J/ApJ/764/21ivo://CDS.VizieR/J/ApJ/764/21doi:10.26093/cds/vizier.17640021CDSChieffi A.Limongi M.2014-12-04T15:01:37Z2014-11-17T11:35:30ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelssupernovaestellar-massesWe present the first set of a new generation of models of massive stars with a solar composition extending between 13 and 120M_{sun}_, computed with and without the effects of rotation. We included two instabilities induced by rotation: the meridional circulation and the shear instability. We implemented two alternative schemes to treat the transport of the angular momentum: the advection-diffusion formalism and the simpler purely diffusive one. The full evolution from the pre-main sequence up to the pre-supernova stage is followed in detail with a very extended nuclear network. The explosive yields are provided for a variety of possible mass cuts and are available at the Web site http://www.iasf-roma.inaf.it/orfeo/public_html. We find that both the He and the CO core masses are larger than those of their non-rotating counterparts. Also the C abundance left by the He burning is lower than in the non-rotating case, especially for stars with an initial mass of 13-25M_{sun}_, and this affects the final mass-radius relation, basically the final binding energy, at the pre-supernova stage. The elemental yields produced by a generation of stars rotating initially at 300km/s do not change substantially with respect to those produced by a generation of non-rotating massive stars, the main differences being a slight overproduction of the weak s-component and a larger production of F. Since rotation also affects the mass-loss rate, either directly or indirectly, we find substantial differences in the lifetimes as O-type and Wolf-Rayet subtypes between the rotating and non-rotating models. The maximum mass exploding as Type IIP supernova ranges between 15 and 20M _{sun}_ in both sets of models (this value depends basically on the larger mass-loss rates in the red supergiant phase due to the inclusion of the dust-driven wind). This limiting value is in remarkably good agreement with current estimates.2013ApJ...764...21Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/764/21CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/558/A131 : Model spectra of hot stars at the pre-SN stage (Groh+, 2013)J/A+A/558/A103 : Stellar models with rotation, Z=0.002 (Georgy+, 2013)J/A+A/553/A24 : Models for rotating stars (Georgy+, 2013)J/ApJS/199/38 : Presupernova evolution (Limongi+, 2012)J/A+A/537/A146 : Stellar models with rotation, Z=0.014 (Ekstrom+, 2012)J/A+A/530/A115 : Rotating massive MS stars evolutionary models (Brott+, 2011)J/A+A/496/841 : VLT-FLAMES survey of massive stars (Hunter+, 2009)J/A+A/479/541 : VLT-FLAMES survey of massive stars (Hunter+, 2008)J/A+A/471/625 : VLT-FLAMES survey of massive stars (Trundle+, 2007)J/A+A/466/277 : VLT-FLAMES survey of massive stars (Hunter+, 2007)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/764/21https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/764/21http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/764/21https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/764/21https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/764/21http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/764/21GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/764/21/table1*Main evolutionary properties of the rotating modelsN/CN/C surface ratiophys.abunddoubleN/ON/O surface ratiophys.abunddoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMini[13/120] Initial masssolMassphys.massintPhaseEvolutionary phase (H, He, C, Ne, O, Si, PSN)meta.id;stat.fitcharTimeLifetime on Phaseyrtime.agedoubleMCC[0/93]? Mass size of the convective coresolMassphys.massfloatnullableTeff[3.5/5.4] log of average effective temperaturelog(K)phys.temperature.effective;stat.meanfloatlogL[4.5/6.3] log of average luminositylog(solLum)phys.luminosityfloatMass[7.3/53] Total masssolMassphys.massfloatMHe[0/46] He core masssolMassphys.massfloatMCO[0/25] CO core masssolMassphys.massfloatHsup[0/0.8] Surface abundance of H in mass fraction H_sup_phys.abunddoubleHesup[0.2/1] Surface abundance of He in mass fraction He_sup_phys.abunddoubleNsupSurface abundance of N in mass fraction N_sup_phys.abunddoubleVeq[0.03/228]? Equatorial velocity (only for table 1)km/sphys.veloc.rotatdoublenullableOms? Surface angular velocity {omega}_sup_ (only for table 1)s**-1phys.veloc.angdoublenullableO/Ocr[0.001/0.7]? Ratio of the surface angular velocity to the critical angular velocity {omega}/{omega}_c_ (only for table 1)stat.fit.paramdoublenullableJtot[0.01/0.7]? Total angular momentum J_tot_ (only for table 1)1e+53g.cm**2.s**-1phys.angMomentumdoublenullableJ/ApJ/764/21/table2Main evolutionary properties of the non-rotating modelsTimeLifetime on Phaseyrtime.agedoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMini[13/120] Initial masssolMassphys.massintPhaseEvolutionary phase (H, He, C, Ne, O, Si, PSN)meta.id;stat.fitcharMCC[0/93]? Mass size of the convective coresolMassphys.massfloatnullableTeff[3.5/5.4] log of average effective temperaturelog(K)phys.temperature.effective;stat.meanfloatlogL[4.5/6.3] log of average luminositylog(solLum)phys.luminosityfloatMass[7.3/53] Total masssolMassphys.massfloatMHe[0/46] He core masssolMassphys.massfloatMCO[0/25] CO core masssolMassphys.massfloatHsup[0/0.8] Surface abundance of H in mass fraction H_sup_phys.abunddoubleHesup[0.2/1] Surface abundance of He in mass fraction He_sup_phys.abunddoubleNsupSurface abundance of N in mass fraction N_sup_phys.abunddoubleN/CN/C surface ratiophys.abunddoubleN/ON/O surface ratiophys.abunddoubleJ/ApJ/764/21/table7Explosion properties and ejected masses of the rotating modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintModelModel parameter at 2.5e+4s after explosion (1)stat.paramM13Model value for Mini=13M_{sun}_solMassphys.massdoubleM15Model value for Mini=15M_{sun}_solMassphys.massdoubleM20Model value for Mini=20M_{sun}_solMassphys.massdoubleM25Model value for Mini=25M_{sun}_solMassphys.massdoubleM30Model value for Mini=30M_{sun}_solMassphys.massdoubleM40Model value for Mini=40M_{sun}_solMassphys.massdoubleM60Model value for Mini=60M_{sun}_solMassphys.massdoubleM80Model value for Mini=80M_{sun}_solMassphys.massdoubleM120Model value for Mini=120M_{sun}_solMassphys.massdoubleJ/ApJ/764/21/table8Explosion properties and ejected masses of the non rotating modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintModelModel parameter at 2.5e+4s after explosion (1)stat.paramM13Model value for Mini=13M_{sun}_solMassphys.massdoubleM15Model value for Mini=15M_{sun}_solMassphys.massdoubleM20Model value for Mini=20M_{sun}_solMassphys.massdoubleM25Model value for Mini=25M_{sun}_solMassphys.massdoubleM30Model value for Mini=30M_{sun}_solMassphys.massdoubleM40Model value for Mini=40M_{sun}_solMassphys.massdoubleM60Model value for Mini=60M_{sun}_solMassphys.massdoubleM80Model value for Mini=80M_{sun}_solMassphys.massdoubleM120Model value for Mini=120M_{sun}_solMassphys.massdouble