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The reaction $^{17}$O$(p,\gamma)^{18}$F influences hydrogen-burningnucleosynthesis in several stellar sites, such as red giants, asymptotic giantbranch (AGB) stars, massive stars and classical novae. In the relevanttemperature range for these environments ($T_{9}=0.01-0.4), the maincontributions to the rate of this reaction are the direct capture process, twolow lying narrow resonances ($E_{r}=65.1$ and 183 keV) and the low-energy tailsof two broad resonances ($E_{r}=557$ and 677 keV). Previous measurements andcalculations give contradictory results for the direct capture contributionwhich in turn increases the uncertainty of the reaction rate. In addition, veryfew published cross section data exist for the high energy region that mightaffect the interpretation of the direct capture and the contributions of thebroad resonances in the lower energy range. This work aims to address theseissues. The reaction cross section was measured in a wide proton energy range($E_{c.m.}=345$ - 1700 keV) and at several angles($\theta_{lab}=0^{\circ},45^{\circ},90^{\circ},135^{\circ}$). The observedprimary $\gamma$-transitions were used as input in an $R$-matrix code in orderto obtain the contribution of the direct capture and the two broad resonancesto the low-energy region. The extrapolated S-factor from the present data is ingood agreement with the existing literature data in the low-energy region. Anew reaction rate was calculated from the combined results of this work andliterature S-factor determinations. Resonance strengths and branchings arereported for several $^{18}$F states. We were able to extrapolate theastrophysical S-factor of the reaction $^{17}$O$(p,\gamma)^{18}$F at lowenergies from cross section data taken at higher energies. No significantchanges in the nucleosynthesis are expected from the newly calculated reactionrate.

Proton Capture on ^{17}O and its astrophysical implications