J/MNRAS/404/1529ivo://CDS.VizieR/J/MNRAS/404/1529doi:10.26093/cds/vizier.74041529CDSBisterzo S.Gallino R.Straniero O.Cristallo S.Kappeler F.2024-07-11T20:16:27Z2011-01-03T14:02:14ZCDS support team

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

cds-question@unistra.fratomic-physicsA large sample of carbon-enhanced metal-poor stars enriched in s-process elements (CEMP-s) have been observed in the Galactic halo. These stars of low mass (M~0.9M_{sun}_) are located on the main-sequence or the red-giant phase, and do not undergo third dredge-up (TDU) episodes. The s-process enhancement is most plausibly due to accretion in a binary system from a more massive companion when on the asymptotic giant branch (AGB) phase (now a white dwarf). In order to interpret the spectroscopic observations, updated AGB models are needed to follow in detail the s-process nucleosynthesis. We present nucleosynthesis calculations based on AGB stellar models obtained with Frascati Raphson-Newton Evolutionary Code (FRANEC) for low initial stellar masses and low metallicities. For a given metallicity, a wide spread in the abundance of the s-process elements is obtained by varying the amount of 13C and its profile in the pocket, where the 13C({alpha}, n)16O reaction is the major neutron source, releasing neutrons in radiative conditions during the interpulse phase. We also account for the second neutron source ^22^Ne({alpha},n)^25^Mg, partially activated during convective thermal pulses.2010MNRAS.404.1529Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/404/1529CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/404/1529https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/404/1529http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/404/1529https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/404/1529https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/404/1529http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/404/1529GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/MNRAS/404/1529/tablea1Theoretical predictions in percentage for elements from Sr to BiElElementphys.atmol.elementcharZAtomic numbermeta.id;meta.mainintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintA(El)Percentage of element obtained by an average of M=1.5 and 3.0M_{sun}_ models (M_aver_) at [Fe/H]=-0.3 (1)%phys.atmolfloatU(El)Percentage element improved with cross section measurements and solar abundances upgraded to 2009 at [Fe/H]=-0.3 (1)%phys.atmolfloat[El/Eu]Normalization of the updated main-s percentages to europium in logarithmic scalephys.abundfloatJ/MNRAS/404/1529/Fe-26.Theoretical [El/Fe] predictions (He to Bi) for [Fe/H]=-2.6 as a function of mass and ^13^C-pocket changes (tables B1 to B4 of paper)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintM[1.3,2.0] Initial mass in AGB stagesolMassphys.massfloatnullablenNumber of thermal pulses (TP) or third dredge-up (TDU) episodesmeta.numberintnullableElElementphys.atmol.elementcharZAtomic numbermeta.id;meta.mainintST*2Theoretical [El/Fe] predictions for ST*2 (1)phys.abundfloatST*1.3Theoretical [El/Fe] predictions for ST*1.3 (1)phys.abundfloatSTTheoretical [El/Fe] predictions for ST (1)phys.abundfloatST/1.5Theoretical [El/Fe] predictions for ST/1.5 (1)phys.abundfloatST/2Theoretical [El/Fe] predictions for ST/2 (1)phys.abundfloatST/3Theoretical [El/Fe] predictions for ST/3 (1)phys.abundfloatST/4.5Theoretical [El/Fe] predictions for ST/4.5 (1)phys.abundfloatST/6Theoretical [El/Fe] predictions for ST/6 (1)phys.abundfloatST/9Theoretical [El/Fe] predictions for ST/9 (1)phys.abundfloatST/12Theoretical [El/Fe] predictions for ST/12 (1)phys.abundfloatST/18Theoretical [El/Fe] predictions for ST/18 (1)phys.abundfloatST/24Theoretical [El/Fe] predictions for ST/24 (1)phys.abundfloatST/30Theoretical [El/Fe] predictions for ST/30 (1)phys.abundfloatST/45Theoretical [El/Fe] predictions for ST/45 (1)phys.abundfloatST/75Theoretical [El/Fe] predictions for ST/75 (1)phys.abundfloatST/150Theoretical [El/Fe] predictions for ST/150 (1)phys.abundfloatJ/MNRAS/404/1529/Fe-varTheoretical [El/Fe] predictions (He to Bi) for -3.6<=[Fe/H]<=-1 and 2 values of ^13^C-pocket (ST and ST/12) (tables B5 and B6 of paper)ElElement namemeta.id;phys.atmol.elementcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintM[1.3,1.5] Initial mass in AGB stagesolMassphys.massfloatnullableZAtomic numbermeta.id;meta.mainint(-3.6)Prediction of [El/Fe] for ST, [Fe/H]=-3.6phys.abundfloat(-3.0)Prediction of [El/Fe] for ST, [Fe/H]=-3.0phys.abundfloat(-2.6)Prediction of [El/Fe] for ST, [Fe/H]=-2.6phys.abundfloat(-2.3)Prediction of [El/Fe] for ST, [Fe/H]=-2.3phys.abundfloat(-2.0)Prediction of [El/Fe] for ST, [Fe/H]=-2.0phys.abundfloat(-1.6)Prediction of [El/Fe] for ST, [Fe/H]=-1.6phys.abundfloat(-1.3)Prediction of [El/Fe] for ST, [Fe/H]=-1.3phys.abundfloat(-1.0)Prediction of [El/Fe] for ST, [Fe/H]=-1.0phys.abundfloat(-3.6)/12Prediction of [El/Fe] for ST/12, [Fe/H]=-3.6phys.abundfloat(-3.0)/12Prediction of [El/Fe] for ST/12, [Fe/H]=-3.0phys.abundfloat(-2.6)/12Prediction of [El/Fe] for ST/12, [Fe/H]=-2.6phys.abundfloat(-2.3)/12Prediction of [El/Fe] for ST/12, [Fe/H]=-2.3phys.abundfloat(-2.0)/12Prediction of [El/Fe] for ST/12, [Fe/H]=-2.0phys.abundfloat(-1.6)/12Prediction of [El/Fe] for ST/12, [Fe/H]=-1.6phys.abundfloat(-1.3)/12Prediction of [El/Fe] for ST/12, [Fe/H]=-1.3phys.abundfloat(-1.0)/12Prediction of [El/Fe] for ST/12, [Fe/H]=-1.0phys.abundfloat