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The $^{17}$O(p,$\alpha$)$^{14}$N reaction plays a key role in variousastrophysical scenarios, from asymptotic giant branch stars to classical novae.It affects the synthesis of rare isotopes such as $^{17}$O and $^{18}$F, whichcan provide constraints on astrophysical models. A new direct determination ofthe $E_{\rm R}~=~64.5$~keV resonance strength performed at the Laboratory forUnderground Nuclear Astrophysics accelerator has led to the most accurate valueto date, $\omega\gamma = 10.0 \pm 1.4_{\rm stat} \pm 0.7_{\rm syst}$~neV,thanks to a significant background reduction underground and generally improvedexperimental conditions. The (bare) proton partial width of the correspondingstate at $E_{\rm x} = 5672$~keV in $^{18}$F is $\Gamma_{\rm p} = 35 \pm 5_{\rmstat} \pm 3_{\rm syst}$~neV. This width is about a factor of 2 higher thanpreviously estimated thus leading to a factor of 2 increase in the$^{17}$O(p,$\alpha$)$^{14}$N reaction rate at astrophysical temperaturesrelevant to shell hydrogen-burning in red giant and asymptotic giant branchstars. The new rate implies lower $^{17}$O/$^{16}$O ratios, with importantimplications on the interpretation of astrophysical observables from thesestars.

Improved Direct Measurement of the 64.5 keV Resonance Strength in the 17O(p,a)14N Reaction at LUNA