Abstract
We present and show the features of the FRUITY database, an interactive web- based interface devoted to the nucleosynthesis in AGB stars. We describe the current available set of AGB models (largely expanded with respect to the original one) with masses in the range 1.3≤M/M⊙≤3.0 and metallicities –2.15 ≤[Fe/H]≤+0.15. We illustrate the details of our s-process surface distributions and we compare our results to observations. Moreover, we introduce a new set of models where the effects of rotation are taken into account. Finally, we shortly describe next planned upgrades.
Highlights
Asymptotic Giant Branch stars are exceptional laboratories to test the robustness of stellar models. Both light (C, N, F, Na) and heavy elements can be produced. The latter are synthesized via the slow neutron capture process
The structure of an AGB consists of a partially degenerate CO core, surrounded by an He-shell and an H-shell separated by a thin layer (He-intershell) and by a cool and expanded convective envelope
The surface luminosity is mainly sustained by the H-burning shell, active for most of the time. This situation is recurrently interrupted by the growing up of thermonuclear runaways driven by violent ignitions of 3α reactions at the base of the He-intershell (Thermal Pulses, hereafter TPs)
Summary
Asymptotic Giant Branch stars (hereafter AGBs) are exceptional laboratories to test the robustness of stellar models. These convective shells efficiently mix the He-intershell, enriching this layer in carbon (produced by 3α reactions) and in s-process elements. A marginal contribution comes from the 22Ne(α,n)25Mg reaction, which is activated at higher temperatures (T> 2.5 × 108 K) during TPs. The great amount of available spectroscopic data such as the need of yields for Chemical Evolution Models require the computation of a large number of detailed AGB evolutionary models.
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