AstrophysicalSfactor of theHe3(α,γ)Be7reaction measured at low energy via detection of prompt and delayed γ rays

Solar neutrino fluxes depend both on astrophysical and on nuclear physics inputs, namely on the cross sections of the reactions responsible for neutrino production inside the Solar core. While the flux of solar ${}^8\mathrm{B}$ neutrinos has been recently measured at Superkamiokande with a 3.5% uncertainty and a precise measurement of ${}^7\mathrm{Be}$ neutrino flux is foreseen in the next future, the predicted fluxes are still affected by larger errors. The largest nuclear physics uncertainty to determine the fluxes of ${}^8\mathrm{B}$ and ${}^7\mathrm{Be}$ neutrinos comes from the ${}^3\mathrm{He}$($\alpha ,\gamma$)${}^7\mathrm{Be}$ reaction. The uncertainty on its S-factor is due to an average discrepancy in results obtained using two different experimental approaches: the detection of the delayed γ rays from ${}^7\mathrm{Be}$ decay and the measurement of the prompt γ emission. Here we report on a new high precision experiment performed with both techniques at the same time. Thanks to the low background conditions of the Gran Sasso LUNA accelerator facility, the cross section has been measured at $E_{\mathrm{c}.\mathrm{m}.}=170$, 106, and 93 keV, the latter being the lowest interaction energy ever reached. The S-factors from the two methods do not show any discrepancy within the experimental errors. An extrapolated $S(0)=0.560\pm 0.017$ keV barn is obtained. Moreover, branching ratios between the two prompt γ-transitions have been measured with 5–8% accuracy.