J/A+A/682/A123ivo://CDS.VizieR/J/A+A/682/A123doi:10.26093/cds/vizier.36820123CDSTemaj D.Schneider F.R.N.Laplace E.Wei D.Podsiadlowski P.2024-11-06T20:06:48Z2024-02-12T08:47:52ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelssupernovaechemical-abundancesUnderstanding and predicting their final fate is increasingly important, e.g., in the context of gravitational-wave astronomy. The interior mixing of stars in general and convective boundary mixing in particular remain some of the largest uncertainties in their evolution. Here, we investigate the influence of convective boundary mixing on the pre-supernova structure and explosion properties of massive stars. Using the 1D stellar evolution code Mesa, we model single, non-rotating stars of solar metallicity with initial masses of 5-70M_{sun}_ and convective core step-overshooting of 0.05-0.50 pressure scale heights. Stars are evolved until the onset of iron core collapse, and the pre-SN models are exploded using a parametric, semi-analytic SN code. We use the compactness parameter to describe the interior structure of stars at core collapse and find a pronounced peak in compactness at carbon-oxygen core masses of MCO~7M_{sun}_ and generally high compactness at M_CO_>~14M_{sun}_. Larger convective core overshooting shifts the location of the compactness peak by 1-2M_{sun}_ to higher M_CO_. These core masses correspond to initial masses of 24M_{sun}_ (19M_{sun}_) and >~40M_{sun}_ (>~30M_{sun}_), respectively, in models with the lowest (highest) convective core overshooting parameter. In both high-compactness regimes, stars are found to collapse into black holes. As the luminosity of the pre-supernova progenitor is determined by M_CO_, we predict blackhole formation for progenitors with luminosities 5.35<=log(L/L_{sun}_)<=5.50 and log(L/L_{sun}_)>=5.80. The luminosity range of black-hole formation from stars in the compactness peak agrees well with the observed luminosity of the red supergiant star N6946 BH1 that disappeared without a bright supernova and likely collapsed into a black hole. While some of our models in the luminosity range log(L/L_{sun}_)=5.1-5.5 indeed collapse to form black holes, this does not fully explain the lack of observed SN IIP progenitors at these luminosities, i.e. the missing red-supergiant problem. The amount of convective boundary mixing also affects the wind mass loss of stars such that the lowest black hole mass are 15M_{sun}_ and 10M_{sun}_ in our models with the lowest and highest convective core overshooting parameter, respectively. The compactness parameter, central specific entropy, and iron core mass describe a qualitatively similar landscape as a function of M_CO_, and we find that entropy is a particularly good predictor of the neutron-star masses in our models. We find no correlation between the explosion energy, kick velocity, and nickel mass production with the convective core overshooting value, but a tight relation with the compactness parameter. We further show how convective core overshooting affects the pre-supernova locations of stars in the Hertzsprung-Russell diagram and the plateau luminosity and duration of SN IIP lightcurves.2024A&A...682A.123Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/682/A123CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/682/A123https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/682/A123http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/682/A123https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/682/A123https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/682/A123http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/682/A123GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/682/A123/tablea1Properties of all our models used throughout the paperrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMiniInitial masssolMassphys.massfloatalphaovConvective core overshooting valuestat.paramfloatMHeHelium-core masssolMassphys.mass;arith.ratiofloatMCO? CO-core masssolMassphys.mass;arith.ratiofloatnullableMFe? Iron-core masssolMassphys.mass;arith.ratiofloatnullableXc? Carbon abundance at the end of core-helium burningphys.abundfloatnullableMfinalFinal mass of the modelsolMassphys.mass;meta.modelledfloatchi2.5? Compactness value {chi}25meta.code;phys.sizefloatnullableSc? Central specific entropy at the onset of iron-core collapsephys.energy.densityfloatnullablemEbind? Gravitational binding energy of the material above the iron core (-Ebind)1e-07Jphys.energyfloatnullableFatePredicted final fatemeta.codecharMrm? Gravitational remnant masssolMassphys.massfloatnullableEexpl? Explosion energy (in units of Bethe, 10^51^erg)1e+44Jphys.energyfloatnullablevkick? Licl velocitykm/sphys.velocfloatnullableMNi? Nickel masssolMassphys.mass;arith.ratiofloatnullableMej? Ejecta masssolMassphys.massfloatnullableLp/Lp0? Plateau luminosity Lp/Lp,0phys.luminosity;arith.ratiofloatnullabletp/tp0? Duration of the plateau tp/tp,0time.intervalfloatnullableLogLcLuminosity at the end of core-helium burninglog(solLum)phys.luminosityfloatlogTeffEffective temperature at the end of core-helium burninglog(K)phys.temperature.effectivefloat