The rate of the final step in the astrophysical $\alpha$p-process, the $^{ 34}$Ar($\alpha$,\textit{ p})$^{ 37}$K reaction, suffers from large uncertainties due to lack of experimental data, despite having a considerable impact on the observable light curves of x-ray bursts and the composition of the ashes of hydrogen and helium burning on accreting neutron stars. We present the first direct measurement constraining the $^{ 34}$Ar($\alpha$,p)$^{ 37}$K reaction cross section, using the Jet Experiments in Nuclear Structure and Astrophysics (JENSA) gas jet target. The combined cross section for the $^{ 34}$Ar,Cl($\alpha$,p)$^{ 37}$K,Ar reaction is found to agree well with Hauser-Feshbach predictions. The $^{ 34}$Ar($\alpha$,2p)$^{ 36}$Ar cross section, which can be exclusively attributed to the $^{ 34}$Ar beam component, also agrees to within the typical uncertainties quoted for statistical models. This indicates the applicability of the statistical model for predicting astrophysical ($\alpha$,p) reaction rates in this part of the $\alpha$p process, in contrast to earlier findings from indirect reaction studies indicating orders-of-magnitude discrepancies. This removes a significant uncertainty in models of hydrogen and helium burning on accreting neutron stars.
Categories: nucl-ex