The 16 O( 3 He,d) 17 F reaction has been used to determine asymptotic normalization coefficients for transitions to the ground and first excited states of 17 F. The coefficients provide the normalization for the tails of the overlap functions for 17 F→ 16 Oϩp and allow us to calculate the S factors for 16 O(p,␥) 17 F at astrophysical energies. The calculated S factors are compared to measurements and found to be in very good agreement. This provides a test of this indirect method to determine astrophysical direct capture rates using transfer reactions. In addition, our results yield S(0) for capture to the ground and first excited states in 17 F, without the uncertainty associated with extrapolation from higher energies. ͓S0556-2813͑99͒00702-5͔ PACS number͑s͒: 25.40. Lw, 25.55.Hp, 26.20.ϩf, 27.20.ϩn

The 15 N(p, γ ) 16 O reaction 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 16 O reaction. The results indicate that the direct capture contribution was previously overestimated. We find the astrophysical factor to be S(0) = 36.0 ± 6.0 keV b, which is about a factor of 2 lower than the presently accepted value. We conclude that for every 2200 ± 300 cycles of the main CN cycle one CN catalyst is lost due to this reaction.

The mass of ~~ has been measured with two different reactions: 9Be(a3C, 12N)1~ ELab=336 MeV, and13C(14C, 17F)l~ ELa b = 337 MeV. The mass excess of 33.445(50) MeV is deduced from the Q-value measurement. l~ is found to be particle-unstable with respect to one-neutron emission by 0.42(5) MeV. In the analysis of the first reaction a low lying excited state is found at 0.38 (8) MeV. This state and the ground state can be most probably identified as the 1 +/2+-doublet coupled from the [Tr 1 p 3/2 | v 1 p 1/2] configuration, the 1 +-state being the ground state. The (13C, 12N)-reaction populates the 1 +-state strongly due to a spin-isospin-flip character of the dominant part of the transition amplitude. The 2+member corresponds to the mass given by Wilcox et al. A second excited state is observed at 4.05(10)MeV with a width of 0.7(2) MeV, it can be associated with the v 1 d 5/2-strength. The second reaction is fully supporting the interpretation of the ground state doublet. The excited state at 4.05 MeV is not observed in this reaction and indeed it should not, because the reaction does not populate in first order excited neutron configurations. The levels are well described by mean field calculations including pairing correlations. The lowest resonance in the calculations is the v 1/2--configuration, whereas the v 1/2+-configuration shows at the neutron threshold a strong nonresonant contribution.

The14 C(n, γ) 15 C reaction plays an important role in inhomogeneous big bang models. In [N. K. Timofeyuk et al., Phys. Rev. Lett. 96, 162501 (2006)] it was shown that the 14 C(n, γ) 15 C radiative capture at astrophysically relevant energies is peripheral reaction, i.e. the overall normalization of its cross section is determined by the asymptotic normalization coefficient (ANC) for 15 C → 14 C+n. Here we present new measurements of the 14 C(d, p) 15 C differential cross sections at deuteron incident energy of 17.06 MeV and the analysis to determine the ANCs for neutron removal from the ground and first excited states of 15 C. The results are compared with the previous estimations.