Determination of the astrophysicalSfactor for11C(p,γ)12Nfrom the<

Elastic scattering of the proton drip-line nucleusF17

“…However, we found that the imaginary part does not need any renormalization (N W ≈ 1.0), which seems a rather general situation for p-shell nuclei [1][2][3]6]. Moreover, the standard range parameters t v = 1.20 fm and t w = 1.75 fm [6] give the best description of the present data.…”

“…[22]), and they have better angular resolution and a larger angular range than previous elastic-scattering data obtained with RNBs (see, e.g. [1][2][3]23]). …”

“…Reaction studies with radioactive nuclear beams (RNBs) are now expanding our understanding of nuclear structure to loosely bound nuclei away from stability. For example, several recent proton-transfer experiments were performed with RNBs at energies around 10 MeV/nucleon, at which reactions are peripheral, with the intention of extracting stellar reaction rates [1][2][3].…”

Scattering ofBe7andB8and the astrophysicalTăbăcaru1, Azhari2, Brinkley3 et al. 2006Phys. Rev. CSelf Cite4810402View full textAdd to dashboardCite

“…We previously reported measurements of the asymptotic normalization coefficients (ANCs) for 8 B that we made by using the proton transfer reactions 10 B( 7 Be, 8 B) 9 Be [9] and 14 N( 7 Be, 8 B) 13 C [10]. We determined the ANCs, which fix the amplitude of the tail of the overlap integral of the ground-state wave function of 8 B onto the two-body channel 7 Be + p, by comparing a distorted-wave Born approximation (DWBA) calculation with the angular distribution for the transfer reaction.…”

Structure ofN12usingC11+Perajärvi1, Fu2, Rogachev3 et al. 2006Phys. Rev. CSelf Cite

“…In addition to the nuclear physics interest, studies involving 12 N around its 11 C+p threshold at 0.601 MeV are often also driven by nuclear astrophysics interests [4][5][6][7][8]. Namely, to be able to accurately determine the astrophysical rate of the 11 C(p, γ ) 12 N reaction, detailed knowledge of the low-lying level structure of 12 N is also required.…”