PI: Andreas Best


Astrophysical Motivation

The reaction 18O(p,γ)19F has a possible influence on the 18O depletion in AGB stars. The strength of a low-energy resonance around 90 keV has been under discussion in the literature and a direct experimental determination was required.


Experimental Aims

Aim of the experiment is the measurement of the so far unknown strength of the 90 keV resonance as well as a better determination of the strength and decay branchings of four more resonances below 400 keV.


Experimental Setup

HPGe Detector Setup for the 18O(p,g) Experiment

This reaction is being measured at the solid target station of LUNA 400. The lowest energy data are taken with a high-efficiency 4 pi BGO summing crystal, higher-energy cross section and resonance branchings are measured with a HPGe detector. Both setups are lead shielded.

Targets are anodised tantalum backings using highly enriched O-18 water.

BGO Detector Setup for 18O(p,g) and an 18O-enriched target



Cross section of the reaction 18O(p,γ)19F at astrophysical energies: The 90 keV resonance and the direct capture component

Physics Letters B 797 (2019) 134900