The CNO cycle is one of the most important nuclear energy sources in stars. At temperatures of hydrostatic H-burning (20 MK < T < 80 MK) the 17O(p; γ)18F reaction rate is dominated by the poorly constrained 64.5 keV resonance. Here, we report on the first direct measurements of its resonance strength and of the direct capture contribution at 142 keV, performed with a new high sensitivity setup at LUNA. The present resonance strength of ωγbare = (30 +/- 6stat +/- 2syst) peV is about a factor of 2 higher than the values in literature, leading to a Γbare = (34 +/- 7stat +/- 3syst) neV, in agreement with the LUNA result from the (p,α) channel. Such agreement strengthens our understanding of the oxygen isotopic ratios measured in red giant stars and in O-rich presolar grains.
First Direct Measurement of the 64.5 keV Resonance Strength in the 17O(p,γ)18F Reaction
F. Casaburo;P. Corvisiero;P. Prati;S. Zavatarelli
2024-01-01
Abstract
The CNO cycle is one of the most important nuclear energy sources in stars. At temperatures of hydrostatic H-burning (20 MK < T < 80 MK) the 17O(p; γ)18F reaction rate is dominated by the poorly constrained 64.5 keV resonance. Here, we report on the first direct measurements of its resonance strength and of the direct capture contribution at 142 keV, performed with a new high sensitivity setup at LUNA. The present resonance strength of ωγbare = (30 +/- 6stat +/- 2syst) peV is about a factor of 2 higher than the values in literature, leading to a Γbare = (34 +/- 7stat +/- 3syst) neV, in agreement with the LUNA result from the (p,α) channel. Such agreement strengthens our understanding of the oxygen isotopic ratios measured in red giant stars and in O-rich presolar grains.
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