First Dredge-Up and further Mixing Mechanisms along the Red Giant Branch in Field Stars

Abstract

In this research we use a large sample of field metal-poor stars ([Fe/H]<-1) in different evolutionary phases to prove observationally that (small mass) subgiants (stars brighter than the first dredge-up and fainter than the RGB bump) have abundances of light elements in agreement with predictions from classical evolutionary models. A further mixing episode occurs just after the RGB bump, in agreement with the predictions by Charbonnel (1994, A&A, 282, 811; 1995, ApJ, 453, L41) The O-Na anti-correlation, typical signature observed amongst globular cluster giants, is not present amongst field stars.

2 pages, 1 figure, LaTex, uses crckapb.sty, poster paper to appear in the proceedings of the meeting "Galaxy Evolution: Connecting the Distant Universe with the Local Fossil Record", Observatoire de Paris-Meudon, 21-25 September 1998

References in corpus (1)

• A consistent explanation for ${}^{12}$C/${}^{13}$C, ${}^7$Li, and ${}^3$He anomalies in red giant stars

Cited by in corpus (4)

• The r-Process Enriched Low Metallicity Giant HD 115444
• An Abundance Analysis for Five Red Horizontal Branch Stars in the Extremely Metal Rich Globular Cluster NGC 6553
• Rubidium in Metal-Deficient Disk and Halo Stars
• Local Stellar Kinematics from RAVE data - VII. Metallicity Gradients from Red Clump Stars