Na22(n,p)22Ne andNa22(n,α)19F cross sections from 25 meV to 35 keV

The ${}_{}{}^{22}{}_{}{}^{}\mathrm{Na}$(n,$p_0$), (n,$p_1$), (n,${\alpha }_0$), (n,${\alpha }_1$), and (n,${\alpha }_2$) cross sections have been measured at thermal neutron energy. In addition, the $p_0$ and $p_1$ cross sections have been measured from thermal energy to 420 eV and 35 keV, respectively. These new data were used to discern the structure of ${}_{}{}^{23}{}_{}{}^{}\mathrm{Na}$ near the neutron threshold. In particular, it was found that a (${\mathrm{}(7/2)\mathrm{}}^{+}$ resonance dominates the $p_1$ cross section but contributes very little to the $p_0$ cross section. The $p_0$, and also most probably the (n,${\alpha }_0$) cross sections, are instead dominated by a separate (${\mathrm{}(5/2)\mathrm{}}^{+}$ resonance. The ${}_{}{}^{22}{}_{}{}^{}\mathrm{Na}$(n,p${)}^{22}$Ne astrophysical reaction rate, $N_A$〈σv〉, was calculated using our new data and compared to published theoretical rates used in previous nucleosynthesis calculations. It was found that the theoretical rates are approximately a factor of 5 to 10 different from the experimental one at most temperatures measured. We discuss the possible implications of this difference on nucleosynthesis calculations for ${}_{}{}^{22}{}_{}{}^{}\mathrm{Na}$ and ${}_{}{}^{22}{}_{}{}^{}\mathrm{Ne}$.