J/ApJS/113/121ivo://CDS.VizieR/J/ApJS/113/121doi:10.26093/cds/vizier.21130121CDSKato M.1998-03-27T01:55:31Z1998-03-27T02:55:22ZCDS support team

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

cds-question@unistra.frnovaestellar-evolutionary-modelsTwenty-six sequences of optically thick wind solutions have been calculated which mimic the time-dependent evolution of classical novae of populations I and II. The peak of the new opacity around log T=5.2 due to iron lines is found to be strong enough to accelerate the winds even in very low iron abundance such as Z=0.001 for massive white dwarfs (>=0.8M_{sun}_). The old population novae show the slow light curve, the long X-ray turn-off time, the small expansion velocity and the small wind mass-loss rate. The X-ray turn-off time is a good indicator of the white dwarf mass because of its strong dependence on the white dwarf mass and weak dependence on the populations. The white dwarf mass is estimated to be ~0.6M_{sun}_ for GQ Mus and ~1.0M_{sun}_ for V1974 Cyg. The systematic difference of the wind velocity is predicted between novae in globular clusters and in galactic disk. Twenty-six tables are presented in the computer readable form of CD-ROM that consists of solutions of the optically thick wind and the static for the decay phase of classical novae with composition of X=0.35, C=0.1 and O=0.2 and heavy elements content Z=0.001, 0.004, 0.02, 0.05 and 0.1 for the white dwarf masses of 0.4, 0.6, 0.7, 0.8, 0.9, 1.0, 1.2 and 1.35M_{sun}_. These tables list the characteristic values of the envelope such as the photospheric temperature, the velocity, the wind mass-loss rate and fluxes of four wavelength bands. The updated OPAL opacity (Iglesias & Rogers, 1996ApJ...464..943I) is used.1997ApJS..113..121Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/113/121CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJS/113/121https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJS/113/121http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJS/113/121https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJS/113/121https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJS/113/121http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJS/113/121GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJS/113/121/headerOverall model parameters for all tablesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTableTable number (in the printed paper)meta.id;meta.datasetintModelModel namemeta.id;stat.fitcharMassWDWhite dwarf masssolMassphys.massfloatZHeavy elements contentphys.abund.ZfloatRowWSNumber of rows of (wind + static) solutionsmeta.numberintRowTotNumber of rows totalmeta.numberintJ/ApJS/113/121/tablesEnvelope solutions for classical novae (table1 to table26)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMassWDWhite dwarf masssolMassphys.massfloatZHeavy elements contentphys.abund.Zfloatlog(Tph)Photospheric temperaturelog(K)phys.temperaturefloatlog(Lph)Photospheric luminositylog(1e-07W)phys.luminosityfloatlog(Rph)Photospheric radiuslog(solRad)phys.size.radiusfloatlog(Vph)Photospheric velocitylog(cm.s**-1)phys.velocfloatlog(Menv)Envelope masslog(solMass)phys.massfloatlog(dM/dtw)Mass loss rate due to optically thick wind (log dM/dt (wind))log(solMass.yr**-1)phys.mass.lossfloatlog(dM/dtn)Mass loss rate due to Hydrogen nuclear burning (log dM/dt (nuc))log(solMass.yr**-1)phys.mass.lossfloatRadcrRadius at the critical pointsolRadphys.size.radiusfloatVelcrVelocity at the critical pointcm/sphys.velocfloattimeEvolutional timeyrtime.agedoubleMbolBolometric magnitudemagphot.mag.bolfloatMvisVisual magnitudemagphot.mag;em.opt.Vfloatlog(FUV)*Flux in UV (912.3250{AA})log(solLum.kpc**-2)phot.flux;em.UVfloatlog(FEUV)*Flux in EUV (100.912{AA})log(solLum.kpc**-2)phot.flux;em.UVfloatlog(FSSXR)*Flux in supersoft X-ray (30.100{AA})log(solLum.kpc**-2)phot.flux;em.UVfloat