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In this work the measurement of the differential cross sections (DCS) of the proton transfer reaction ${}^{12}$C(${}^{10}$B,${}^{9}$Be${}_{g.s.}$)${}^{13}$N${}_{g.s.}$. has been carried out (Fig. 1) for the ANC ${}^{13}$N${}_{g.s.}$→${}^{12}$C+p obtaining. The experiment was fulfilled at 10B ions beam of the C-200P cyclotron of the Heavy Ion Laboratory (University of Warsaw) at the energy $E_{10B}$=41.3 MeV. At this energy the proton transferring process is practically peripheral what is suggested by behavior of the testing function $R(b)$ of the MDWBA method 1 in which the single DCS calculated using the LOLA computer code [2]. So the DCS of the reaction is expressed via the product of the ANCs squares ${(C_{10B→9Be+p})}^{2}$×${(C_{13N→12C+p})}^{2}$. The ANC ${(C_{13N→12C+p})}^{2}$ = 2.6±0.3 fm${}^{-1}$ was preliminary evaluated from the analysis (the solid curve in Fig.1), as the ANC ${(C_{10B→9Be+p})}^{2}$ is rather well known from [3,4]. The channel coupling was found to be negligible by evaluation with the FRESCO code. More correct value will be found by analysis of the data in the frameworks of the developed asymptotic reaction theory [5] along with a careful selection of parameters of the optical potentials.
The derived ANC for ${}^{12}$C+p→${}^{13}$N will be applied for calculation of the nuclear-astrophysical ${}^{12}$C(p,$\gamma$)${}^{13}$N reaction rates at stellar temperatures.
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