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• W1920742086 abstract "The $R$-matrix approach has proved to be very useful in extrapolating the astrophysical factor down to astrophysically relevant energies, since the majority of measurements are not available in this region. However, such an approach has to be critically considered when no complete knowledge of the reaction model is available. To get reliable results in such cases one has to use all the available information from independent sources and, accordingly, fix or constrain variations of the parameters. In this paper we present a thorough $R$-matrix analysis of the ${}^{15}mathrm{N}(p,ensuremath{gamma}){}^{16}mathrm{O}$ reaction, which provides a path from the CN cycle to the CNO bi-cycle and CNO tri-cycle. The measured astrophysical factor for this reaction is dominated by resonant capture through two strong ${J}^{ensuremath{pi}}={1}^{ensuremath{-}}$ resonances at ${E}_{R}=312$ and $962$ keV and direct capture to the ground state. Recently, a new measurement of the astrophysical factor for the ${}^{15}mathrm{N}(p,ensuremath{gamma}){}^{16}mathrm{O}$ reaction has been published [P. J. LeBlanc et al., Phys. Rev. C 82, 055804 (2010)]. The analysis has been done using the $R$-matrix approach with unconstrained variation of all parameters including the asymptotic normalization coefficient (ANC). The best fit has been obtained for the square of the ANC ${C}^{2}=539.2$ fm${}^{ensuremath{-}1}$, which exceeds the previously measured value by a factor of $ensuremath{approx}3$. Here we present a new $R$-matrix analysis of the Notre Dame--LUNA data with the fixed within the experimental uncertainties square of the ANC ${C}^{2}=200.34$ fm${}^{ensuremath{-}1}$. Rather than varying the ANC we add the contribution from a background resonance that effectively takes into account contributions from higher levels. Altogether we present ten fits, seven unconstrained and three constrained. For the unconstrained fit with the boundary condition ${B}_{c}={S}_{c}({E}_{2})$, where ${E}_{2}$ is the energy of the second level, we get $S(0)=39.0ifmmodepmelsetextpmfi{}1.1$ keVb and normalized ${mathrm{ensuremath{chi}ifmmode tilde{}else ~{}fi{}}}^{2}=1.84$, i.e., the result which is similar to LeBlanc et al. From all our fits we get the range $33.1ensuremath{leqslant}S(0)ensuremath{leqslant}40.1$ keVb which overlaps with the result of LeBlanc et al. We address also the physical interpretation of the fitting parameters." @default.
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• W1920742086 date "2011-04-11" @default.
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• W1920742086 title "Astrophysical<mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline><mml:mrow><mml:mi>S</mml:mi></mml:mrow></mml:math>factor for the<mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline><mml:mmultiscripts><mml:mi mathvariant=normal>N</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>15</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>(<mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline><mml:mrow><mml:mi>p</mml:mi></mml:mrow…" @default.
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• W1920742086 doi "https://doi.org/10.1103/physrevc.83.044604" @default.
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