Volume 459, Number 1, November III 2006
|Page(s)||125 - 135|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||12 September 2006|
First stars X. The nature of three unevolved carbon-enhanced metal-poor stars
Department of Physics & Astronomy, CSCE: Center for the Study of Cosmic Evolution, and JINA: Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, MI 48824, USA e-mail: firstname.lastname@example.org
2 CIFIST Marie Curie Excellence Team
3 Observatoire de Paris, GEPI, 92195 Meudon Cedex, France
4 Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Trieste, via Tiepolo 11, 34131 Trieste, Italy
5 Los Alamos National Laboratory (LANL), Los Alamos, New Mexico, NM 87545, USA
6 GRAAL, Université de Montpellier II, 34095 Montpellier Cedex 05, France
7 The Niels Bohr Institute, Astronomy, Juliane Maries Vej 30, 2100 Copenhagen, Denmark
8 Nordic Optical Telescope Scientific Association, Apartado 474, 38 700 Santa Cruz de La Palma, Spain
9 Universidade de Sao Paulo, Departamento de Astronomia, Rua do Matao 1226, 05508-900 Sao Paulo, Brazil
10 European Southern Observatory (ESO), 3107 Alonso de Cordova, Vitacura, Casilla 19001, Santiago 19, Chile
11 Lund Observatory, Box 43, 221 00 Lund, Sweden
12 European Southern Observatory (ESO), Karl-Schwarschild-Str. 2, 85749 Garching b. München, Germany
Accepted: 8 July 2006
Context.On the order of 20% of the very metal-poor stars in the Galaxy exhibit large carbon enhancements. It is important to establish which astrophysical sites and processes are responsible for the elemental abundance patterns of this early Galactic population.
Aims.We seek to understand the nature of the progenitors of three main-sequence turnoff Carbon-Enhanced Metal-Poor (CEMP) stars, CS 31080-095, CS 22958-042, and CS 29528-041, based on a detailed abundance analysis.
Methods.From high-resolution VLT/UVES spectra (), we determine abundances or upper limits for Li, C, N, O, and other important elements, as well as 12C/13C isotopic ratios.
Results.All three stars have and moderate to high CNO abundances. CS 22958-042 is one of the most carbon-rich CEMP stars known ([ C/Fe), while CS 29528-041 (one of the few N-enhanced metal-poor stars known) is one of the most nitrogen rich ([ N/Fe). Oxygen is very high in CS 31080-095 ([ O/Fe) and in CS 22958-042 ([ O/Fe). All three stars exhibit [ Sr/Fe; Ba is not detected in CS 22958-042 ([ Ba/Fe), but it is moderately enhanced ([ Ba/Fe) in the other two stars. CS 22958-042 displays one of the largest sodium overabundances yet found in CEMP stars ([ Na/Fe). CS 22958-042 has 12C/, similar to most other CEMP stars without enhanced neutron-capture elements, while 12C/ in CS 31080-095. CS 31080-095 and CS 29528-041 have A(Li, below the Spite Plateau, while Li is not detected in CS 22958-042.
Conclusions.CS 22958-042 is a CEMP-no star, but the other two stars are in no known class of CEMP star and thus either constitute a new class or are a link between the CEMP-no and CEMP-s classes, adding complexity to the abundance patterns for CEMP stars. We interpret the abundance patterns in our stars to imply that current models for the presumed AGB binary progenitors lack an extra-mixing process, similar to those apparently operating in RGB stars.
Key words: stars: abundances / stars: population II / Galaxy: abundances / stars: AGB and post-AGB
© ESO, 2006
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