J/A+AS/98/523ivo://CDS.VizieR/J/A+AS/98/523CDSSchaerer D.Meynet G.Maeder A.Schaller G.2017-07-11T13:08:19Z2011-10-09T11:57:53ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelsstellar-mass-lossmagellanic-cloudsContinuing the effort to provide a homogeneous base of extensive and accurate grids of stellar models covering a wide range of metallicities we present a new grid of stellar models at metallicity Z = 0.008, roughly corresponding to the Large Magellanic Cloud composition. The models have been computed for 0.8 to 120 solar masses, using up-to-date input physics and the new radiative opacities from Rogers and Iglesias (1992ApJS...79..507R) and Kurucz (1991). Mass loss and moderate core overshooting are taken into account. The resulting HR diagram and the lifetimes in the H-, He-, and C-burning phases as well as some general results on massive stars are discussed and compared with complementary grids, using the same input physics at metallicities Z of 0.020 and 0.001 used by Schaller et al. (1992, Cat. J/A+AS/96/269)1993A&AS...98..523Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+AS/98/523CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+AS/98/523https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+AS/98/523http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+AS/98/523https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+AS/98/523https://vizier.iucaa.in/viz-bin/votable?-source=J/A+AS/98/523http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+AS/98/523GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+AS/98/523/modelsCombined table from original tablesNe20c20Ne central abundance (mass fraction)phys.abund;em.wl.centraldoubleNe22c22Ne central abundance (mass fraction)phys.abund;em.wl.centraldoublerecnoRecord 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.ZfloatnullableOSimbad column added by the CDSmeta.notecharMdSimbad column added by the CDSmeta.noteintnullableNBnumber of selected pointmeta.numberintAgeageyrtime.agedoubleMassactual mass in solar masseslog(solMass)phys.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(Sun.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.centraldouble