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Fluorine in carbon-enhanced metal-poor stars: a binary scenario

Lugaro, Maria Anna; de Mink, S. E.; Izzard, R G; Campbell, S; Karakas, Amanda; Cristallo, S; Pols, O.R.; Lattanzio, John; Straniero, O; Gallino, Roberto; Beers, Timothy C

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Aims. A super-solar fluorine abundance was observed in the carbon-enhanced metal-poor (CEMP) star HE 1305+0132 ([F/Fe] = +2.90, [Fe/H] = -2.5). We propose that this observation can be explained using a binary model that involve mass transfer from an asymptotic giant branch (AGB) star companion and, based on this model, we predict F abundances in CEMP stars in general. We discuss wether F can be used to discriminate between the formation histories of most CEMP stars: via binary mass transfer or...[Show more]

dc.contributor.authorLugaro, Maria Anna
dc.contributor.authorde Mink, S. E.
dc.contributor.authorIzzard, R G
dc.contributor.authorCampbell, S
dc.contributor.authorKarakas, Amanda
dc.contributor.authorCristallo, S
dc.contributor.authorPols, O.R.
dc.contributor.authorLattanzio, John
dc.contributor.authorStraniero, O
dc.contributor.authorGallino, Roberto
dc.contributor.authorBeers, Timothy C
dc.date.accessioned2015-12-08T22:33:32Z
dc.identifier.issn0004-6361
dc.identifier.urihttp://hdl.handle.net/1885/34724
dc.description.abstractAims. A super-solar fluorine abundance was observed in the carbon-enhanced metal-poor (CEMP) star HE 1305+0132 ([F/Fe] = +2.90, [Fe/H] = -2.5). We propose that this observation can be explained using a binary model that involve mass transfer from an asymptotic giant branch (AGB) star companion and, based on this model, we predict F abundances in CEMP stars in general. We discuss wether F can be used to discriminate between the formation histories of most CEMP stars: via binary mass transfer or from the ejecta of fast-rotating massive stars.Methods. We compute AGB yields using different stellar evolution and nucleosynthesis codes to evaluate stellar model uncertainties. We use a simple dilution model to determine the factor by which the AGB yields should be diluted to match the abundances observed in HE 1305+0132. We further employ a binary population synthesis tool to estimate the probability of F-rich CEMP stars.Results. The abundances observed in HE 1305+0132 can be explained if this star accreted 3-11% of the mass lost by its former AGB companion. The primary AGB star should have dredged-up at least 0.2 M⊗ of material from its He-rich region into the convective envelope via third dredge-up, which corresponds to AGB models of Z ≃ 0.0001 and mass ≃ 2 M⊗. Many AGB model uncertainties, such as the treatment of convective borders and mass loss, require further investigation. We find that in the binary scenario most CEMP stars should also be FEMP stars, that is, have [F/Fe] > +1, while fast-rotating massive stars do not appear to produce fluorine. We conclude that fluorine is a signature of low-mass AGB pollution in CEMP stars, together with elements associated with the neutron-capture process.
dc.publisherSpringer
dc.sourceAstronomy and Astrophysics
dc.subjectKeywords: Astrophysics; Carbon; Chemical elements; Fluorine; Helium; Mass transfer; Microfluidics; Rotation; Steel analysis; Uncertainty analysis; (e ,3e) process; Asymptotic giant branch (AGB); binary models; Convective borders; Convective envelope; General (CO); Nuclear reactions, nucleosynthesis, abundances; Stars: abundances; Stars: AGB and post-AGB; Stars: individual: HE 1305+0132
dc.titleFluorine in carbon-enhanced metal-poor stars: a binary scenario
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume484
dc.date.issued2008
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.ariespublicationu4362859xPUB116
local.type.statusPublished Version
local.contributor.affiliationLugaro, Maria Anna, Utrecht University
local.contributor.affiliationde Mink, S. E., Universiteit Utrecht
local.contributor.affiliationIzzard, R G, University of Cambridge
local.contributor.affiliationCampbell, S, Monash University
local.contributor.affiliationKarakas, Amanda, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationCristallo, S, INAF, Osservatorio Astronomico di Collurania
local.contributor.affiliationPols, O.R., Astronomical Institute Utrecht
local.contributor.affiliationLattanzio, John, Monash University
local.contributor.affiliationStraniero, O, INAF-Osservatorio Astronomico di Teramo
local.contributor.affiliationGallino, Roberto, Universita di Torino
local.contributor.affiliationBeers, Timothy C, Michigan State University
local.description.embargo2037-12-31
local.bibliographicCitation.startpageL27
local.bibliographicCitation.lastpageL30
local.identifier.doi10.1051/0004-6361:20079169
dc.date.updated2015-12-08T09:36:40Z
local.identifier.scopusID2-s2.0-44849116271
local.identifier.thomsonID000256511100003
CollectionsANU Research Publications

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