J/A+A/553/A24ivo://CDS.VizieR/J/A+A/553/A24doi:10.26093/cds/vizier.35530024CDSGeorgy C.Ekstrom S.Granada A.Meynet G.Mowlavi N.Eggenberger P.,Maeder A.2013-04-25T15:53:12Z2013-04-25T08:29:06ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelsbe-starsstellar-mass-lossB-type stars are known to rotate at various velocities, including very fast rotators near the critical velocity as the Be stars. In this paper, we provide stellar models covering the mass range between 1.7 to 15M_{sun}_, which includes the typical mass of known Be stars, at Z=0.014, 0.006 and 0.002 and for an extended range of initial velocities on the zero-age main sequence. We use the Geneva stellar-evolution code including the effects of shellular rotation and with a numerical treatment that has been improved in order for the code to track in a precise way the variation of the angular momentum content of the star as it changes under the influence of radiative winds and/or mechanical mass loss. We discuss the impact of the initial rotation rate on the tracks in the Hertzsprung-Russell diagram, the main-sequence (MS) lifetimes, the evolution of the surface rotation and abundances, as well as on the ejected masses of various isotopes. Among the new results obtained from the present grid we have that: 1) fast rotating stars with initial masses around 1.7M_{sun}_ present at the beginning of the core hydrogen-burning phase quite small convective cores with respect to their slowly rotating counterparts. This fact may be interesting to keep in mind in the frame of the asteroseismic studies of such stars; 2) the contrast between the core and surface angular velocity is higher in slower rotating stars. The values presently obtained are quite in the range of the very few values obtained for B-type stars from asteroseismology; 3) at Z=0.002, the stars in the mass range of 1.7 to 3M_{sun}_ with a mean velocity on the MS of the order of 150km/s show N/H enhancement superior to 0.2dex at mid-MS, and superior to 0.4dex at the end of the MS phase. At solar metallicity the corresponding values are below 0.2dex at any time in the MS. An extended database of stellar models containing 270 evolutionary tracks is provided to the community.2013A&A...553A..24Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/553/A24CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/291/155 : Rotating neutron stars models .I. (Salgado+, 1994)J/A+AS/108/455 : Rotating neutron stars models. II. (Salgado+, 1994)J/A+A/346/586 : Rotating models of A and F stars (Perez Hernandez+, 1999)J/A+A/530/A115 : Rotating massive MS stars evolutionary models (Brott+, 2011)J/A+A/537/A146 : Stellar models with rotation. 0.8<M<120, Z=0.014https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/553/A24https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/553/A24http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/553/A24https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/553/A24https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/553/A24http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/553/A24GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/553/A24/modelsEvolutionary tracks for 270 combinations of initial M, Z and Omega/omega_critrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMiniInitial mass (1)solMassphys.massfloattrackEvolutionary track for this mass and OOcmeta.ref.urlcharZiniInitial Z abundance (1)phys.atmol.initialfloatOOciniOmega/omega_crit value (1)stat.fit.paramfloatLineNumber of selected pointmeta.idintTimeAgeyrtime.agedoubleMassActual mass in solar massessolMassphys.massfloatlogLlog(luminosity) in solar unitslog(solLum)phys.luminosityfloatlogTelog(effective temperature)log(K)phys.temperature.effectivefloatXH 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.massfloatlogTulog(uncorrected Teff) (WR stars only)log(K)arith.zpfloatlogdM/dtlog(mass loss rate)log(solMass.yr**-1)phys.mass.lossdoublelog(rhoc)log(central density)log(g.cm**-3)arith.zpfloatlogTclog(central temperature)log(K)arith.zpfloatXcH 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 velocitys**-1phys.veloc.angdoubleOmegacCentral angular velocitys**-1phys.veloc.angdoubleRpReOblatenessphys.size;arith.ratiodoubledM/dtRRotational dM/dt correction factorphys.mass.lossfloatvcrit1First critical velocity (Omega-limit)km/sphys.velocdoublevcrit2Second critical velocity (OmegaGamma-limit)km/sphys.velocdoubleveqEquatorial velocitykm/sphys.veloc.rotatdoubleOOcOmega_surf/Omega_critstat.fit.paramdoubleGeddEddington factorphys.luminosity;arith.ratiodoubledM/dtmMechanical equatorial dM/dtsolMass/yrphys.mass.lossdoubleLtotTotal angular momentum1e+53g.cm**2.s**-1phys.angMomentumdouble