a factor in the gas-dust separation process due to the lack of sufficient carbon grain formation, or the stellar winds and their efficacy as dust-grain separators is influenced by the metallicity of the stellar envelope which, unlike the photosphere, is never subject to alteration by a dust-gas separation. Our analysis is most complete for V84, for which we have estimated the abundances of 19 chemical elements. Compared to the other giants in M5, this star displays a very large excess of Na and a deficit of O. This finding is consistent with a recently proposed mechanism of Na production in the ON-cycling region of metal-poor RGB stars. The value of [Al/Fe] for V84 is also high (also consistent with ON-cycling), but a comparison with the other cluster giants cannot be performed until Al is measured in their spectra. The s-process elements are not significantly enhanced in the atmosphere of V84 relative to the other cluster members. (c) 1997 American Astronomical Society.1997AJ....114..341Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/114/341CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/114/341https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/114/341http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/114/341https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/114/341https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/114/341http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/114/341GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/AJ/114/341/tablesIndividual abundance results using the model atmospheres in Table 1recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintObjectObject designation (1)meta.id;meta.maincharSpeciesIon speciesphys.atmol.elementcharLambdaWavelength0.1nmem.wlfloatEPLow energy potentialeVphys.energy;phys.atmol.levelfloatlog(gf)Oscillator strengthphys.atmol.wOscStrengthfloatDate1Observation date (2)time.epochnullableEW1? Equivalent width for Date10.0001nmspect.line.eqWidthintnullablelog(e1)? Mean number density abundance relative to H for Date1phys.abundfloatnullableDate2Observation date (2)time.epochnullablel_EW2limit flag for EW2meta.code.errorcharEW2? Equivalent width for Date20.0001nmspect.line.eqWidthintnullablel_log(e2)limit flag for E2meta.code.errorcharlog(e2)? Mean number density abundance relative to H for Date2phys.abundfloatnullableDate3Observation date (2)time.epochnullableEW3? Equivalent width for Date30.0001nmspect.line.eqWidthintnullablelog(e3)? Mean number density abundance relative to H for Date3phys.abundfloatnullable