J/A+AS/96/269ivo://CDS.VizieR/J/A+AS/96/269CDSSchaller G.Schaerer D.Meynet G.Maeder A.2017-07-11T13:08:51Z1999-02-27T12:33:32ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelsstellar-mass-losssupergiant-starswolf-rayet-starsNew grids of stellar evolutionary models covering the range of 0.8 to 120 solar masses have been computed for metallicites Z=0.020 and Z=0.001. The models use the new opacities by Rogers and Iglesias (1992ApJS...79..507R) and by Kurucz (1991) at low T. The consequent changes in the solar helium content, in the mixing length ratio and in the overshooting parameter are taken into account after careful calibrations. Important physical ingredients as the nuclear reaction rates and the neutrino loss rates have been updated. The ionization of the main heavy elements is calculated in details. Results of the models are given in a compact way at corresponding evolutionary stages in each model. In addition to the tables, we shortly present some general results on the tracks in the HR diagrams, the lifetimes in the H-, He-, C-burning phases, and on massive and WR stars.1992A&AS...96..269Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+AS/96/269CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+AS/96/269https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+AS/96/269http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+AS/96/269https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+AS/96/269https://vizier.iucaa.in/viz-bin/votable?-source=J/A+AS/96/269http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+AS/96/269GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+AS/96/269/modelsCombined table from original tablesMoStar initial masssolMassphys.massfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTnoNumber of table in the publicationmeta.id;meta.datasetcharZoStar initial metallicity: 0.001 or 0.020phys.abund.ZfloatnullableOSimbad column added by the CDSmeta.notecharMdSimbad 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.YdoubleC12^12^C surface abundance (mass fraction)meta.notedoubleC13^13^C surface abundance (mass fraction)meta.notedoubleN14^14^N surface abundance (mass fraction)meta.notedoubleO16^16^O surface abundance (mass fraction)meta.notedoubleO17^17^O surface abundance (mass fraction)meta.notedoubleO18^18^O surface abundance (mass fraction)meta.notedoubleNe20^20^Ne surface abundance (mass fraction)meta.notedoubleNe22^22^Ne 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.YdoubleC12c^12^C central abundance (mass fraction)phys.abund;em.wl.centraldoubleC13c^13^C central abundance (mass fraction)phys.abund;em.wl.centraldoubleN14c^14^N central abundance (mass fraction)phys.abund;em.wl.centraldoubleO16c^16^O central abundance (mass fraction)phys.abund;em.wl.centraldoubleO17c^17^O central abundance (mass fraction)phys.abund;em.wl.centraldoubleO18c^18^O central abundance (mass fraction)phys.abund;em.wl.centraldoubleNe20c^20^Ne central abundance (mass fraction)phys.abund;em.wl.centraldoubleNe22c^22^Ne central abundance (mass fraction)phys.abund;em.wl.centraldouble