S-process nucleosynthesis in AGB stars with the full spectrum of turbulence scheme for convection.

A Yagüe,P Ventura,M Lugaro,D A García-Hernández

doi:10.1088/1742-6596/728/7/072004

Abstract

The chemical evolution of asymptotic giant branch (AGB) stars models depends greatly on the input physics (e.g. convective model, mass loss recipe). Variations of hot bottom burning (HBB) strength, or third dredge-up (TDU) efficiency are among the main consequences of adopting different input physics in the AGB models. The ATON evolutionary code stands apart from others in that it uses the Full Spectrum of Turbulence convective model. Here we present the first results of a newly developed s-process nucleosynthesis module for ATON AGB models. Our results are compared also with observations and theoretical predictions of present AGB nucleosynthesis models using different input physics.

Highlights

1.1 Stellar evolution: from the main sequence to the thermally pulsing asymptotic giant branch (TP-Asymptotic Giant Branch (AGB))From the first fusion reaction to the last, the behavior and evolution of a star is dominated mainly by its structure, initial mass, and chemical composition
We have found that the GS method is an adequate alternative to an LU factorization when solving the sparse system of linear equations that arise during the application of an implicit method when applied to our AGB nucleosynthesis simulations
We have shown that SNUPPAT is able to follow a much better stablished AGB evolutionary code such as ATON along several thermal pulse (TP), giving the correct intershell abundances for most of the species followed by the computations

Summary

Introduction

1.1 Stellar evolution: from the main sequence to the TP-AGBFrom the first fusion reaction to the last, the behavior and evolution of a star is dominated mainly by its structure, initial mass, and chemical composition. We must test the complete code to ensure that the interplay between the nucleosynthesis and mixing mechanisms is working as intended in our interest to accurately portray the s-process nucleosynthesis, as well as the impact on the evolution of the stellar surface chemistry. For this we have chosen ATON, the very same evolutionary code we wish to apply post-processing to, understanding that consistency with it is essential for our objective. In order to conduct a meaningful conversation on the differ-

Objectives

Results

Conclusion