J/ApJ/899/132ivo://CDS.VizieR/J/ApJ/899/132doi:10.26093/cds/vizier.18990132CDSGe H.Webbink R.F.Chen X.Han Z.2022-03-14T07:06:32Z2021-11-10T12:56:10ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelsstellar-massesmultiple-starsstellar-mass-lossinfrared-photometryThe distinguishing feature of the evolution of close binary stars is the role played by the mass exchange between the component stars. Whether or not the mass transfer is dynamically stable is one of the essential questions in binary evolution. In the limit of extremely rapid mass transfer, the response of a donor star in an interacting binary becomes asymptotically one of adiabatic expansion. We use the adiabatic mass-loss model to systematically survey the thresholds for dynamical timescale mass transfer over the entire span of possible donor star evolutionary states. We also simulate mass-loss process with isentropic envelopes, the specific entropy of which is fixed to be that at the base of the convective envelope, to artificially mimic the effect of such mass loss in superadiabatic surface convection regions, where the adiabatic approximation fails. We illustrate the general adiabatic response of 3.2M{odot} donor stars at different evolutionary stages. We extend our study to a grid of donor stars with different masses (from 0.1 to 100 M{sun} with Z=0.02) and at different evolutionary stages. We proceed to present our criteria for dynamically unstable mass transfer in both tabular and graphical forms. For red giant branch (RGB) and asymptotic giant branch (AGB) donors in systems with such mass ratios, they may have convective envelopes deep enough to evolve into common envelopes on a thermal timescale, if the donor star overfills its outer Lagrangian radius. Our results show that the RGB and AGB stars tend to be more stable than previously believed, and this may be helpful to explain the abundance of observed post-AGB binary stars with an orbital period of around 1000 days.2020ApJ...899..132Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/899/132CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/MNRAS/403/1213 : Tracers of stellar mass-loss. I. (Gonzalez-Lopezlira+, 2010)J/ApJ/753/71 : Mass-loss return from LMC evolved stars. VI. (Riebel+, 2012)J/A+A/556/A38 : Period-mass-loss rate relation of Miras (Uttenthaler, 2013)J/ApJ/812/40 : Adiabatic mass loss in binary stars. II. (Ge+, 2015)J/MNRAS/470/3765 : Mass-loss rates in LMC and SMC O stars (Massa+, 2017)J/A+A/616/A58 : Variability of the adiabatic parameter (de Avillez+, 2018)J/ApJ/856/170 : Tracers of stellar mass-loss. II. (Gonzalez-Lopezlira, 2018)J/A+A/622/A120 : Mass loss from Miras with and without Tc (Uttenthaler, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/899/132https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/899/132http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/899/132https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/899/132https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/899/132http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/899/132GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfrareddefaultJ/ApJ/899/132/table1Interior properties of initial modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMass[0.1/100] Model masssolMassphys.mass;meta.modelledfloatk[1/71] Mass loss sequence numbermeta.id;meta.numberintAge[0/13] Log age (1)log(yr)time.agedoubleMassCE[0/31] Convective envelope mass (2)solMassphys.massfloatMassC[0/85] Core mass (3)solMassphys.massfloatMassIC[0/40] Inner core mass (4)solMassphys.massfloatpsic[-8/206] Central electron chemical potential (5)phys.energy;phys.atmol.levelfloatrhoc[0.1/9.4] Log central densitylog(g.cm**-3)phys.densityfloatTc[6.6/9] Log central temperaturelog(K)phys.temperaturefloatHc[0/0.7] Central hydrogen abundance (6)phys.abund.XfloatHec[0/1] Central helium abundance (6)phys.abund.YfloatHs[0.1/0.8] Surface hydrogen abundance (6)phys.abund.XfloatJ/ApJ/899/132/table2Global properties of initial modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMass[0.1/100] Model masssolMassphys.mass;meta.modelleddoublek[1/71] Mass loss sequence numbermeta.id;meta.numberintRad[-0.9/3.6] Log radiuslog(solRad)phys.size.radiusfloatTeff[3.4/4.7] Log effective temperaturelog(K)phys.temperature.effectivefloatLum[-3.1/6.5] Log stellar Luminositylog(solLum)phys.luminosityfloatLumH[-17.4/6.5] Log hydrogen-burning luminositylog(solLum)phys.luminosityfloatLumHe[-39/6.3]? Log helium-burning luminositylog(solLum)phys.luminosityfloatnullableLumZ[-41.3/5.8]? Log heavy-element burning luminositylog(solLum)phys.luminosityfloatnullableLumnu[-4.8/6.8] Log neutrino luminositylog(solLum)phys.luminosityfloatf_Lumnu[*] Flag on Lumnu (1)meta.codecharLumth[-7.7/6.7] Log gravothermal luminositylog(solLum)phys.luminosityfloatf_Lumth[*] Flag on Lumth (1)meta.codecharI/MR2[0/0.3] Dimensionless moment of inertiastat.variance;pos.distance;phys.sizefloatJ/ApJ/899/132/table3Thresholds for conservative dynamical time scale mass transferrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMass[0.1/100] Initial mass modelsolMassphys.mass;meta.modelledfloatk[1/71] Mass loss sequence numbermeta.id;meta.numberintRad[-0.9/3.6] Log initial radius (1)log(solRad)phys.size.radiusfloatMKH[0.07/70.15]? Mass threshold (2)solMassphys.massfloatnullableRKH[-1.8/2.6]? Log Roche lobe radius (2)log(solRad)phys.size.radiusfloatnullableR*KH[-1.8/3.61]? Log stellar radius (2)log(solRad)phys.size.radiusfloatnullablezetaad[-2.635/8700]? Critical mass-radius exponent for dynamical time scale massarith.factordoublenullableqad[-0.433/4400]? Critical mass ratio for dynamical time scale (conservative) mass transfer (1)phys.mass;arith.ratiodoublenullableDexp[0/1.6]? Log superadiabatic expansion factor (3)stat.fit.paramfloatnullableMKHic[0.07/76.07]? Mass threshold (4)solMassphys.massfloatnullableRKHic[-1.7/2.6]? Log Roche lobe radius (4)log(solRad)phys.size.radiusfloatnullableR*KHic[-1.7/3.7]? Log stellar radius (4)log(solRad)phys.size.radiusfloatnullablezetaadic[-0.4/52000]? Critical mass-radius exponent for dynamical time scale mass transfer (3)arith.factordoublenullableqadic[0.6/26000]? Critical mass ratio for dynamical time scale (conservative) mass transfer (3)phys.mass;arith.ratiodoublenullable