Astrophysical [ital S] factor for [sup 9]Be(p,[gamma])[sup 10]B

The [sup 9]Be(p,[gamma])[sup 10]B reaction plays an important role in primordial and stellar nucleosynthesis of light elements in the [ital p] shell, but the energy dependence of S(E) has not been well understood. We reanalyze the existing [sup 9]Be(p,[gamma])[sup 10]B experimental data within the framework of the [ital R]-matrix method. The direct capture part of the [ital S] factor is calculated using the experimentally measured asymptotic normalization coefficients for [sup 10]B[r arrow][sup 9]Be+p. The fitted parameters of the low-lying [sup 10]B resonances are also required to be consistent with previous measurements of [sup 6]Li([alpha],[gamma])[sup 10]B. A good simultaneous fit to both radiative capture reactions is found, in contrast to previous analyses. These results demonstrate that experimentally measured asymptotic normalization coefficients, coupled to the [ital R]-matrix method, can provide a reasonable determination of direct radiative capture rates, even when the captured proton is tightly bound in the final nucleus. [copyright] [ital 1999] [ital The American Physical Society]