J/A+AS/106/275ivo://CDS.VizieR/J/A+AS/106/275CDSBertelli G.Bressan A.Chiosi C.Fagotto F.Nasi E,1999-03-01T15:22:11Z1999-03-01T16:20:59ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelshertzsprung-russell-diagramIn this paper we present large grids of theoretical isochrones for the initial chemical compositions [Z=0.0004, Y=0.23], [Z=0.004, Y=0.24], [Z=0.008, Y=0.25], [Z=0.02, Y=0.28], and [Z= 0.05, Y=0.352] and ages in the range 4Myr to 16Gyr. These isochrones are derived from stellar models computed with the most recent radiative opacities by Iglesias et al. (1992). In addition to this we present another set with chemical composition [Z=0.001, Y=0.23] based on models calculated with the radiative opacities by Huebner et al. (1977). All the stellar models are followed from the zero age main sequence (ZAMS) to the central carbon ignition for massive stars or to the beginning of the thermally pulsing regime of the asymptotic giant branch phase (TP-AGB) for low and intermediate mass stars. For each isochrone, we give the current mass, effective temperatures, bolometric and visual magnitudes, (U-B), (B-V), (V-R), (V-I), (V-J), (V-H), and (V-K) colors, and the luminosity function for the case of the Salpeter law. In addition to this, integrated magnitudes and colors at several characteristic points are also presented together with the mass of the remnant star when appropriate. The main characteristic that makes this set of isochrones very valuable is based on their extension in mass and chemical composition, besides the calculation of late stages of evolution, beyond the red giant tip till the white dwarf stage after the planetary nebula phase.1994A+AS..106..275Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+AS/106/275CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+AS/106/275https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+AS/106/275http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+AS/106/275https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+AS/106/275https://vizier.iucaa.in/viz-bin/votable?-source=J/A+AS/106/275http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+AS/106/275GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+AS/106/275/table4Model for z=0.0080, Y=0.25recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlog(Age)Logarithm of the agelog(yr)time.agefloatMCurrent mass (1)solMassphys.massfloatlog(Teff)Logarithm of effective temperaturelog(K)phys.temperature.effectivefloatMbolBolometric magnitudemagphot.mag.bolfloatVAbsolute visual magnitudemagphys.magAbs;em.optfloat(U-B)(U-B) color indexmagphot.color;em.opt.U;em.opt.Bfloat(B-V)(B-V) color indexmagphot.color;em.opt.B;em.opt.Vfloat(V-R)(V-R) color indexmagphot.color;em.opt.V;em.opt.Rfloat(V-I)(V-I) color indexmagphot.color;em.opt.V;em.opt.Ifloat(V-J)(V-J) color indexmagphot.color;em.opt.V;em.IR.Jfloat(V-H)(V-H) color indexmagphot.color;em.opt.V;em.IR.Hfloat(V-K)(V-K) color indexmagphot.color;em.opt.V;em.IR.KfloatFLUMLuminosity function for the case of the Salpeter lawphys.luminosity.fundoubleMwindReal value of the mass after mass loss by stellar wind for massive stars (2)solMassphys.massfloatJ/A+AS/106/275/table1Model for z=0.0004, Y=0.23recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlog(Age)Logarithm of the agelog(yr)time.agefloatMCurrent mass (1)solMassphys.massfloatlog(Teff)Logarithm of effective temperaturelog(K)phys.temperature.effectivefloatMbolBolometric magnitudemagphot.mag.bolfloatVAbsolute visual magnitudemagphys.magAbs;em.optfloat(U-B)(U-B) color indexmagphot.color;em.opt.U;em.opt.Bfloat(B-V)(B-V) color indexmagphot.color;em.opt.B;em.opt.Vfloat(V-R)(V-R) color indexmagphot.color;em.opt.V;em.opt.Rfloat(V-I)(V-I) color indexmagphot.color;em.opt.V;em.opt.Ifloat(V-J)(V-J) color indexmagphot.color;em.opt.V;em.IR.Jfloat(V-H)(V-H) color indexmagphot.color;em.opt.V;em.IR.Hfloat(V-K)(V-K) color indexmagphot.color;em.opt.V;em.IR.KfloatFLUMLuminosity function for the case of the Salpeter lawphys.luminosity.fundoubleMwindReal value of the mass after mass loss by stellar wind for massive stars (2)solMassphys.massfloatJ/A+AS/106/275/table2Model for z=0.0010, Y=0.23recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlog(Age)Logarithm of the agelog(yr)time.agefloatMCurrent mass (1)solMassphys.massfloatlog(Teff)Logarithm of effective temperaturelog(K)phys.temperature.effectivefloatMbolBolometric magnitudemagphot.mag.bolfloatVAbsolute visual magnitudemagphys.magAbs;em.optfloat(U-B)(U-B) color indexmagphot.color;em.opt.U;em.opt.Bfloat(B-V)(B-V) color indexmagphot.color;em.opt.B;em.opt.Vfloat(V-R)(V-R) color indexmagphot.color;em.opt.V;em.opt.Rfloat(V-I)(V-I) color indexmagphot.color;em.opt.V;em.opt.Ifloat(V-J)(V-J) color indexmagphot.color;em.opt.V;em.IR.Jfloat(V-H)(V-H) color indexmagphot.color;em.opt.V;em.IR.Hfloat(V-K)(V-K) color indexmagphot.color;em.opt.V;em.IR.KfloatFLUMLuminosity function for the case of the Salpeter lawphys.luminosity.fundoubleMwindReal value of the mass after mass loss by stellar wind for massive stars (2)solMassphys.massfloatJ/A+AS/106/275/table3Model for z=0.0040, Y=0.24recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlog(Age)Logarithm of the agelog(yr)time.agefloatMCurrent mass (1)solMassphys.massfloatlog(Teff)Logarithm of effective temperaturelog(K)phys.temperature.effectivefloatMbolBolometric magnitudemagphot.mag.bolfloatVAbsolute visual magnitudemagphys.magAbs;em.optfloat(U-B)(U-B) color indexmagphot.color;em.opt.U;em.opt.Bfloat(B-V)(B-V) color indexmagphot.color;em.opt.B;em.opt.Vfloat(V-R)(V-R) color indexmagphot.color;em.opt.V;em.opt.Rfloat(V-I)(V-I) color indexmagphot.color;em.opt.V;em.opt.Ifloat(V-J)(V-J) color indexmagphot.color;em.opt.V;em.IR.Jfloat(V-H)(V-H) color indexmagphot.color;em.opt.V;em.IR.Hfloat(V-K)(V-K) color indexmagphot.color;em.opt.V;em.IR.KfloatFLUMLuminosity function for the case of the Salpeter lawphys.luminosity.fundoubleMwindReal value of the mass after mass loss by stellar wind for massive stars (2)solMassphys.massfloatJ/A+AS/106/275/table6Model for z=0.0500, Y=0.352recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlog(Age)Logarithm of the agelog(yr)time.agefloatMCurrent mass (1)solMassphys.massfloatlog(Teff)Logarithm of effective temperaturelog(K)phys.temperature.effectivefloatMbolBolometric magnitudemagphot.mag.bolfloatVAbsolute visual magnitudemagphys.magAbs;em.optfloat(U-B)(U-B) color indexmagphot.color;em.opt.U;em.opt.Bfloat(B-V)(B-V) color indexmagphot.color;em.opt.B;em.opt.Vfloat(V-R)(V-R) color indexmagphot.color;em.opt.V;em.opt.Rfloat(V-I)(V-I) color indexmagphot.color;em.opt.V;em.opt.Ifloat(V-J)(V-J) color indexmagphot.color;em.opt.V;em.IR.Jfloat(V-H)(V-H) color indexmagphot.color;em.opt.V;em.IR.Hfloat(V-K)(V-K) color indexmagphot.color;em.opt.V;em.IR.KfloatFLUMLuminosity function for the case of the Salpeter lawphys.luminosity.fundoubleMwindReal value of the mass after mass loss by stellar wind for massive stars (2)solMassphys.massfloatJ/A+AS/106/275/table5Model for z=0.0200, Y=0.28recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlog(Age)Logarithm of the agelog(yr)time.agefloatMCurrent mass (1)solMassphys.massfloatlog(Teff)Logarithm of effective temperaturelog(K)phys.temperature.effectivefloatMbolBolometric magnitudemagphot.mag.bolfloatVAbsolute visual magnitudemagphys.magAbs;em.optfloat(U-B)(U-B) color indexmagphot.color;em.opt.U;em.opt.Bfloat(B-V)(B-V) color indexmagphot.color;em.opt.B;em.opt.Vfloat(V-R)(V-R) color indexmagphot.color;em.opt.V;em.opt.Rfloat(V-I)(V-I) color indexmagphot.color;em.opt.V;em.opt.Ifloat(V-J)(V-J) color indexmagphot.color;em.opt.V;em.IR.Jfloat(V-H)(V-H) color indexmagphot.color;em.opt.V;em.IR.Hfloat(V-K)(V-K) color indexmagphot.color;em.opt.V;em.IR.KfloatFLUMLuminosity function for the case of the Salpeter lawphys.luminosity.fundoubleMwindReal value of the mass after mass loss by stellar wind for massive stars (2)solMassphys.massfloat