| 摘 要： | 13N（p, γ）14O is is one of the key reactions in the hot CNO cycle which occurs at stellar temperatures around T9≤0.1. At the energies of astrophysical interest, the 13N（p, γ）14O reaction is dominated by the low energy tail of the s-wave capture on the broad 1- resonance at Er = 527.9 keV （which has a total width of （37.34-0.9） keV）. A considerable effort has been expended in recent years to determine the parameters for the resonance. These include the direct measurements using the radioactive ^13N beam, particle transfer reactions, and coulomb dissociation of high-energy ^14O beams in the field of a heavy nucleus.
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