EDP Sciences
Free access
Volume 431, Number 1, February III 2005
Page(s) 279 - 288
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20041917

A&A 431, 279-288 (2005)
DOI: 10.1051/0004-6361:20041917

Full computation of massive AGB evolution

I. The large impact of convection on nucleosynthesis
P. Ventura and F. D'Antona

Osservatorio Astronomico di Roma, via Frascati 33, 00040 MontePorzio Catone, Italy
    e-mail: [ventura;dantona]@mporzio.astro.it

(Received 27 August 2004 / Accepted 3 October 2004)

It is well appreciated that the description of overadiabatic convection affects the structure of the envelopes of luminous asymptotic giant branch (AGB) stars in the phase of "hot bottom burning" (HBB). We stress that this important uncertainty in the modeling plays a role which is much more dramatic than the role which can be ascribed, e.g., to the uncertainty in the nuclear cross-sections. Due to the role tentatively attributed today to the HBB nucleosynthesis as the site of self-enrichment of Globular Clusters stars, it is necessary to explore the difference in nucleosynthesis obtained by different prescriptions for convection. We present results of detailed evolutionary calculations of the evolution of stars of intermediate mass during the AGB phase for the metallicity typical of the Globular Clusters that show the largest spread in CNO abundances ( $Z\sim 10^{-3}$). We follow carefully the nucleosynthesis at the base of the external convective region, showing that very different results can be obtained according to the presciption adopted to find out the temperature gradient within the instability regions. We discuss the uncertainties in the yields of the various chemical species and the role which these sources can play as polluters of the interstellar medium.

Key words: stars: evolution -- stars: interiors -- stars: AGB and post-AGB -- stars: abundances

SIMBAD Objects

© ESO 2005