J/A+A/566/A146ivo://CDS.VizieR/J/A+A/566/A146doi:10.26093/cds/vizier.35660146CDSKozyreva A.Yoon S.-C.Langer N.2014-12-21T20:34:08Z2014-06-26T13:02:33ZCDS support team

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

cds-question@unistra.frastronomical-modelssupernovaechemical-abundancesBoth recent observations and stellar evolution models suggest that pair-instability supernovae (PISNe) could occur in the local Universe, at metallicities below Z_{sun}_/3. Previous PISN models were mostly produced at very low metallicities in the context of the early Universe. We present new PISNe models at a metallicity of Z=0.001, which are relevant for the local Universe. We take the self-consistent stellar evolutionary models of pair-instability progenitors with initial masses of 150 and 250 solar masses at metallicity of Z=0.001 by Langer et al. (2007A&A...475L..19L) and follow the evolution of these models through the supernova explosions, using a hydrodynamics stellar evolution code with an extensive nuclear network including 200 isotopes. Both models explode as PISNe without leaving a compact stellar remnant. Our models produce a nucleosynthetic pattern that is generally similar to that of Population III PISN models, which is mainly characterized by the production of large amounts of elements and a strong deficiency of the odd-charged elements. However, the odd-even effect in our models is significantly weaker than that found in Population III models. The comparison with the nucleosynthetic yields from core-collapse supernovae at a similar metallicity (Z=0.002) indicates that PISNe could have strongly influenced the chemical evolution below Z=0.002, assuming a standard initial mass function. The odd-even effect is predicted to be most prominent for the intermediate mass elements between silicon and calcium. With future observations of chemical abundances in Population II stars, our result can be used to constrain the number of PISNe that occurred during the past evolution of our Galaxy.2014A&A...566A.146Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/566/A146CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJ/664/1033 : Variations in supernova yields (Young+ 2007)J/MNRAS/408/827 : Simulations of supernova explosions (Dessart+, 2010)J/A+A/558/A131 : Model spectra of hot stars at the pre-SN stage (Groh+, 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/566/A146https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/566/A146http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/566/A146https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/566/A146https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/566/A146http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/566/A146GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/566/A146/table3Total nucleosynthetic yields and production factorsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElElement namemeta.id;phys.atmol.elementcharA[1/71] Isotope numberphys.atmol.weightintY(150)Isotopic yields for model 150MsolMassphys.composition.yielddoubleY(250)Isotopic yields for model 250MsolMassphys.composition.yielddoublePF(150)Isotopic production factors for model 150Mstat.paramdoublePF(250)Isotopic production factors for model 250Mstat.paramdouble