Presolar grain isotopic ratios as constraints to nuclear physics inputs for s-process calculations

¹ Department of Physics and Geology, University of Perugia, via A. Pascoli s/n, Perugia, Italy
² INFN Sezione di Perugia, via A. Pascoli s/n, Perugia, Italy
³ INAF Astronomical Observatory of Rome, Via Frascati 33, Monte Porzio Catone (Rome), Italy.
⁴ Goethe University Frankfurt, Max-von-Laue-Strasse 1, Frankfurt am Main D-60438, Germany
⁵ INAF, Osservatorio Astronomico d’Abruzzo, Via Mentore Maggini snc, I-64100 Collurania, Teramo, Italy
⁶ ENEA, Agenzia Nazionale per la nuove Tecnologie, l’Energia e lo Sviluppo Economico Sostenibile, Via Martiri di Monte Sole 4, Bologna, Italy
⁷ INFN Sezione di Bologna, Viale Berti Pichat 6/2, Bologna, Italy
⁸ Physics Division, School of Science and Technology, University of Camerino, Via Madonna delle Carceri 9B, Camerino, Macerata, Italy
⁹ European Centre for Theoretical Studies in Nuclear Physics and Related Areas, Str. delle Tabarelle, 286, Trento, Italy
¹⁰ Trento Institute for Fundamental Physics and Applications, Via Sommarive, 14, Trento, Italy

^* e-mail: sara.palmerini@pg.infn.it

Published online: 22 March 2023

Abstract

The isotopic abundances in presolar SiC grains of AGB origin provide important and precise constraints to those star nucleosynthesis models. By comparing the values of the s-element abundances resulting from calculations with the ones measured in these dust grains, it turns out that new measurements of weak-interaction rates in ionized plasmas, as well as of neutron-capture cross sections, are needed, especially in the region near the neutron magic numbers 50 and 82.