# Cross section measurement of the astrophysically important 17O(p,gamma)18F reaction in a wide energy range

## TL;DR

This study measures the 17O(p,g)18F reaction cross section across a wide energy range using activation, providing high-precision data crucial for astrophysical models and improving the understanding of stellar hydrogen burning processes.

## Contribution

The paper presents the first wide-range, high-precision cross section measurements of the 17O(p,g)18F reaction using activation, reducing uncertainties in astrophysical reaction rates.

## Key findings

- Cross section measured between 500 keV and 1.8 MeV with 10% uncertainty.
- Results generally agree with previous data, with some deviations.
- R-matrix analysis supports reliable extrapolation of the zero-energy S-factor.

## Abstract

The 17O(p,g)18F reaction plays an important role in hydrogen burning processes in different stages of stellar evolution. The rate of this reaction must therefore be known with high accuracy in order to provide the necessary input for astrophysical models. The cross section of 17O(p,g)18F is characterized by a complicated resonance structure at low energies. Experimental data, however, is scarce in a wide energy range which increases the uncertainty of the low energy extrapolations. The purpose of the present work is therefore to provide consistent and precise cross section values in a wide energy range. The cross section is measured using the activation method which provides directly the total cross section. With this technique some typical systematic uncertainties encountered in in-beam gamma-spectroscopy experiments can be avoided. The cross section was measured between 500 keV and 1.8 MeV proton energies with a total uncertainty of typically 10%. The results are compared with earlier measurements and it is found that the gross features of the 17O(p,g)18F excitation function is relatively well reproduced by the present data. Deviation of roughly a factor of 1.5 is found in the case of the total cross section when compared with the only one high energy dataset. At the lowest measured energy our result is in agreement with two recent datasets within one standard deviation and deviates by roughly two standard deviations from a third one. An R-matrix analysis of the present and previous data strengthen the reliability of the extrapolated zero energy astrophysical S-factor. Using an independent experimental technique, the literature cross section data of 17O(p,g)18F is confirmed in the energy region of the resonances while lower direct capture cross section is recommended at higher energies. The present dataset provides a constraint for the theoretical cross sections.