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The 13C(p, γ)14N radiative capture reaction is analyzed within the R-matrix approach with the aim to determine the astrophysical S factor. The low-energy astrophysical S factor has important contributions from both resonant and nonresonant captures. The contribution of the nonresonant component of the transition to a particular 14N bound state is expressed in terms of the asymptotic normalization coefficient (ANC). The experimental ANCs induced from the 13C(14N, 13C)14N and 13C(3He, d)14N reactions are used in the analysis. The fits of the calculated S factors to the experimental data are sensitive to the ANC values and are used to test the extracted ANCs. It is found that the ANCs determined from the transfer reactions provide the best fit for transitions to all the states in 14N, except for the third excited state. The obtained astrophysical factor, S(0)=7.6±1.1 keV b, is in excellent agreement with published values. [Copyright &y& Elsevier]

We discuss the use of one-nucleon breakup reactions of loosely bound nuclei at intermediate energies as an indirect method in nuclear astrophysics. In particular, the breakup of 8B and 9C is described in detail in terms of an extended Glauber model. Existing experimental data for the breakup of 8B at energies from 30 to 1000 MeV/u and of 9C at 285 MeV/u on light through heavy targets are analyzed. The predictions of the model are in excellent agreement with independent reaction data (reaction cross sections and parallel momentum distributions for core-like fragments). Final state interaction has been included in the Coulomb dissociation component. Glauber model calculations using different effective interactions give consistent, though slightly different results. The results of this new analysis are compared with the earlier one for the astrophysical factor S17(0) for the key reaction for solar neutrino production 7Be(p,γ)8B. They are consistent with the values from most direct measurements and other indirect methods. [Copyright &y& Elsevier]