Welcome and Introduction

• Konrad Schmidt (Helmholtz-Zentrum Dresden-Rossendorf, Germany)

Room: online

Structure and equilibrium of normal stars

• Maurizio Busso (University of Perugia, Italy)

Room: online

Moderated questions

• Sara Palmerini (INFN Perugia & University of Perugia, Italy)

Room: online

How to make elements in my computer

• Marco Pignatari (Konkoly Observatory, Hungary)

Room: online

Moderated questions

• Rosario Gianluca Pizzone (Laboratori Nazionali del Sud, Italy)

Room: online

Nuclear Physics in Astrophysics X (NPAX) conference and school

• Alberto Mengoni (ENEA Bologna and INFN, Sezione di Bologna, Italy)

Room: online Invitation to Nuclear Physics in Astrophysics X (NPAX) conference (Sep 5 to 9, 2022) and school (Aug 29 to Sep 2, 2022)

3D hydrodynamics simulations of massive stars with the PROMPI code

• Federico Rizzuti (Keele University, United Kingdom)

Room: online The evolution of massive stars is deeply affected by uncertainties related to multi-dimensional processes that take place in stellar interiors (e.g. convection, rotation, magnetic activity). However, it is not computationally possible to simulate the entire lifetime of a star while also following its fluid motions explicitly. For this reason, 3D hydrodynamics simulations are used to support 1D stellar evolution codes by reproducing on a short timescale (minutes or hours) realistic 3D processes. In this talk, I will present the multi-dimensional hydrodynamics code PROMPI and results coming from a new set of high-resolution simulations of the neon-burning shell in a massive star, focusing on the interplay between nuclear burning and convection, as well as discussing the impacts of different resolutions and nuclear rate boosting on the results. This work was done in collaboration with Cyril Georgy, Raphael Hirschi, and David Arnett.

Moderated questions

• Andreas Korn (Uppsala University, Sweden)

Room: online

Direct measurement of the 19F(p,α)16O reaction

• Teodora Andreea Madgearu (Extreme Light Infrastructure, Romania)

Room: online The 19F(p,α)16O reaction is important for understanding the fluorine abundance in the outer layers of asymptotic giant branch (AGB) stars and it might also play a role in hydrogen-deficient post-AGB star nucleosynthesis. Up to now, theoretical models overproduce F abundances in AGB stars with respect to the observed values, thus calling for further investigation of the reactions involving fluorine. Indeed, in the last years, new direct and indirect measurements improved significantly the knowledge of the 19F(p,α0)16O cross section at deeply sub-Coulomb energies (below 0.8 MeV). Nevertheless, those data are larger by a factor of about 1.4 with respect to the previous data reported in the NACRE compilation in the energy region 0.6-0.8 MeV. In order to solve these discrepancies, we present here a direct experiment performed at INFN-LNS using a silicon strip detector array (LHASA - Large High-resolution Array of Silicon for Astrophysics). Our results clearly confirm the trend of the latest experimental data in the energy region of interest. The 19F(p,α)16O reaction rate is the sum over the (p,α0), (p,απ) and the (p,αγ) channels. While the (p,α0) rate is well constrained by the present existing data, down to the lowest energies, almost nothing is known from experiments on the (p,απ) and (p,αγ) rates. Despite its importance, the S-factors and the branching ratio between the α0, απ and αγ outgoing channels in the 19F(p,α)16O reaction are still largely uncertain at astrophysical energies, emphasizing the need for better measurements. Thus, a direct measurement using the new detector, ELISSA (Extreme Light Infrastructure – Silicon Strip Array), coupled with LHASA will be performed in September 2022 at IFIN-HH. This setup is allowing us to discriminate the (p,απ) and (p,αγ) reaction rates at very low energies.

Moderated questions

• Andreas Korn (Uppsala University, Sweden)

Room: online

Round table discussion Room: online Questions that were compiled in the chat during and after lectures and the breakout session will be answered and discussed.