Population synthesis of binary carbon-enhanced metal-poor stars

Robert George Izzard, Evert Glebbeek, Richard James Stancliffe, Onno R Pols

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The carbon-enhanced metal-poor (CEMP) stars constitute approximately one fifth of the metal-poor ([Fe/H] less than or similar to -2) population but their origin is not well understood. The most widely accepted formation scenario, at least for the majority of CEMP stars which are also enriched in s-process elements, invokes mass-transfer of carbon-rich material from a thermally-pulsing asymptotic giant branch (TPAGB) primary star to a less massive main-sequence companion which is seen today. Recent studies explore the possibility that an initial mass function biased toward intermediate-mass stars is required to reproduce the observed CEMP fraction in stars with metallicity [Fe/H] <-2.5.
Original languageEnglish
Pages (from-to)1359 - 1374
Number of pages16
JournalAstronomy & Astrophysics
Issue number3
Publication statusPublished - 2009

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