Mixing along the Red Giant Branch in Metal-poor Field Stars

Details Mixing along the Red Giant Branch in Metal-poor Field Stars Mixing along the Red Giant Branch in Metal-poor Field Stars

1999-12-07

arxiv.org/abs/astro-ph/9912126v1

Astronomy and Astrophysics

Astrophysics

6 pages, 3 encapsulated figures, LateX, uses crckapb.sty; invited talk, in "The Chemical Evolution of the Milky Way: Stars vs

Scientific paper

We have determined Li, C, N, O, Na, and Fe abundances, and 12C/13C isotopic ratios for a sample of 62 field metal-poor stars (plus 43 taken from the literature). This large sample was used to show that small mass lower-RGB stars (i.e., fainter than the RGB bump) have abundances of light elements in agreement with theoretical predictions from classical evolutionary models. A second, distinct mixing episode occurs just after the RGB bump, reaching regions of incomplete CNO burning. No O-Na anticorrelation, as observed in globular cluster stars, is found in field stars. This means that the mixing episode is not deep enough to reach regions where ON-burning occurs.

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