Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...464l..57s&link_type=abstract
Astronomy and Astrophysics, Volume 464, Issue 3, March IV 2007, pp.L57-L60
Astronomy and Astrophysics
Astrophysics
49
Stars: Evolution, Stars: Binaries: General, Stars: Carbon, Stars: Abundances
Scientific paper
One possible scenario for the formation of carbon-enhanced metal-poor stars is the accretion of carbon-rich material from a binary companion which may no longer visible. It is generally assumed that the accreted material remains on the surface of the star and does not mix with the interior until first dredge-up. However, thermohaline mixing should mix the accreted material with the original stellar material as it has a higher mean molecular weight. We investigate the effect that this has on the surface abundances by modelling a binary system of metallicity Z=10-4 with a 2 M_&sun; primary star and a 0.74 M_&sun; secondary star in an initial orbit of 4000 days. The accretion of material from the wind of the primary leads to the formation of a carbon-rich secondary. We find that the accreted material mixes fairly rapidly throughout 90% of the star, with important consequences for the surface composition. Models with thermohaline mixing predict very different surface abundances after first dredge-up compared to canonical models of stellar evolution.
Glebbeek Evert
Izzard Robert G.
Pols Onno R.
Stancliffe Richard J.
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