Hydrogen burning of the oxygen isotopes takes place in low-mass stars, asymptotic giant branch stars, and classical novae. Observations of oxygen elemental and isotopic abundances in stellar spectra or in presolar grains provide strong constraints for stellar models if reliable thermonuclear reaction rates for hydrogen burning of oxygen are available. We present the results of a new measurement of the ${}^{17}\mathrm{O}{(p,\gamma )}^{18}\mathrm{F}$ reaction in the laboratory bombarding energy range of $170–530$ keV. The measurement is performed with significantly higher beam intensities ($I_{\max }$ $\approx$ 2 mA) compared to previous work and by employing a sophisticated $\gamma$-ray coincidence spectrometer. We measured the cross section at much lower energies than previous in-beam experiments. We also apply a novel data-analysis technique that is based on the decomposition of different contributions to the measured pulse-height spectrum. Our measured strengths of the low-energy resonances amount to $\omega {\gamma }_{\mathrm{pres}}\left(193\mathrm{keV}\right)=(1.86\pm 0.13)\times {10}^{-6}$ eV and $\omega {\gamma }_{\mathrm{pres}}\left(518\mathrm{keV}\right)=(13.70\pm 0.96)\times {10}^{-3}$ eV. For the direct capture $S$ factor at zero energy, we find a value of $S_{\mathrm{DC}}^{\mathrm{pres}}\left(0\right)$ = $4.82\pm 0.41$ keV b. We also present new thermonuclear rates for the ${}^{17}\mathrm{O}+p$ reactions, taking into account all consistent results from previous measurements.

• Received 30 October 2014
• Revised 5 January 2015

DOI:https://doi.org/10.1103/PhysRevC.91.015812