Astrophysical<i>S</i>factor<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi mathvariant="normal">for</mml:mi><mml:mrow><mml:msup><mml:mrow><mml:mi> </mml:mi></mml:mrow><mml:mrow><mml:mn>13</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mi mathvariant="normal">C</mml:mi><mml:mo>(</mml:mo><mml:mi>p</mml:mi><mml:mo>,</mml:mo><mml:mi>γ</mml:mi><mml:mrow><mml:msup><mml:mrow><mml:mo>)</mml:mo></mml:mrow><mml:mrow><mml:mn>14</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mi mathvariant="normal">N</mml:mi></mml:math>and asymptotic normalization coefficients

We reanalyze the ${}^{13}\mathrm{C}(p,\ensuremath{\gamma}{)}^{14}\mathrm{N}$ radiative capture reaction within the R-matrix approach. The low-energy astrophysical S factor has important contributions from both resonant and onresonant captures. The normalization of the nonresonant component of the transition to a particular ${}^{14}\mathrm{N}$ bound state is expressed in terms of the asymptotic normalization coefficient (ANC). In the analysis we use the experimental ANC's inferred from $\mathrm{the}{}^{13}\mathrm{C}{(}^{14}\mathrm{N}{,}^{13}\mathrm{C}{)}^{14}\mathrm{N}$ and ${}^{13}\mathrm{C}{(}^{3}\mathrm{He}{,d)}^{14}\mathrm{N}$ reactions. The fits of the calculated S factors to the experimental data are sensitive to the ANC values and are used to test the extracted ANC's. We find that for transitions to all the states $\mathrm{in}{}^{14}\mathrm{N},$ except the third excited state, the ANC's determined from the transfer reactions provide the best fit. The astrophysical factor we obtain, $S(0)=7.7\ifmmode\pm\else\textpm\fi{}1.1 \mathrm{keV}\mathrm{}\mathrm{b},$ is in excellent agreement with previous results.

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