J/A+A/537/A146ivo://CDS.VizieR/J/A+A/537/A146doi:10.26093/cds/vizier.35370146CDSEkstrom S.Georgy C.Eggenberger P.Meynet G.Mowlavi N.,Wyttenbach A.Granada A.Decressin T.Hirschi R.Frischknecht U.,Charbonnel C.Maeder A.2012-04-03T12:38:45Z2012-01-26T08:53:37ZCDS 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-starsMany topical astrophysical research areas, such as the properties of planet host stars, the nature of the progenitors of different types of supernovae and gamma ray bursts, and the evolution of galaxies, require complete and homogeneous sets of stellar models at different metallicities in order to be studied during the whole of cosmic history. We present here a first set of models for solar metallicity, where the effects of rotation are accounted for in a homogeneous way. We computed a grid of 48 different stellar evolutionary tracks, both rotating and non-rotating, at Z=0.014, spanning a wide mass range from 0.8 to 120M_{sun}_. For each of the stellar masses considered, electronic tables provide data for 400 stages along the evolutionary track and at each stage, a set of 43 physical data are given. These grids thus provide an extensive and detailed data basis for comparisons with the observations. The rotating models start on the ZAMS with a rotation rate v_ini_/v_crit_=0.4. The evolution is computed until the end of the central carbon-burning phase, the early AGB phase, or the core helium-flash for, respectively, the massive, intermediate, and both low and very low mass stars. The initial abundances are those deduced by Asplund et collaborators, which best fit the observed abundances of massive stars in the solar neighbourhood. We update both the opacities and nuclear reaction rates, and introduce new prescriptions for the mass-loss rates as stars approach the Eddington and/or the critical velocity. We account for both atomic diffusion and magnetic braking in our low-mass star models. The present rotating models provide a good description of the average evolution of non-interacting stars. In particular, they reproduce the observed MS width, the positions of the red giant and supergiant stars in the HR diagram, the observed surface compositions and rotational velocities. Very interestingly, the enhancement of the mass loss during the RSG stage, when the luminosity becomes supra-Eddington in some outer layers, help models above 15-20 Msun to lose a significant part of their hydrogen envelope and evolve back into the blue part of the HR diagram. This result has interesting consequences for the blue to red supergiant ratio, the minimum mass for stars to become WR stars, and the maximum initial mass of stars that explode as type II-P supernovae.2012A&A...537A.146Ehttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/537/A146CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/508/355 : Scaled solar tracks and isochrones (Bertelli+, 2009)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/537/A146https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/537/A146http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/537/A146https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/537/A146https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/537/A146http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/537/A146GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/537/A146/tablesEvolutionary tracksrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMiniInitial masssolMassphys.massfloattrackEvolutionary trask for this massmeta.ref.urlcharZini[0.014] Initial metallicityphys.abund.ZfloatRot[nr] r for rotation, n for no rotationmeta.codecharLine[1/400] Number of selected pointmeta.idintTimeAgeyrtime.agedoubleMassActual masssolMassphys.massfloatlogLLuminosity in log scalelog(solLum)phys.luminosityfloatlogTeEffective temperature in log scalelog(K)phys.temperature.effective;instr.scalefloatXH surface abundance (mass fraction)phys.abund.FefloatYHe surface abundance (mass fraction)phys.abund.YfloatC1212C 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.notedoubleAl2626Al surface abundance (mass fraction)phys.abunddoubleQCCConvective core mass fractionphys.massfloatlogTe.uUncorrected effective temperature in log scale (WR stars only)log(K)phys.temperature.effectivefloatlogdM/dtMass loss rate in log scalelog(solMass.yr**-1)phys.mass.lossdoublelog(rhoc)Central density in log scalelog(g.cm**-3)instr.scalefloatlogTcCentral temperature in log scalelog(K)instr.scalefloatXcH central abundance (mass fraction)phys.abund.FefloatYc4He central abundance (mass fraction)phys.abund;em.wl.centralfloatC12c12C 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.centraldoubleAl26c26Al central abundance (mass fraction)phys.abunddoubleOmegasSurface angular velocity {Omega}_s_rad/sphys.veloc.angdoubleOmegacCentral angular velocity {Omega}_c_rad/sphys.veloc.angdoubleoblat[0/1] Oblateness (R_pol_/R_eq_)phys.size;arith.ratiofloatdM/dtRRotational dM/dt correction factorphys.mass.lossfloatvcrit1First critical velocity ({Omega}-limit)km/sphys.velocdoublevcrit2Second critical velocity ({Omega}{Gamma}-limit)km/sphys.velocdoubleveqEquatorial velocitykm/sphys.veloc.rotatdoubleOOc[0/1] {Omega}_surf_/{Omega}_crit_stat.fit.paramdoubleGedd[0/1] Eddington factor {Gamma}phys.luminosity;arith.ratiodoubledM/dtmMechanical equatorial mass loss dM/dtsolMass/yrphys.mass.lossdoubleLtotTotal angular momentum1e+53g.cm**2.s**-1phys.angMomentumdoubleJ/A+A/537/A146/isoIsochrnonesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogAgeInitial agelog(yr)time.agefloatisoIsochrone for this agemeta.ref.urlcharRot[nr] r for rotation, n for no rotationmeta.codecharMiniInitial masssolMassphys.massfloatZini[0.014] Initial metallicityphys.abund.ZfloatOOcini[0,0.4] Initial {Omega}_surf_/{Omega}_crit_stat.fit.paramfloatMassActual mass at the age of the isochronesolMassphys.massfloatlogLLuminosity in log scalelog(solLum)phys.luminosityfloatlogTeEffective temperature in log scalelog(K)phys.temperature.effective;instr.scalefloatlogTe.ncEffective temperature not corrected for the thickness of the wind (WR) in log scalelog(K)phys.temperature.effectivefloatMbolBolometric magnitudemagphys.magAbs.bolfloatVmagV-band absolute magnitudemagphot.mag;em.opt.VfloatU-BU-B colour indexmagphot.color;em.opt.U;em.opt.BfloatB-VB-V colour indexmagphot.color;em.opt.B;em.opt.VfloatB2-V1B2-V1 colour indexmagphot.magfloatRpolPolar radiuscmphys.angSize;srcdoubleoblatOblateness (R_pol_/R_eq_)phys.size;arith.ratiofloatloggPolar effective surface gravity in log scalelog(cm.s**-2)instr.scalefloatOmsSurface angular velocity {Omega}_s_rad/ssrc.densitydoubleVeqEquatorial velocitykm/sphys.veloc;pos.eqdoublevcrit1Critical velocity ({Omega}-limit)km/sphys.velocdoublevcrit2Critical velocity ({Gamma}{Omega}-limit)km/sphys.velocdoubleOOcActual {Omega}_surf_/{Omega}_crit_stat.fit.paramfloatlogdM/dtrRadiative mass loss in log scalelog(solMass.yr**-1)phys.mass.lossdoublelogdM/dtmMechanical mass loss in log scalelog(solMass.yr**-1)phys.mass.lossdoubleGeddEddington factor {Gamma}phys.luminosity;arith.ratiofloatH1H surface abundance (mass fraction)phys.abunddoubleHe44He surface abundance (mass fraction)phys.abunddoubleC1212C 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.notedoubleAl2626Al surface abundance (mass fraction)phys.abunddouble