VESCOVI, DiegoDiegoVESCOVICRISTALLO, SergioSergioCRISTALLOPalmerini, S.S.PalmeriniAbia, C.C.AbiaBusso, M.M.Busso2022-03-112022-03-1120210004-6361http://hdl.handle.net/20.500.12386/31552Asymptotic giant branch (AGB) stars are considered to be among the most significant contributors to the fluorine budget in our Galaxy. While observations and theory agree at close-to-solar metallicity, stellar models at lower metallicities overestimate the fluorine production with respect to that of heavy elements. We present <SUP>19</SUP>F nucleosynthesis results for a set of AGB models with different masses and metallicities in which magnetic buoyancy acts as the driving process for the formation of the <SUP>13</SUP>C neutron source (the so-called <SUP>13</SUP>C pocket). We find that <SUP>19</SUP>F is mainly produced as a result of nucleosynthesis involving secondary <SUP>14</SUP>N during convective thermal pulses, with a negligible contribution from the <SUP>14</SUP>N present in the <SUP>13</SUP>C pocket region. A large <SUP>19</SUP>F production is thus prevented, resulting in lower fluorine surface abundances. As a consequence, AGB stellar models with mixing induced by magnetic buoyancy at the base of the convective envelope agree well with available fluorine spectroscopic measurements at low and close-to-solar metallicity.STAMPAenArticle10.1051/0004-6361/2021411732-s2.0-85112095096WOS:000686499900001https://www.aanda.org/articles/aa/abs/2021/08/aa41173-21/aa41173-21.htmlhttp://arxiv.org/abs/2106.08241v12021A&A...652A.100VFIS/05 - ASTRONOMIA E ASTROFISICA