J/A+A/635/A104ivo://CDS.VizieR/J/A+A/635/A104doi:10.26093/cds/vizier.36350104CDSHanke M.Hansen C.J.Ludwig H.-G.Cristallo S.McWilliam A.,Grebel E. K.Piersanti L.2021-03-10T09:21:27Z2020-03-16T06:12:38ZCDS support team

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

cds-question@unistra.fratomic-physicsspectroscopychemical-abundanceschemically-peculiar-starsline-intensitiesMetal-poor stars with available detailed information about their chemical inventory pose powerful empirical benchmarks for nuclear astrophysics. Here we present our spectroscopic chemical abundance investigation of the metal-poor ([Fe/H]=-1.60dex), r-process-enriched ([Eu/Fe]=0.73dex) halo star HD 20 using novel and archival high-resolution data at outstanding signal-to-noise ratios (up to 1000 per Angstroem). By combining one of the first asteroseismic gravity measurements in the metal-poor regime from a TESS light curve with the spectroscopic analysis of iron lines under non-local thermodynamic equilibrium conditions, we derive a set of highly accurate and precise stellar parameters. These allow us to delineate a reliable chemical pattern that is comprised of solid detections of 48 elements, including 28 neutron-capture elements. Hence, we establish HD 20 among the few benchmark stars that have almost complete patterns and possess low systematic dependencies on the stellar parameters. Our light-element (Z<30) abundances are representative of other, similarly metal-poor stars in the Galactic halo with contributions from core-collapse supernovae of type II. In the realm of the neutron-capture elements, our comparison to the scaled solar r-pattern shows that the lighter neutron-capture elements (Z<60) are poorly matched. In particular, we find imprints of the weak r-process acting at low metallicities. Nonetheless, by comparing our detailed abundances to the observed metal-poor star BD +17 3248, we find a persistent residual pattern involving mainly the elements Sr, Y, Zr, Ba, and La. These are indicative of enrichment contributions from the s-process and we show that mixing with material from predicted yields of massive, rotating AGB stars at low metallicity considerably improves the fit. Based on a solar ratio of heavy- to light-s elements -- at odds with model predictions for the i-process -- and a missing clear residual pattern with respect to other stars with claimed contributions from this process, we refute (strong) contributions from such astrophysical sites providing intermediate neutron densities. Finally, nuclear cosmochronology is used to tie our detection of the radioactive element Th to an age estimate for HD 20 of 11.0+/-3.8Gyr.2020A&A...635A.104Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/635/A104CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/635/A104https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/635/A104http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/635/A104https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/635/A104https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/635/A104http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/635/A104GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/635/A104/tablec1Atomic data, equivalent widths, and abundancesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelength0.1nmem.wldoubleIonIon designationphys.atmol.ionStagecharchiex? Excitation potentialeVphys.atmol.excitationfloatnullableloggf? Oscillator strengthphys.atmol.oscStrengthfloatnullableEW? Equivalent width0.1pmspect.line.eqWidthfloatnullablee_EW? Equivalent width error0.1pmstat.error;spect.line.eqWidthfloatnullablelogepsLTE abundancephys.abundfloate_logeps? LTE abundance errorstat.errorfloatnullablelogepsNLTE? NLTE abundancephys.abundfloatnullabledeltaNLTE? NLTE correctionarith.factorfloatnullableRefReference flag (1)meta.notecharNote[12, ]? Special note flag (2)meta.notecharl_logeps[3]? 3 for upper limit abundancemeta.code.errorintnullable