Astrophysical S(E) for the Be-9(p, d)Be-8 and Be-9(p, alpha)Li-6 Reactions by Direct Measurement

The p-Be-9 reactions play a key role in accurate prediction of the primordial abundance of beryllium, and its abundance can be used to exquisitely probe the nucleosynthesis and mixing mechanism of stars. In the present work, astrophysical S(E) factors of the Be-9(p, d)Be-8 and Be-9(p, alpha)Li-6 reactions have been obtained from the thick-target yield Yield(E-i) for proton energies from 18 to 100 keV. A full R-matrix analysis was performed to fit both the Be-9(p, alpha)Li-6 and Be-9(p, d)Be-8 reactions simultaneously. The resulting astrophysical S(E) factors agree well with direct measurements, leading to S(0) = 17.3 2.1 and 13.9 1.8 MeVb for the Be-9(p, alpha)Li-6 and Be-9(p, d)Be-8 reactions, respectively. However, the obtained screening potential (U-s = 512 77 eV) is lower than results of previous work (900 50 and 806 eV), and all of them are larger than the adiabatic limit of 264 eV. The reaction rates were also calculated in the temperature range (0.01-1) 10(9) K, which improves on the precision of the standard database NACRE and NACRE II.