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Low mass Asymptotic Giant Branch stars are among the most important pollutersof the interstellar medium. In their interiors, the main component (A>90) ofthe slow neutron capture process (the s-process) is synthesized, the mostimportant neutron source being the 13C(alpha,n)16O reaction. In this paper wereview its current experimental status discussing possible future synergiesbetween some experiments currently focused on the determination of its rate.Moreover, in order to determine the level of precision needed to fullycharacterize this reaction, we present a theoretical sensitivity study, carriedout with the FUNS evolutionary stellar code and the NEWTON post-process code.We modify the rate up to a factor of two with respect to a reference case. Wefind that variations of the 13C(alpha,n)16O rate do not appreciably affects-process distributions for masses above 3 Msun at any metallicity. Apart froma few isotopes, in fact, the differences are always below 5%. The situation iscompletely different if some 13C burns in a convective environment: this occursin FUNS models with M<3 Msun at solar-like metallicities. In this case, achange of the 13C(alpha,n)16O reaction rate leads to non-negligible variationsof the elements Surface distribution (10% on average), with larger peaks forsome elements (as rubidium) and for neutron-rich isotopes (as 86Kr and 96Zr).Larger variations are found in low-mass low-metallicity models, if protons aremixed and burnt at very high temperatures. In this case, the surface abundancesof the heavier elements may vary by more than a factor 50.

The importance of the 13C(alpha,n)16O reaction in Asymptotic Giant Branch stars