Nuclear reaction rates for the s-process

Session

Perspectives

23 Feb 2024, 09:30

Sala B (Centro Congressi Partenope)

27. Nuclear Astrophysics at LUNA

Dr Axel Boeltzig (LNGS)

23/02/2024, 09:30

28. Nuclear Astrophysics at JUNA

Dr Bingshui Goa

23/02/2024, 10:00

The 13C(a,n)16O reaction is the main neutron source for the s-process in AGB stars. Meanwhile, this reaction is also believed to be the neutron source for the i-process although its astrophysical site is still unclear. Direct measurement of its cross section at astrophysical energies is challenging in above-ground laboratories due to the vast cosmic-ray induced background. Underground...

29. Nuclear Astrophysics at CASPAR

Prof. Michael Wiescher (University of Notre Dame)

23/02/2024, 10:30

This talk will provide a short overview of the development of the CASPAR laboratory and its scientific program over the last decade. Because of the installation of the DUNE detector, CASPAR is presently not accessible. The talk will report on the present status of CASPAR and the scientific priorities after the laboratory reopens in summer 2024.

30. 22Ne(α,n)25Mg with SHADES

Chemseddine Ananna (Università degli Studi di Napoli "Federico II")

23/02/2024, 11:30

The talk is a summary of the characterisation work done for the understanding, calibration and then commissioning of the EJ-309 organic liquid scintillators used by the ERC funded SHADES project lead by prof. Best. A new nuclear astrophysics experiment aiming to perform, for the first time, a direct cross section measurements for the 22Ne(α,n)25Mg reaction at very low energy. The SHADES...

31. 22Ne(α,γ)26Mg with EASγ

Daniela Mercogliano (Istituto Nazionale di Fisica Nucleare)

23/02/2024, 11:45

The reaction 22Ne(α,γ)26Mg is associated with several questions in nuclear astrophysics like the Mg isotope ratio in stellar atmospheres and its competition with the neutron source 22Ne(α,n)25Mg.
Due to very low stellar energies and therefore very low cross section, direct experiments have been only able to provide upper limits below a strong resonance at 832 keV.
The purpose of the EASγ...

32. Remeasuring the gamma-decay branching ratio of the Hoyle state at The Oslo Cyclotron Laboratory

Wanja Paulsen

10. Talk 10

11. Talk 11

12. Talk 12

13. Talk 13

8. Talk 8

9. Talk 9