J/A+A/618/A133ivo://CDS.VizieR/J/A+A/618/A133doi:10.26093/cds/vizier.36180133CDSChoplin A.Hirschi R.Meynet G.Ekstroem S.Chiappini C.Laird A.2018-12-03T15:02:03Z2018-10-23T09:35:49ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelschemical-abundancesRecent studies show that rotation significantly affects the s-process in massive stars. We provide tables of yields for non-rotating and rotating massive stars between 10 and 150M_{sun}_ at Z=10^-3^([Fe/H]=-1.8). Tables for different mass cuts are provided. The complete s-process is followed during the whole evolution with a network of 737 isotopes, from Hydrogen to Polonium. A grid of stellar models with initial masses of 10, 15, 20, 25, 40, 60, 85, 120 and 150M_{sun}_ and with an initial rotation rate of both 0 or 40% of the critical velocity was computed. Three extra models were computed in order to investigate the effect of faster rotation (70% of the critical velocity) and of a lower ^17^O({alpha},{gamma}) reaction rate. At the considered metallicity, rotation has a strong impact on the production of s-elements for initial masses between 20 and 60M_{sun}_. In this range, the first s-process peak is boosted by 2-3dex if rotation is included. Above 60M_{sun}_, s-element yields of rotating and non-rotating models are similar. Increasing the initial rotation from 40% to 70% of the critical velocity enhances the production of 40<~Z<~60 elements by ~0.5-1dex. Adopting a reasonably lower ^17^O({alpha},{gamma}) rate in the fast rotating model (70% of the critical velocity) boosts again the yields of s-elements with 55<~Z<~82 by about 1dex. In particular, a modest amount of Pb is produced. Together with s-elements, some light elements (particularly fluorine) are strongly overproduced in rotating models.2018A&A...618A.133Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/618/A133CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/618/A133https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/618/A133http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/618/A133https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/618/A133https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/618/A133http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/618/A133GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/618/A133/yieldsYields (table4)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMassInitial mass (10, 15, 20, 25, 40, 60, 85, 120, 150)solMassphys.massintRotInitial rotation rate (v_ini_/v_crit_) (0.0, 0.4, 0.7)arith.ratefloatRate[0/1] Rate for the ^17^O(a,g)21Ne reaction (1)meta.noteintMcutMass cutsolMassphys.massfloatIsotopeIsotope namephys.atmol.elementcharEjMassEjected mass of the considered isotopesolMassphys.massdoubleYieldStellar yield (Eq. 3 of the paper)solMassphys.composition.yielddouble