19F(p,γ)20Ne
PI: Jakub Skowronski, Axel Boeltzing
Astrophysical Motivation
The 19F(p,γ)20Ne reaction plays a key role in the nucleosynthesis of fluorine in stellar environments, particularly in asymptotic giant branch (AGB) stars and novae.
Accurate cross-section data at astrophysically relevant energies are essential to understand the depletion of fluorine and the operation of the CNO cycles in stellar interiors.
Recent measurements at JUNA have provided new insights, but additional data at lower energies are necessary to reduce uncertainties in stellar models.
Experimental Aim
The LUNA measurement aims to extend the cross-section data of the 19F(p,γ)20Ne reaction to even lower energies within the Gamow window relevant for hydrogen burning in stars.
The goal is to improve constraints on the reaction rate and to test theoretical models, particularly those involving direct capture and low-energy resonances suggested by recent experiments.
Experimental Setup
The experiment is being conducted at the LUNA 400 kV accelerator located deep underground in the Gran Sasso Laboratory, benefiting from extremely low background conditions.
A high-efficiency BGO detector is used to capture the full γ-ray cascade following the 19F(p,γ)20Ne reaction.
Proton beams are delivered onto a fluorine-rich target under ultra-high vacuum, allowing precise determination of cross sections at energies approaching the stellar Gamow window.