000008048 001__ 8048
000008048 005__ 20260306091349.0
000008048 0247_ $$2DOI$$a10.3847/1538-4357/ae12a0
000008048 037__ $$aSCART-2026-0132
000008048 100__ $$a Riyas, A. M.
000008048 245__ $$aAbundance of Heavy r-process Elements in CEMP-rs Stars: The Role of the i-process
000008048 260__ $$c2026
000008048 520__ $$aCarbon-enhanced metal-poor (CEMP) stars are ancient stars enriched in carbon and heavy elements. Some of these stars exhibit enhanced s-process and/or r-process elements, and hence are classified as CEMP-s, CEMP-rs, or CEMP-r. This classification is challenging due to the limited availability of heavy element abundances, particularly among r-process elements. Heavy r-process elements such as terbium, holmium, thulium, ytterbium, lutetium, tantalum, and iridium have rarely been measured because their sensitive lines are located in the ultraviolet. However, they provide sensitive diagnostics of the s-, r-, and i- nucleosynthetic processes. In this work, we aim to obtain a secure classification of CEMP-s and -rs stars and investigate whether the i-process can account for the measured abundance patterns in CEMP-rs stars. We derive the abundance profiles, notably for 12 heavy r-elements, including, in some cases, tantalum, using high-resolution UVES spectra of 17 CEMP-s and -rs stars. Based on indicators such as the [s/r] abundance ratio or the model-independent "abundance distance", nine stars are confirmed as CEMP-rs and six as CEMP-s. The classification of two objects remains uncertain. The i-process satisfactorily reproduces the abundance patterns of CEMP-rs stars. However, larger samples are needed to confirm trends with metallicity and clarify how CEMP-rs stars differ from CEMP-s stars. 
000008048 536__ $$aBELSPO/$$cFED-tWIN Prf-2020-033 BISTRO/$$fFED-tWIN Prf-2020-033 BISTRO
000008048 594__ $$aNO
000008048 6531_ $$aChemical abundances
000008048 6531_ $$aStellar nucleosynthesis
000008048 6531_ $$aAsymptotic giant branch stars
000008048 6531_ $$aBinary stars
000008048 700__ $$aKarinkuzhi, D.
000008048 700__ $$aVan Eck, S.
000008048 700__ $$aChoplin, A.
000008048 700__ $$aGoriely, S.
000008048 700__ $$aSiess, L.
000008048 700__ $$aKeerthy, M. V. 
000008048 700__ $$aJorissen, A.
000008048 700__ $$aMerle, T. 
000008048 773__ $$c29$$n1$$pThe Astrophysical Journal$$v997$$y2026
000008048 8560_ $$fthibault.merle@ksb-orb.be
000008048 85642 $$ahttps://iopscience.iop.org/article/10.3847/1538-4357/ae12a0
000008048 85642 $$ahttps://arxiv.org/abs/2510.13339
000008048 8564_ $$s3211497$$uhttps://publi2-as.oma.be/record/8048/files/Riyas_2026_ApJ_997_44.pdf
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000008048 8564_ $$s25905$$uhttps://publi2-as.oma.be/record/8048/files/Riyas_2026_ApJ_997_44.jpg?subformat=icon-180$$xicon-180
000008048 905__ $$apublished in
000008048 980__ $$aREFERD