Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/8190
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dc.contributor.authorGoswami, P. P-
dc.contributor.authorGoswami, A-
dc.date.accessioned2023-05-04T05:30:15Z-
dc.date.available2023-05-04T05:30:15Z-
dc.date.issued2023-04-01-
dc.identifier.citationThe Astronomical Journal, Vol.165, No. 4, 154en_US
dc.identifier.issn1538-3881-
dc.identifier.urihttp://hdl.handle.net/2248/8190-
dc.descriptionOpen Accessen_US
dc.descriptionOriginal content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.-
dc.description.abstractWe have performed detailed high-resolution spectroscopic analysis on seven metal-poor stars (BD+75 348, BD +09 3019, HD238020, HE0319–0215, HE0507–1653, HE0930–0018, HE1023–1504) and derived their atmospheric parameters Teff, log g, [Fe/H], and microturbulent velocity (ξ). The metallicity range is found to be –2.57 < [Fe/H] < –0.42. The elemental abundances of 17 light elements and 12 heavy elements are estimated. We have classified BD+75 348 and BD+09 3019 as strong Ba stars, HD238020 as a mild Ba star, and the remaining four objects as CEMP-s stars. We have estimated the masses of the stars from Hertzsprung–Russel (HR) diagram, and, compiling the data of 205 Ba stars from literature, estimated the mass distribution of Ba stars. We have also estimated the initial masses of the companion AGBs of the program stars as well as the masses of the companion AGBs of 159 Ba and 36 CEMP-s stars from literature, with the help of a parametric-model-based analysis using FRUITY models. While the primary mass distribution of mild Ba stars peaks at 3.7 Me, for the strong Ba stars the peak appears at 2.5 Me. We, therefore, propose that the initial masses of the progenitor AGBs dominantly control the formation of mild and strong Ba stars. However, a clear overlap, in the range 1.3–4.0 Me, noticed between the progenitor masses of both the subclasses of Ba stars, may indicate that other factors, such as the metallicities and the orbital periods, may also have significant contributions. The progenitor AGBs’ mass distribution of CEMP-s stars is found to peak at 2.03 M☉en_US
dc.language.isoenen_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.urihttps://doi.org/10.3847/1538-3881/aca971-
dc.rights© 2023. The Author(s).-
dc.subjectCEMP starsen_US
dc.subjectBarium starsen_US
dc.subjectCarbon starsen_US
dc.subjectChemically peculiar starsen_US
dc.subjectHertzsprung Russell diagramen_US
dc.subjectStellar physicsen_US
dc.subjectAsymptotic giant branch starsen_US
dc.subjectChemical abundancesen_US
dc.subjectS-processen_US
dc.subjectSpectroscopyen_US
dc.titleSpectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitorsen_US
dc.typeArticleen_US
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