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There is now strong evidence for stars that have been born with initial helium mass fractions as high as Y=0.40, such as in the globular cluster Omega Centauri. However, the evolution, chemical yields, and final fates of helium-rich stars are poorly understood. In this talk, I will present results for the evolution and nucleosynthesis of asymptotic giant branch models with masses of 3 to 6 Msun at a metallicity of [Fe/H] ~= -1.4 with He-normal and He-rich compositions. I will also discuss the implications for chemical evolution and white dwarf remnant formation. |
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