The ${}^9\mathrm{Be}(p,\gamma {)}^{10}\mathrm{B}$ reaction plays an important role in primordial and stellar nucleosynthesis of light elements in the p shell, but the energy dependence of $S\left(E\right)\mathrm{}$ has not been well understood. We reanalyze the existing ${}^9\mathrm{Be}(p,\gamma {)}^{10}\mathrm{B}$ experimental data within the framework of the R-matrix method. The direct capture part of the S factor is calculated using the experimentally measured asymptotic normalization coefficients for ${}^{10}{\overrightarrow{\mathrm{B}}}^9\mathrm{Be}+p.\mathrm{}$ The fitted parameters of the low-lying ${}^{10}\mathrm{B}$ resonances are also required to be consistent with previous measurements of ${}^6\mathrm{Li}(\alpha ,\gamma {)}^{10}\mathrm{B}.$ 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 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.

• Received 8 April 1999

DOI:https://doi.org/10.1103/PhysRevC.60.035801