Abstract
Stars in the globular cluster co Cen span a range of metallicities, from [Fe/H] from —1.8 to —0.8 (Norris et al. 1996, Suntzeff & Kraft 1996). High-resolution spectroscopic analyses of a number of red giant stars (Smith et al. 2000, Norris & Da Costa 1995) has allowed the abundance determination of many elements that can be classified under different groups. The first includes O, Na, Mg, and Al, which show anticorrelations of [Na/Fe] and [Al/Fe] versus [0/Fe] and [Mg/Fe] similar to what is observed in many globular clusters (Kraft 1994; Kraft et al. 1997). A complete interpretation of the behavior of these elements is still lacking. They might indicate deep internal mixing in the stars now evolving along the giant branch by the so-called cool bottom process (CBP) operating in low mass stars (Charbonnel 1994, 1995, Wasserburg, Boothroyd, & Sackmann 1995, Charbonnel, Brown, & Wallerstein 1998). The CPB phenomenon is possibly driven by rotation (Sweigart & Mengel 1979, Langer et al. 1998).
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Gallino, R., Smith, V.V., Busso, M., Cunha, K. (2000). Evolution of Heavy Elements in Omega Centauri: The Puzzle of S-Enrichment. In: Matteucci, F., Giovannelli, F. (eds) The Evolution of The Milky Way. Astrophysics and Space Science Library, vol 255. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0938-6_39
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