Mixing And Mass Transfer In Carbon-Enhanced Metal-Poor Stars

Details Mixing And Mass Transfer In Carbon-Enhanced Metal-Poor Stars Mixing And Mass Transfer In Carbon-Enhanced Metal-Poor Stars

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21341604m&link_type=abstract

American Astronomical Society, AAS Meeting #213, #416.04; Bulletin of the American Astronomical Society, Vol. 41, p.227

Astronomy and Astrophysics

Astronomy

Scientific paper

Carbon-Enhanced Metal-Poor (CEMP) stars have been seen to make up a large fraction of metal-poor stars ( 30% below [Fe/H] = -3.0). These stars often show enhancements of s-process material, which is believed to have formed near the core of an AGB star, is mixed to the surface during third dredge-up, and then transferred via Roche Lobe overflow to a binary companion. Thus, observed CEMP stars are thought to be mainly the surviving secondary stars of binary systems. These stars are thus useful probes of a number of quantities, including the efficiencies of (1) carbon and s-process production as a function of metallicity, (2) mixing during third dredge-up, (3) mass transfer during Roche Lobe overflow, and (4) the subsequent mixing during the evolution of the secondary star. We report here several projects in progress studying stars at a variety of stages along this path, over a range of metallicities, to probe these mechanisms in greater detail.

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