| Issue |
A&A
Volume 447, Number 2, February IV 2006
|
|
|---|---|---|
| Page(s) | 641 - 647 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:20053956 | |
| Published online | 07 February 2006 | |
The s-process weak component: uncertainties due to convective overshooting
1
Istituto Nazionale di Astrofisica – Osservatorio Astrofisico di Catania (INAF-OAC), Città Universitaria, via S. Sofia 78, 95123 Catania, Italy e-mail: vcosta@oact.inaf.it
2
Università di Catania, Dipartimento di Fisica e Astronomia (sez. astrofisica), Città Universitaria, via S. Sofia 78, 95123 Catania, Italy
Received:
1
August
2005
Accepted:
29
September
2005
Using a new s-nucleosynthesis code, coupled with the stellar evolution code Star2003, we performed simulations to study the impact of the convection treatment on the s-process during core He-burning in a 
star (ZAMS mass) with an initial metallicity of 
.
Particular attention was devoted to the impact of the extent of overshooting on the s-process efficiency.
The results show enhancements of about a factor 
in s-process efficiency (measured as the average overproduction factor of the 6 s-only nuclear species with 
) with overshooting parameter values in the range 
, compared to results obtained with the same model but without overshooting. The impact of these results on the p-process model based on type II supernovae is discussed.
Key words: nuclear reactions, nucleosynthesis, abundances / convection / stars: evolution / stars: interiors
© ESO, 2006
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