J/A+A/440/647ivo://CDS.VizieR/J/A+A/440/647doi:10.26093/cds/vizier.34400647CDSClaret A.2017-06-13T11:08:20Z2005-09-14T15:49:41ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelsNew stellar models spefically designed for the Small Magellanic Cloud are presented in this paper. In order to take into account the uncertainties in the metal content we computed two grids with different metallicities: Z=0.002 and Z=0.004. The covered mass range is from 0.8 up to 125M_{sun} and the models are followed until the exhaustion of carbon in the core, for the more massive ones. We have introduced a recent measurement of the nuclear rate ^14^N(p,{gamma})^15^O. A comparison among models with the old and new rate was carried out revealed that the former are slightly hotter than the first ones. Such differences depend on the mass range. The opacities, the equation of state, the remaining nuclear reactions rates, the core overshooting parameterization and the convective transport of energy are the same as discussed previously by us. We also give, besides the classical evolutionary models outputs, the internal structure constants needed to investigate apsidal motion and tidal evolution in close binaries. This aspect acquires importance in the light of recent investigations on circularization and synchronization levels in binary systems belonging to the Magellanic Clouds. The role of rotation can also be investigated through the gravity-darkening exponents which allow us to compute the brightness distribution of a given stellar surface.2005A&A...440..647Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/440/647CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/424/919 : New grids of stellar models - I. (Claret, 2004)J/A+A/453/769 : New grids of stellar models - III. (Claret, 2006)J/A+A/467/1389 : New grids of stellar models - IV. (Claret, 2007)J/A+AS/109/441 : Stellar models until He burning - I. (Claret, 1995)J/A+AS/114/549 : Stellar models until He burning - II. (Claret+, 1995)J/A+AS/125/439 : Stellar models until He burning - III. (Claret+, 1997)J/A+AS/133/123 : Stellar models until He burning - IV. (Claret+ 1998)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/440/647https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/440/647http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/440/647https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/440/647https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/440/647http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/440/647GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/440/647/gridSummary of parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintX[0.748,0.754] X initial X compositionfloatZ[0.002,0.004] Z initial compositionfloatMInitial masssolMassfloatnullablelogMInitial masslog(solMass)floatOv[0/1] 1 = with OvershootingintFileNameOriginal filename with result (in subdirectory)charHRPlot the Herzspring-Russel diagram for this masscharEvolutionDetails of evolution for this set of (X Z M) parameterscharJ/A+A/440/647/z002X=0.754, Z=0.002 models (log(M)=-0.0969 to 2.1000)Ov[0/1] Overshooting (1)intN14s14N surface abundance (mass fraction)doubleMg26s26Mg surface abundance (mass fraction)doublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogMInitial masslog(solMass)floatAgeAge of the modelsyrdoublelog(L)Log (Total luminosity)log(solLum)doublelog(g)Log (Surface gravity)log(cm.s**-2)doublelog(Teff)Log (Effective temperature)log(K)doubleMassActual mass of the modelsolMassdoublelogdM/dtLog (mass loss rate)log(solMass.yr**-1)doublelogDcLog (central density)log(g.cm**-3)doublelogTcLog (central temperature)log(K)doubleQcCore mass (fraction)doubleXcH central abundance (mass fraction)doubleXsH surface abundance (mass fraction)doubleYc4He central abundance (mass fraction)doubleYs4He surface abundance (mass fraction)doubleC12c12C central abundance (mass fraction)doubleC12s12C surface abundance (mass fraction)doubleC13c13C central abundance (mass fraction)doubleC13s13C surface abundance (mass fraction)doubleN14c14N central abundance (mass fraction)doubleO16c16O central abundance (mass fraction)doubleO16s16O surface abundance (mass fraction)doubleO17c17O central abundance (mass fraction)doubleO17s17O surface abundance (mass fraction)doubleO18c18O central abundance (mass fraction)doubleO18s18O surface abundance (mass fraction)doubleNe20c20Ne central abundance (mass fraction)doubleNe20s20Ne surface abundance (mass fraction)doubleNe22c22Ne central abundance (mass fraction)doubleNe22s22Ne surface abundance (mass fraction)doubleMg24c24Mg central abundance (mass fraction)doubleMg24s24Mg surface abundance (mass fraction)doubleMg25c25Mg central abundance (mass fraction)doubleMg25s25Mg surface abundance (mass fraction)doubleMg26c26Mg central abundance (mass fraction)doublelogK2Log(Apsidal motion constant (j=2))doublelogK3Log(Apsidal motion constant (j=3))doublelogK4Log(Apsidal motion constant (j=4))doubleXBFFractional depth of convective envelopedoublelogE2Log(Tidal torque constant)doubleECOPolytropic envelope characteristicdoublealphaPalphaP = -Ep x R/GM2doubleRgyrFractional gyration radiusdoublebeta1Gravity-darkening exponentdoubleJ/A+A/440/647/z004X=0.748, Z=0.004 models (log(M)=-0.0969 to 2.1000)AgeAge of the modelsyrdoublelog(L)Log (Total luminosity)log(solLum)doublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogMInitial masslog(solMass)floatOv[0/1] Overshooting (1)intlog(g)Log (Surface gravity)log(cm.s**-2)doublelog(Teff)Log (Effective temperature)log(K)doubleMassActual mass of the modelsolMassdoublelogdM/dtLog (mass loss rate)log(solMass.yr**-1)doublelogDcLog (central density)log(g.cm**-3)doublelogTcLog (central temperature)log(K)doubleQcCore mass (fraction)doubleXcH central abundance (mass fraction)doubleXsH surface abundance (mass fraction)doubleYc4He central abundance (mass fraction)doubleYs4He surface abundance (mass fraction)doubleC12c12C central abundance (mass fraction)doubleC12s12C surface abundance (mass fraction)doubleC13c13C central abundance (mass fraction)doubleC13s13C surface abundance (mass fraction)doubleN14c14N central abundance (mass fraction)doubleN14s14N surface abundance (mass fraction)doubleO16c16O central abundance (mass fraction)doubleO16s16O surface abundance (mass fraction)doubleO17c17O central abundance (mass fraction)doubleO17s17O surface abundance (mass fraction)doubleO18c18O central abundance (mass fraction)doubleO18s18O surface abundance (mass fraction)doubleNe20c20Ne central abundance (mass fraction)doubleNe20s20Ne surface abundance (mass fraction)doubleNe22c22Ne central abundance (mass fraction)doubleNe22s22Ne surface abundance (mass fraction)doubleMg24c24Mg central abundance (mass fraction)doubleMg24s24Mg surface abundance (mass fraction)doubleMg25c25Mg central abundance (mass fraction)doubleMg25s25Mg surface abundance (mass fraction)doubleMg26c26Mg central abundance (mass fraction)doubleMg26s26Mg surface abundance (mass fraction)doublelogK2Log(Apsidal motion constant (j=2))doublelogK3Log(Apsidal motion constant (j=3))doublelogK4Log(Apsidal motion constant (j=4))doubleXBFFractional depth of convective envelopedoublelogE2Log(Tidal torque constant)doubleECOPolytropic envelope characteristicdoublealphaPalphaP = -Ep x R/GM2doubleRgyrFractional gyration radiusdoublebeta1Gravity-darkening exponentdouble