The CEMP star SDSSJ0222–0313: the first evidence of proton ingestion in very low-metallicity AGB stars?

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dc.contributor.authorCaffau, E.
dc.contributor.authorMonaco, L.
dc.contributor.authorBonifacio, P.
dc.contributor.authorKorotin, S.
dc.contributor.authorAndrievsky, Serhii M.
dc.contributor.authorCristallo, S.
dc.contributor.authorSpite, M.
dc.contributor.authorSpite, F.
dc.contributor.authorSbordone, L.
dc.contributor.authorFrançois, P.
dc.contributor.authorCescutti, G.
dc.contributor.authorSalvadori, S.
dc.contributor.authorАндрієвський, Сергій Михайлович
dc.contributor.authorАндриевский, Сергей Михайлович
dc.date.accessioned2022-06-03T11:59:56Z
dc.date.available2022-06-03T11:59:56Z
dc.date.issued2019
dc.description.abstractContext. Carbon-enhanced metal-poor (CEMP) stars are common objects in the metal-poor regime. The lower the metallicity we look at, the larger the fraction of CEMP stars with respect to metal-poor stars with no enhancement in carbon. The chemical pattern of CEMP stars is diversified, strongly suggesting a different origin of the C enhancement in the different types of CEMP stars. Aims. We selected a CEMP star, SDSS J0222–0313, with a known high carbon abundance and, from a low-resolution analysis, a strong enhancement in neutron-capture elements of the first peak (Sr and Y) and of the second peak (Ba). The peculiarity of this object is a greater overabundance (with respect to iron) of the first s-process peak than the second s-process peak. Methods. We analysed a high-resolution spectrum obtained with the Mike spectrograph at the Clay Magellan 6.5m telescope in order to derive the detailed chemical composition of this star. Results. We confirmed the chemical pattern we expected; we derived abundances for a total of 18 elements and significant upper limits. Conclusions. We conclude that this star is a carbon-enhanced metal-poor star enriched in elements produced by s-process (CEMP-s), whose enhancement in heavy elements is due to mass transfer from the more evolved companion in its asymptotic giant branch (AGB) phase. The abundances imply that the evolved companion had a low main sequence mass and it suggests that it experienced a proton ingestion episode at the beginning of its AGB phase.uk_UA
dc.identifier.citationAstronomy & Astrophysicsuk_UA
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201935680
dc.identifier.urihttps://dspace.onu.edu.ua/handle/123456789/33027
dc.language.isoenuk_UA
dc.relation.ispartofseries;A&A 628, A46
dc.subjectstarsuk_UA
dc.subjectcarbonuk_UA
dc.subjectabundancesuk_UA
dc.subjectPopulation IIuk_UA
dc.subjectGalaxyuk_UA
dc.subjecthalouk_UA
dc.titleThe CEMP star SDSSJ0222–0313: the first evidence of proton ingestion in very low-metallicity AGB stars?uk_UA
dc.typeArticleuk_UA
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11. Caffau, E., L. Monaco, P. Bonifacio, S. Korotin, S. Andrievsky, S. Cristallo, M. Spite, et al. 2019. The CEMP Sta.pdf
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