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: firstname.lastname@example.org
2 Department of Physics, Northeastern State University, Tahlequah, OK 74464, USA e-mail: email@example.com
3 Dpto. de Física de Fusión y Partículas elementales, C.I.E.M.A.T., Avda. Complutense 22, 28040 Madrid, Spain e-mail: firstname.lastname@example.org
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
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.