“…Thus, knowledge of S 17 , the 7 Be(p, γ) 8 B S-factor at solar energies (center-of-mass energy E ≈ 20 keV), is crucial to conclusions drawn from present (Homestake, Kamiokande) and future (SNO, Superkamiokande) solar neutrino experiments [1,2]. Despite extensive experimental efforts, the 7 Be(p, γ) 8 B cross section is still the most uncertain nuclear input to the standard solar model [1,3], due to a significant spread among the values of S 17 deduced from the various experiments (direct capture [4]: S 17 = 18 − 28 eV·b and Coulomb break-up [5]: S 17 = 16.7 ± 3.5 eV·b). Theoretical estimates also vary (S 17 = 16 − 30 eV·b) [6], making these predictions rather unreliable.…”