J/A+AS/102/339ivo://CDS.VizieR/J/A+AS/102/339CDSSchaerer D.Charbonnel C.Meynet G.Maeder A.Schaller G.2022-05-25T09:10:39Z2011-10-09T12:27:47ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelsstellar-mass-losshertzsprung-russell-diagramThe present grid of evolutionary sequences at metallicity Z=0.040, completes the set of grids computed for Z=0.020 and 0.001 by Schaller et al. (1992, Cat. J/A+AS/96/269), Z=0.008 by Schaerer et al. (1992, Cat. J/A+AS/98/523) and Z=0.004 by Charbonnel et al. (1993, Cat. J/A+AS/101/415). The models with mass loss and moderate core overshooting have been computed for 0.8 to 120 M{sun} using up-to-date input physics and the new radiative opacities from Iglesias et al. (1992ApJ...397..717I) and Kurucz (1991).1993A&AS..102..339Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+AS/102/339CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+AS/102/339https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+AS/102/339http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+AS/102/339https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+AS/102/339https://vizier.iucaa.in/viz-bin/votable?-source=J/A+AS/102/339http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+AS/102/339GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+AS/102/339/modelsCombined table from original tablesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTnoNumber of table in the publicationmeta.id;meta.datasetcharMoStar initial masssolMassphys.massfloatZoStar initial metallicity: 0.001 or 0.020phys.abund.ZfloatOmeta.notecharMdmeta.noteintNBnumber of selected pointmeta.numberintAgeageyrtime.agedoubleMassactual mass in solar massesSunphys.massdoublelogLlog(luminosity) in solar unitslog(solLum)phys.luminosityfloatlogTelog(effective temperature)log(K)phys.temperature.effectivefloatXH surface abundance (mass fraction)phys.abund.FedoubleYHe surface abundance (mass fraction)phys.abund.YdoubleC1212C surface abundance (mass fraction)meta.notedoubleC1313C surface abundance (mass fraction)meta.notedoubleN1414N surface abundance (mass fraction)meta.notedoubleO1616O surface abundance (mass fraction)meta.notedoubleO1717O surface abundance (mass fraction)meta.notedoubleO1818O surface abundance (mass fraction)meta.notedoubleNe2020Ne surface abundance (mass fraction)meta.notedoubleNe2222Ne surface abundance (mass fraction)meta.notedoubleQCCcore mass fractionphys.massfloatlogTu? log(uncorrected Teff) (WR stars only)log(K)arith.zpfloatnullablelogMdotlog(mass loss rate)log(solMass.yr**-1)phys.mass.lossfloatlog(rho.c)log(central density)log(g.cm**-3)arith.zpfloatlogTclog(central temperature)log(K)arith.zpfloatXcH central abundance (mass fraction)phys.abund.FedoubleYcHe central abundance (mass fraction)phys.abund.YdoubleC12c12C central abundance (mass fraction)phys.abund;em.wl.centraldoubleC13c13C central abundance (mass fraction)phys.abund;em.wl.centraldoubleN14c14N central abundance (mass fraction)phys.abund;em.wl.centraldoubleO16c16O central abundance (mass fraction)phys.abund;em.wl.centraldoubleO17c17O central abundance (mass fraction)phys.abund;em.wl.centraldoubleO18c18O central abundance (mass fraction)phys.abund;em.wl.centraldoubleNe20c20Ne central abundance (mass fraction)phys.abund;em.wl.centraldoubleNe22c22Ne central abundance (mass fraction)phys.abund;em.wl.centraldouble