A chemodynamical analysis of bright metal-poor stars from the HESP-GOMPA survey - indications of a non-prevailing site for light <i>r</i>-process elements

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dc.contributor.authorBandyopadhyay, Avrajit
dc.contributor.authorBeers, Timothy C.
dc.contributor.authorEzzeddine, Rana
dc.contributor.authorSivarani, Thirupathi
dc.contributor.authorNayak, Prasanta K.
dc.contributor.authorPandey, Jeewan C.
dc.contributor.authorSaraf, Pallavi
dc.contributor.authorSusmitha, Antony
dc.date.accessioned2025-01-20T17:06:18Z
dc.date.available2025-01-20T17:06:18Z
dc.date.issued2024
dc.description.abstractWe present a comprehensive analysis of the detailed chemical abundances for a sample of 11 metal-poor, very metal-poor, and extremely metal-poor stars ([Fe/H] = -1.65 to [Fe/H] = -3.0) as part of the HESP-GOMPA (Galactic survey Of Metal Poor stArs) survey. The abundance determinations encompass a range of elements, including C, Na, Mg, Al, Si, Ca, Sc, Ti, Cr, Mn, Fe, Co, Ni, Cu, Zn, Sr, and Ba, with a subset of the brighter objects allowing for the measurement of additional key elements. Notably, the abundance analysis of a relatively bright highly r-process-enhanced (r-II) star (SDSS J0019+3141) exhibits a predominantly main r-process signature and variations in the lighter r-process elements. Moreover, successful measurements of thorium in this star facilitate stellar age determinations. We find a consistent odd-even nucleosynthesis pattern in these stars, aligning with expectations for their respective metallicity levels, thus implicating Type II supernovae as potential progenitors. From the interplay between the light and heavy r-process elements, we infer a diminishing relative production of light r-process elements with increasing Type II supernova contributions, challenging the notion that Type II supernovae are the primary source of these light r-process elements in the early Milky Way. A chemodynamical analysis based on Gaia astrometric data and our derived abundances indicates that all but one of our program stars are likely to be of accreted origin. Additionally, our examination of alpha-poor stars underscores the occurrence of an early accretion event from a satellite on a prograde orbit, similar to that of the Galactic disc.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stae613
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stae613
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/90775
dc.identifier.wosidWOS:001187239400001
dc.issue.numero3
dc.language.isoen
dc.pagina.final2207
dc.pagina.inicio2191
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjecttechniques: spectroscopic
dc.subjectstars: abundances
dc.subjectstars: atmospheres
dc.subjectstars: fundamental parameters
dc.subjectGalaxy: formation
dc.titleA chemodynamical analysis of bright metal-poor stars from the HESP-GOMPA survey - indications of a non-prevailing site for light <i>r</i>-process elements
dc.typeartículo
dc.volumen529
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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