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dc.contributor.authorMura-Guzmán, A.
dc.contributor.authorYong, D.
dc.contributor.authorAbate, C.
dc.contributor.authorKarakas, A.
dc.contributor.authorKobayashi, C.
dc.contributor.authorOh, H.
dc.contributor.authorChun, S.
dc.contributor.authorMace, G.
dc.contributor.author.
dc.date.accessioned2020-09-24T00:10:29Z
dc.date.available2020-09-24T00:10:29Z
dc.date.issued2020-11-01
dc.identifier.citationMura-Guzmán , A , Yong , D , Abate , C , Karakas , A , Kobayashi , C , Oh , H , Chun , S , Mace , G & . 2020 , ' Constraining Nucleosynthesis in Two CEMP Progenitors Using Fluorine ' , Monthly Notices of the Royal Astronomical Society , vol. 498 , no. 3 , staa2610 , pp. 3549–3559 . https://doi.org/10.1093/mnras/staa2610
dc.identifier.issn0035-8711
dc.identifier.otherArXiv: http://arxiv.org/abs/2008.10136v2
dc.identifier.otherORCID: /0000-0002-4343-0487/work/80948509
dc.identifier.urihttp://hdl.handle.net/2299/23169
dc.description© 2020 The Author(s). The version of record [Aldo Mura-Guzmán, D Yong, C Abate, A Karakas, C Kobayashi, H Oh, S-H Chun, G Mace, Constraining nucleosynthesis in two CEMP progenitors using fluorine, Monthly Notices of the Royal Astronomical Society, Volume 498, Issue 3, November 2020, Pages 3549–3559] is available online at: https://doi.org/10.1093/mnras/staa2610.
dc.description.abstractWe present new fluorine abundance estimations in two carbon enhanced metal-poor (CEMP) stars, HE 1429-0551 and HE 1305+0007. HE 1429-0551 is also enriched in slow neutron-capture process (s-process) elements, a CEMP-s, and HE 1305+0007 is enhanced in both, slow and rapid neutron-capture process elements, a CEMP-s/r. The F abundances estimates are derived from the vibration-rotation transition of the HF molecule at 23358.6 Š using high-resolution infrared spectra obtained with the Immersion Grating Infrared Spectrometer (IGRINS) at the 4-m class Lowell Discovery Telescope. Our results include an F abundance measurement in HE 1429-0551 of A(F) = +3.93 ([F/Fe] = +1.90) at [Fe/H] = -2.53, and an F upper limit in HE 1305+0007 of A(F) < +3.28 ([F/Fe] < +1.00) at [Fe/H] = -2.28. Our new derived F abundance in HE 1429-0551 makes this object the most metal-poor star where F has been detected. We carefully compare these results with literature values and state-of-the-art CEMP-s model predictions including detailed asymptotic giant branch (AGB) nucleosynthesis and binary evolution. The modelled fluorine abundance for HE 1429-0551 is within reasonable agreement with our observed abundance, although is slightly higher than our observed value. For HE 1429-0551, our findings support the scenario via mass transfer by a primary companion during its thermally pulsing phase. Our estimated upper limit in HE 1305+0007, along with data from the literature, shows large discrepancies compared with AGB models. The discrepancy is principally due to the simultaneous s- and r-process element enhancements which the model struggles to reproduce.en
dc.format.extent11
dc.format.extent2022570
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectastro-ph.SR
dc.subjectastro-ph.GA
dc.subjectstars: AGB and post-AGB
dc.subjectstars: chemically peculiar
dc.subjectstars: abundances
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleConstraining Nucleosynthesis in Two CEMP Progenitors Using Fluorineen
dc.contributor.institutionCentre for Astrophysics Research (CAR)
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85096845545&partnerID=8YFLogxK
rioxxterms.versionofrecord10.1093/mnras/staa2610
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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