Volume 432, Number 3, March IV 2005
|Page(s)||861 - 877|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||07 March 2005|
Low and intermediate mass star yields: The evolution of carbon abundances*
Departamento de Física Teórica, Universidad Autónoma de Madrid, 28049 Cantoblanco, Spain e-mail: email@example.com
2 Department of Physics, Northeastern State University, Tahlequah, OK 74464, USA e-mail: firstname.lastname@example.org
3 Dpto. de Física de Fusión y Partículas elementales, C.I.E.M.A.T., Avda. Complutense 22, 28040 Madrid, Spain e-mail: email@example.com
Accepted: 8 November 2004
We present a set of low and intermediate mass star yields based on a modeling of the TP-AGB phase which affects the production of nitrogen and carbon. These yields are evaluated by using them in a Galaxy Chemical Evolution model, with which we analyze the evolution of carbon abundances. By comparing the results with those obtained with other yield sets, and with a large amount of observational data, we conclude that the model using these yields combined with those from [CITE] for massive stars properly reproduce all the data. The model reproduces well the increase of C/O with increasing O/H abundances. Since these massive star yields do not include winds, it implies that these stellar winds might have a smoother dependence on metallicity than usually assumed and that a significant quantity of carbon proceeds from LIM stars.
Key words: Galaxy: abundances / stars: evolution / Galaxy: abundances / Galaxy: evolution / galaxies: spiral
© ESO, 2005
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