EDP Sciences
Free Access
Volume 432, Number 3, March IV 2005
Page(s) 861 - 877
Section Galactic structure, stellar clusters and populations
DOI https://doi.org/10.1051/0004-6361:20041949

A&A 432, 861-877 (2005)
DOI: 10.1051/0004-6361:20041949

Low and intermediate mass star yields: The evolution of carbon abundances

M. Gavilán1, J. F. Buell2 and M. Mollá3

1  Departamento de Física Teórica, Universidad Autónoma de Madrid, 28049 Cantoblanco, Spain
    e-mail: mgavilan@eresmas.net
2  Department of Physics, Northeastern State University, Tahlequah, OK 74464, USA
    e-mail: buell@cherokee.nsuok.edu
3  Dpto. de Física de Fusión y Partículas elementales, C.I.E.M.A.T., Avda. Complutense 22, 28040 Madrid, Spain
    e-mail: mercedes.molla@ciemat.es

(Received 5 September 2004 / 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 Woosley & Weaver (1995) 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