Astrophysical factor for the CNO cycle radiative capture reaction$^{15}\mbox{N}(p,\gamma )^{16}\mbox{O}$

The reaction ${ }^{15}\mbox{N}(p,\gamma ){ }^{16}\mbox{O}$ leaks from CN cycle and determines the oxygen isotopes generated in CNO tri-cycle. Direct measurements of the astrophysical S(E) factor for this reaction were reported [1]. The analysis [1] assumes that the reaction is dominated by resonances at $E_{cm} =312\,\,\mbox{and}\,\,964\,\,$keV, and direct capture to the ground state of ${ }^{16}\mbox{O}.$ The ANCs for bound states of ${ }^{16}\mbox{O}$ have been measured in reaction ${ }^{15}\mbox{N}({ }^3He,d){ }^{16}\mbox{O}$ [2]. Using these ANCs, the astrophysical factor for ${ }^{15}\mbox{N}(p,\gamma ){ }^{16}\mbox{O}$ has been calculated by the R-matrix approach. The proton and $\alpha $ widths of two resonances were determined from the fit to the direct data for ${ }^{15}\mbox{N}(p,\alpha ){ }^{12}\mbox{C}$ [3] and used to calculate the S(E) factor for${ }^{15}\mbox{N}(p,\gamma ){ }^{16}\mbox{O}$. Radiative were varied within experimental uncertainty to fit to the direct data for ${ }^{15}\mbox{N}(p,\gamma ){ }^{16}\mbox{O}$. The calculated S(E) factor is $S(0)=38\,$keVb if we fit the S(E) factor at the resonance peaks; this is significantly smaller than the value $S(0)=64\pm 6$ keVb reported in [1]. Hence, one reaction ${ }^{15}\mbox{N}(p,\gamma ){ }^{16}\mbox{O}$ occurs for almost 1500 CN cycles, rather than 880 cycles as estimated in [1]. The problem with fitting the data from [1] at resonance peaks and small energies necessitates re-measurement at lower energies of this reaction. [1] Rolfs, C., and Rodney, W.S., \textit{Nucl. Phys. }A235 (1974) 450. [2] A. M. Mukhamedzhanov, P. Bem, V. Burjan et al., Phys. Rev. C (will be submitted). [3] A. Redder et al., Z. Phys. A305, 325 (1982).