TY - JOUR
T1 - Population synthesis of binary carbon-enhanced metal-poor stars
AU - Izzard, Robert George
AU - Glebbeek, Evert
AU - Stancliffe, Richard James
AU - Pols, Onno R
PY - 2009
Y1 - 2009
N2 - 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.
AB - 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.
UR - http://apps.isiknowledge.com.ezproxy.lib.monash.edu.au/full_record.do?product=UA&search_mode=GeneralSearch&qid=1&SID=4B78Ka8f4lL4BC8mnh2&page=1&doc=1&
M3 - Article
SN - 0004-6361
VL - 508
SP - 1359
EP - 1374
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
IS - 3
ER -