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A precise determination of proton capture rates on oxygen is mandatory to predict the abundance ratios of the oxygen isotopes in a stellar environment where hydrogen burning is active. The  17 O(p, γ ) 18 F reaction, specically, plays a crucial role in AGB nucleosynthesis as well as in explosive hydrogen burning occurring in type Ia novae. At temperatures of interest for the former scenario (20 MK ≤ T ≤ 80 MK) the main contribution to the astrophysical reaction rate comes from the  E  c.m.  = 65 keV resonance. The strength of this resonance is presently determined only through indirect measurements, with an adopted value of  ωγ  = (1.6 ± 0.3) × 10 −11  eV. Thanks to the low background environment of the Laboratori Nazionali del Gran Sasso, the intense and stable beam provided by the LUNA 400 kV accelerator and the experience in oxygen target production, the LUNA collaboration is aiming the rst direct measurement of the above mentioned resonance strength. In the present work details of challenging direct measurement planned at LUNA will be described.

The challenging direct measurement of the 65 keV resonance strength of the 17O(p,γ)18F reaction at LUNA

The challenging direct measurement of the 65 keV resonance strength of the ¹⁷O(p,γ)¹⁸F reaction at LUNA