Carbon and Oxygen Galactic Abundance Gradients: A Comparative Study of Stellar Yields

Abstract

Chemical evolution models for the Galactic disk under an inside-out formation scenario are presented for seven sets of stellar yields, all of them metal dependent. In particular, the effects of yields from massive and low-and-intermediate-mass stars on the C/O chemical history of the solar neighborhood and on abundance gradients are discussed comparing the predictions with abundance ratios from nearby HII regions, B-stars, dwarf stars, and the Sun. In the solar vicinity, the increase of C/O with metallicity is due to massive stars alone. Models with yields by Maeder (1992) or by Portinari, Chiosi, & Bressan (1998) reproduce the observed C/O increase with metallicity, while models assuming yields by Woosley & Weaver (1995) and Woosley, Langer, & Weaver (1993) do not. Models based on yields by Maeder (1992) are in agreement with the C/O gradient, while those based on yields by Portinari et al. (1998) or by Woosley & Weaver (1995) and Woosley et al. (1993) are not. To match both, the C/O enrichment history of the solar neighborhood and the C/O local gradient, models call for: i) yields that take into account metal-dependent stellar winds; and ii) for massive stars, a mass-loss rate with a metallicity dependence not as simple as Z^{0.5}. C/O abundance ratios predicted with yields by Marigo, Bressan, & Chiosi (1996, 1998) are higher than those with yields by Renzini & Voli (1981), which in turn are higher than those with yields by the van den Hoek & Groenewegen (1997).