S.Uttenthaler (1), T. Lebzelter (1), M. Busso (2), S. Palmerini (3,4), B.Aringer (1), and M. Schultheis (5) ((1) University of Vienna, Department of Astrophysics, Türkenschanzstraße 17, 1180 Vienna, Austria; (2) Dipartimento di Fisica, Universitá di Perugia, and INFN, Sezione di Perugia. Via Pascoli, 06123 Perugia, Italy; (3) Centro Siciliano di Fisica Nucleare e Struttura dalla Materia, Viale A. Doria, 6 – 95125
Catania, Italy; (4) Laboratori Nazionali del Sud I.N.F.N., via S. Sofia 62, Catania, Italy; (5) Institut Utinam, CNRS UMR6213, OSU THETA, Université de Franche-Comté, 41bis
avenue de l’Observatoire, 25000 Besanc¸on, France)
According to standard stellar evolution, lithium is destroyed throughout most of the evolution of low- to intermediate-mass stars. However, a number of evolved stars on the red giant branch (RGB) and the asymptotic giant branch (AGB) are known to contain a considerable amount of Li, whose origin is not always understood well. Here we present the latest development on the observational side to obtain a better understanding of Li-rich K giants (RGB), moderately Li-rich low-mass stars on the AGB, as well as very Li-rich intermediate-mass AGB stars possibly undergoing the standard hot bottom burning phase. These last ones probably also enrich the interstellar medium with freshly produced Li.
Complete preprint ==> http://arxiv.org/abs/1206.2759