J/A+A/467/1389ivo://CDS.VizieR/J/A+A/467/1389doi:10.26093/cds/vizier.34671389CDSClaret A.2017-07-06T06:26:16Z2007-07-28T22:36:32ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelsThe aim of the present grid of stellar models is to complete our previous calculations and provide a tool for investigating the astrophysical properties of eclipsing binaries, stellar clusters, galactic bulges, and elliptical galaxies with a high metal content. To explore the applicability of high metallic models, we have computed three grids: (X, Z)=(0.64, 0.04), (0.58, 0.06), and (0.46, 0.10). For all these grids, we adopted an enrichment law {Delta}Y/{Delta}Z=2.0, as in our previous papers on this subject. The input physics is almost the same as adopted in our earlier work except for some numerical details, recent measurement of the rate for the reaction ^14^N(p,gamma)^15^O, and the recent mass-loss rate for the Wolf-Rayet stages. Two high-metallicity clusters, NGC 6253 and NGC 6791, were used to test the present calculations with very satisfactory results. On the other hand, as this series of grids was mainly designed to investigate the tidal evolution of close binaries, we analyse the present status of circularization times in both clusters and isolated binaries.2007A&A...467.1389Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/467/1389CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/453/769 : New grids of stellar models III (Claret, 2006)J/A+A/440/647 : New grids of stellar models II (Claret, 2005)J/A+A/424/919 : New grids of stellar models I (Claret, 2004)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/467/1389https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/467/1389http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/467/1389https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/467/1389https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/467/1389http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/467/1389GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/467/1389/gridSummary of parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMInitial masssolMassphys.massfloatnullablelogMInitial masslog(solMass)phys.massfloatX[0.460-0.640] X initial X composition (H)phys.abund.XfloatZ[0.04-0.10] Z initial compositionsrc.redshift;phys.compositionfloatOv[0/1] 1=with overshootingstat.paramintFileNameOriginal filename with result (in subdirectory)meta.id;meta.filecharHRPlot the Herzsprung-Russel diagram for this massmeta.ref.urlcharEvolutionDetails of evolution for this set of (X Z M) parametersmeta.ref.urlcharJ/A+A/467/1389/z04Grid for (X,Z)=(0.640,0.04)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogMInitial masslog(solMass)phys.massfloatX[0.460-0.640] X initial X composition (H)phys.abund.XfloatZ[0.04-0.10] Z initial compositionsrc.redshift;phys.compositionfloatOv[0/1] 1=with overshootingstat.paramintAgeAge of the modelsyrtime.agedoublelog(L)Log (Total luminosity)log(solLum)phys.luminosityfloatlog(g)Log (Surface gravity)log(cm.s**-2)arith.zpfloatlog(Teff)Log (Effective temperature)log(K)arith.zpfloatMassActual mass of the modelsolMassphys.mass;meta.modelleddoublelogdM/dtLog (mass loss rate)log(solMass.yr**-1)phys.mass.lossdoublelogDcLog (central density)log(g.cm**-3)arith.zpdoublelogTcLog (central temperature)log(K)arith.zpdoubleQcCore mass (fraction)phys.massdoubleXcH central abundance (mass fraction)phys.abund.XdoubleXsH surface abundance (mass fraction)phys.abund.XdoubleYc4He central abundance (mass fraction)phys.abund;em.wl.centraldoubleYs4He surface abundance (mass fraction)meta.notedoubleC12c12C central abundance (mass fraction)phys.abunddoubleC12s12C surface abundance (mass fraction)phys.abunddoubleC13c13C central abundance (mass fraction)phys.abunddoubleC13s13C surface abundance (mass fraction)phys.abunddoubleN14c14N central abundance (mass fraction)phys.abunddoubleN14s14N surface abundance (mass fraction)phys.abunddoubleO16c16O central abundance (mass fraction)phys.abunddoubleO16s16O surface abundance (mass fraction)phys.abunddoubleO17c17O central abundance (mass fraction)phys.abunddoubleO17s17O surface abundance (mass fraction)phys.abunddoubleO18c18O central abundance (mass fraction)phys.abunddoubleO18s18O surface abundance (mass fraction)phys.abunddoubleNe20c20Ne central abundance (mass fraction)phys.abunddoubleNe20s20Ne surface abundance (mass fraction)phys.abunddoubleNe22c22Ne central abundance (mass fraction)phys.abunddoubleNe22s22Ne surface abundance (mass fraction)phys.abunddoubleMg24c24Mg central abundance (mass fraction)phys.abunddoubleMg24s24Mg surface abundance (mass fraction)phys.abunddoubleMg25c25Mg central abundance (mass fraction)phys.abunddoubleMg25s25Mg surface abundance (mass fraction)phys.abunddoubleMg26c26Mg central abundance (mass fraction)phys.abunddoubleMg26s26Mg surface abundance (mass fraction)phys.abunddoublelogK2Log(Apsidal motion constant (j=2))stat.paramdoublelogK3Log(Apsidal motion constant (j=3))stat.paramdoublelogK4Log(Apsidal motion constant (j=4))stat.paramdoubleXBFFractional depth of convective envelopestat.paramdoublelogE2Log(Tidal torque constant)stat.paramdoubleECOPolytropic envelope characteristicstat.paramdoublealphaPalphaP = -Ep x R/GM2stat.paramdoubleRgyrFractional gyration radiusstat.paramdoublebeta1Gravity-darkening exponentstat.paramdoubleJ/A+A/467/1389/z06Grid for (X,Z)=(0.580,0.06)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogMInitial masslog(solMass)phys.massfloatX[0.460-0.640] X initial X composition (H)phys.abund.XfloatZ[0.04-0.10] Z initial compositionsrc.redshift;phys.compositionfloatOv[0/1] 1=with overshootingstat.paramintAgeAge of the modelsyrtime.agedoublelog(L)Log (Total luminosity)log(solLum)phys.luminosityfloatlog(g)Log (Surface gravity)log(cm.s**-2)arith.zpfloatlog(Teff)Log (Effective temperature)log(K)arith.zpfloatMassActual mass of the modelsolMassphys.mass;meta.modelleddoublelogdM/dtLog (mass loss rate)log(solMass.yr**-1)phys.mass.lossdoublelogDcLog (central density)log(g.cm**-3)arith.zpdoublelogTcLog (central temperature)log(K)arith.zpdoubleQcCore mass (fraction)phys.massdoubleXcH central abundance (mass fraction)phys.abund.XdoubleXsH surface abundance (mass fraction)phys.abund.XdoubleYc4He central abundance (mass fraction)phys.abund;em.wl.centraldoubleYs4He surface abundance (mass fraction)meta.notedoubleC12c12C central abundance (mass fraction)phys.abunddoubleC12s12C surface abundance (mass fraction)phys.abunddoubleC13c13C central abundance (mass fraction)phys.abunddoubleC13s13C surface abundance (mass fraction)phys.abunddoubleN14c14N central abundance (mass fraction)phys.abunddoubleN14s14N surface abundance (mass fraction)phys.abunddoubleO16c16O central abundance (mass fraction)phys.abunddoubleO16s16O surface abundance (mass fraction)phys.abunddoubleO17c17O central abundance (mass fraction)phys.abunddoubleO17s17O surface abundance (mass fraction)phys.abunddoubleO18c18O central abundance (mass fraction)phys.abunddoubleO18s18O surface abundance (mass fraction)phys.abunddoubleNe20c20Ne central abundance (mass fraction)phys.abunddoubleNe20s20Ne surface abundance (mass fraction)phys.abunddoubleNe22c22Ne central abundance (mass fraction)phys.abunddoubleNe22s22Ne surface abundance (mass fraction)phys.abunddoubleMg24c24Mg central abundance (mass fraction)phys.abunddoubleMg24s24Mg surface abundance (mass fraction)phys.abunddoubleMg25c25Mg central abundance (mass fraction)phys.abunddoubleMg25s25Mg surface abundance (mass fraction)phys.abunddoubleMg26c26Mg central abundance (mass fraction)phys.abunddoubleMg26s26Mg surface abundance (mass fraction)phys.abunddoublelogK2Log(Apsidal motion constant (j=2))stat.paramdoublelogK3Log(Apsidal motion constant (j=3))stat.paramdoublelogK4Log(Apsidal motion constant (j=4))stat.paramdoubleXBFFractional depth of convective envelopestat.paramdoublelogE2Log(Tidal torque constant)stat.paramdoubleECOPolytropic envelope characteristicstat.paramdoublealphaPalphaP = -Ep x R/GM2stat.paramdoubleRgyrFractional gyration radiusstat.paramdoublebeta1Gravity-darkening exponentstat.paramdoubleJ/A+A/467/1389/z10Grid for (X,Z)=(0.460,0.10)Ov[0/1] 1=with overshootingstat.paramintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogMInitial masslog(solMass)phys.massfloatX[0.460-0.640] X initial X composition (H)phys.abund.XfloatZ[0.04-0.10] Z initial compositionsrc.redshift;phys.compositionfloatAgeAge of the modelsyrtime.agedoublelog(L)Log (Total luminosity)log(solLum)phys.luminosityfloatlog(g)Log (Surface gravity)log(cm.s**-2)arith.zpfloatlog(Teff)Log (Effective temperature)log(K)arith.zpfloatMassActual mass of the modelsolMassphys.mass;meta.modelleddoublelogdM/dtLog (mass loss rate)log(solMass.yr**-1)phys.mass.lossdoublelogDcLog (central density)log(g.cm**-3)arith.zpdoublelogTcLog (central temperature)log(K)arith.zpdoubleQcCore mass (fraction)phys.massdoubleXcH central abundance (mass fraction)phys.abund.XdoubleXsH surface abundance (mass fraction)phys.abund.XdoubleYc4He central abundance (mass fraction)phys.abund;em.wl.centraldoubleYs4He surface abundance (mass fraction)meta.notedoubleC12c12C central abundance (mass fraction)phys.abunddoubleC12s12C surface abundance (mass fraction)phys.abunddoubleC13c13C central abundance (mass fraction)phys.abunddoubleC13s13C surface abundance (mass fraction)phys.abunddoubleN14c14N central abundance (mass fraction)phys.abunddoubleN14s14N surface abundance (mass fraction)phys.abunddoubleO16c16O central abundance (mass fraction)phys.abunddoubleO16s16O surface abundance (mass fraction)phys.abunddoubleO17c17O central abundance (mass fraction)phys.abunddoubleO17s17O surface abundance (mass fraction)phys.abunddoubleO18c18O central abundance (mass fraction)phys.abunddoubleO18s18O surface abundance (mass fraction)phys.abunddoubleNe20c20Ne central abundance (mass fraction)phys.abunddoubleNe20s20Ne surface abundance (mass fraction)phys.abunddoubleNe22c22Ne central abundance (mass fraction)phys.abunddoubleNe22s22Ne surface abundance (mass fraction)phys.abunddoubleMg24c24Mg central abundance (mass fraction)phys.abunddoubleMg24s24Mg surface abundance (mass fraction)phys.abunddoubleMg25c25Mg central abundance (mass fraction)phys.abunddoubleMg25s25Mg surface abundance (mass fraction)phys.abunddoubleMg26c26Mg central abundance (mass fraction)phys.abunddoubleMg26s26Mg surface abundance (mass fraction)phys.abunddoublelogK2Log(Apsidal motion constant (j=2))stat.paramdoublelogK3Log(Apsidal motion constant (j=3))stat.paramdoublelogK4Log(Apsidal motion constant (j=4))stat.paramdoubleXBFFractional depth of convective envelopestat.paramdoublelogE2Log(Tidal torque constant)stat.paramdoubleECOPolytropic envelope characteristicstat.paramdoublealphaPalphaP = -Ep x R/GM2stat.paramdoubleRgyrFractional gyration radiusstat.paramdoublebeta1Gravity-darkening exponentstat.paramdouble