Issue A&A Volume 484, Number 3, June IV 2008 Page(s) L27 - L30 Section Letters DOI http://dx.doi.org/10.1051/0004-6361:20079169 Published online 15 May 2008

A&A 484, L27-L30 (2008)
DOI: 10.1051/0004-6361:20079169

Letter

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

M. Lugaro^{1, 2}, S. E. de Mink¹, R. G. Izzard¹, S. W. Campbell^{2, 3}, A. I. Karakas⁴, S. Cristallo⁵, O. R. Pols¹, J. C. Lattanzio², O. Straniero⁵, R. Gallino^{2, 6}, and T. C. Beers<sup>7

1</sup>  Sterrekundig Instituut, Universiteit Utrecht, PO Box 80000, 3508 TA Utrecht, The Netherlands
    e-mail: [M.lugaro;s.e.demink;r.g.izzard;o.r.pols]@uu.nl
²  Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Victoria 3800, Australia
    e-mail: John.Lattanzio@sci.monash.edu.au
³  Academia Sinica Institute of Astronomy & Astrophysics, Taipei, Taiwan
    e-mail: simcam@asiaa.sinica.edu.tw
⁴  Research School of Astronomy and Astrophysics, Mt. Stromlo Observatory, Cotter Rd., Weston, ACT 2611, Australia
    e-mail: akarakas@mso.anu.edu.au
⁵  INAF, Osservatorio Astronomico di Collurania, 64100 Teramo, Italy
    e-mail: [cristallo;straniero]@oa-teramo.inaf.it
⁶  Dipartimento di Fisica Generale, Universitá di Torino, Torino, Italy
    e-mail: gallino@ph.unito.it
⁷  Department of Physics and Astronomy, Center for the Study of Cosmic Evolution, and Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, MI, USA
    e-mail: beers@pa.msu.edu

Received 30 November 2007 / Accepted 25 April 2008

Abstract
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 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  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 . 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 slow neutron-capture process.

Key words: stars: individual: HE 1305+0132 -- stars: AGB and post-AGB  -- stars: abundances -- nuclear reactions, nucleosynthesis, abundances

© ESO 2008

What is OpenURL?