J/A+AS/103/97ivo://CDS.VizieR/J/A+AS/103/97CDSMeynet G.Maeder A.Schaller G.Schaerer D.Charbonnel C.2017-07-12T06:59:54Z1999-02-26T15:19:22ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelsstellar-mass-losshertzsprung-russell-diagramMost outputs of massive star evolution critically depend on the mass loss rates. In order to broaden the comparison basis and to illustrate the effects of different mass loss rates, we have computed new sets of models, with initial masses between 12 and 120 M{sun}, and metallicities, Z, between 0.001 and 0.040, with a mass loss rate increased by a factor of two during the phases when the stellar winds are believed to be essentially driven by the radiation pressure. A moderate core-overshooting and the new radiative opacities from Iglesias et al. (1992ApJ...397..717I) and Kurucz (1991) were taken into account. These models complete the homogeneous and extended theoretical database formed by the previous grids of this series, computed by Schaller et al. (1992, Cat. J/A+AS/96/269) for Z=0.020 and Z=0.001, by Schaerer et al. (1992, Cat. J/A+AS/98/523; 1993, Cat. J/A+AS/102/339) for Z=0.008 and Z=0.040 and by Charbonnel et al. (1993, Cat. J/A+AS/101/415) for Z=0.004. This paper closes this series. Of particular interest is the predicted behaviour of metal rich stars such as may be found in the inner regions of our Galaxy. New evolutionary connexions are found, in particular we show that the most massive and metal rich stars may spend a relatively long time as He and N enriched stars and may even end their evolution as white dwarfs.1994A&AS..103...97Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+AS/103/97CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+AS/103/97https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+AS/103/97http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+AS/103/97https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+AS/103/97https://vizier.iucaa.in/viz-bin/votable?-source=J/A+AS/103/97http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+AS/103/97GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+AS/103/97/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.massfloatnullableZoStar initial metallicity: 0.001 or 0.020phys.abund.ZfloatnullableMdSimbad column added by the CDSmeta.noteintnullableNBnumber of selected pointmeta.numberintAgeageyrtime.agedoubleMassactual mass in solar massessolMassphys.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)arith.zpfloatlog(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