[en] The angular distribution of the ²H (⁶He,⁷Li)n reaction was measured with a secondary ⁶He beam of 36.4MeV for the first time. The proton spectroscopic factor of ⁷Li ground state was extracted to be 0.42±0.06 by normalizing the calculational differential cross-sections with the distorted-wave Born approximation to the experimental data. It was discussed that the uncertainty of extracted spectroscopic factors from the one-nucleon transfer reactions induced by deuteron might be reduced by determining the volume integrals of imaginary optical potentials precisely. (orig.)

[en] In order to investigate the possible influence of metallic environment on the alpha decay process, we have measured the ¹⁴⁷Sm activities in the hosts of metal samarium and Sm₂O₃. The ¹⁴⁷Sm half-life was found to be (1.06±0.01) x 10¹¹ y in metal samarium and (1.07±0.01) x 10¹¹ y in Sm₂O₃, respectively. No significant change has been observed within the experimental uncertainty. The absolute half-life presented here is consistent with the recommended value. (orig.)

[en] The ground state of the unstable ²⁶Al nucleus (²⁶Al_g) with t_1/2= 0.717 Myr was the first radioisotope detected in the galaxy, via the characteristic 1.809 MeV γ-emission of ²⁶Mg. The observation is direct proof of ongoing stellar nucleosynthesis in our Galaxy and indicates that there are approximately 2-3 M⊙ of ²⁶Al_g. It is therefore fundamental to understand the yields of ²⁶Al_g. ²⁶Al has an isomeric state (²⁶Al_m) which is prohibited to decay into ²⁶Al_g due to the large spin difference. However, an equilibration between ²⁶Al_m and ²⁶Al_g could proceed via intermediate states and influence the abundance of ²⁶Al_g. To clarify the production mechanism of ²⁶Al_g, we present our investigation of the sensitivity of the yields to variation of nuclear reaction rates involving ²⁶Al_g and ²⁶Al_m in single stars. (author)

[en] Angular distributions of ²H(⁶He,⁷Li)n and ¹²C(⁷Li,⁶He)¹³N reactions were measured at the HI-13 tandem accelerator, Beijing. Asymptotic normalization coefficient (ANC) of ¹³N →¹²C + p was derived to be 1.64±0.11 fm^-1/2 through distorted wave Born approximation (DWBA) analysis, which was then used to deduce the astrophysical S(E) factors for direct capture in ¹²C(p,γ)¹³N at energies of astrophysical relevance.

[en] Systematic studies of nuclear astrophysical reactions induced by lithium isotopes using the unstable ion beam facility GIRAFFE in CIAE were performed. We have measured the angular distributions of some single nucleon transfer reactions, such as ⁸Li(d,p)⁹Li, ⁸Li(d,n)⁹Be and ⁸Li(p,d)⁷Li in inverse kinematics, and derived the astrophysical S-factors or reaction rates for ⁸Li(n,γ)⁹Li and ⁸Li(p,γ)⁹Be by using asymptotic normalization coefficient (ANC) or spectroscopic factor.

[en] The elastic resonance scattering of ¹³N+p and ¹⁷F+p has been studied in inverse kinematics via a thick-target method. The excitation function for the ¹³N+p scattering was obtained in the energy interval of E_c.m.≅0.5-3.2MeV with a ¹³N secondary beam of (47.8±1.5)MeV. The resonance parameters for five low-lying levels in ¹⁴O were deduced by R-matrix fitting calculations. In the case of ¹⁷F+p scattering, preliminary result on the experimental excitation function is presented, in which the 4.52 MeV 3⁺ and 5.11 MeV 2⁺ states in ¹⁸Ne are clearly discernable.

[en] The ¹³C(⁷Li, ⁶He) ¹⁴ N_0,1 reactions were measured at E (⁷Li) = 34 MeV with the Q3D magnetic spectrometer of the HI-13 tandem accelerator, and the first peaks of the angular distributions were obtained for the first time. The ¹⁴N_0,1 proton spectroscopic factors were extracted to be 0.67±0.09 and 0.73±0.10, respectively. Using the ¹³C(p, γ) ¹⁴N direct capture S_dc(E) factors derived by the spectroscopic factors, the direct measurement data for both 1^- and 0^- resonances were well fitted via updating the resonance parameters, and then the total astrophysical ¹³C(p, γ) ¹⁴N S(E) factors and reaction rates were determined at stellar energies. The present work offers an independent examination to the existing results of the ¹³ C(p, γ) ¹⁴N reaction. (orig.)

[en] The stellar ¹⁴O (α, p) ¹⁷F reaction is thought to be one of the most important breakout reactions from the Hot CNO cycles into the rp-process in Type I X-ray bursters. In the present work, the properties of proton resonances in ¹⁸Ne have been investigated efficiently by utilizing a technique of proton resonant elastic scattering with a ¹⁷F radioactive-ion (RI) beam and a thick proton target. A 4.22 MeV/nucleon ¹⁷F RI beam, which was produced via a projectile-fragmentation reaction and experiencing a series of energy degradation, was separated by a Radioactive Ion Beam Line in Lanzhou (RIBLL) and bombarded a (CH₂)_n target. Energy spectra of the recoiled protons were measured by two sets of ΔE-E silicon telescope at center-of-mass scattering angles of θ _c.m. ∼ 175 ± 5 , θ _c.m. ∼ 152 ± 8 , respectively. Several proton resonances in ¹⁸Ne were observed, and their resonant parameters have been determined by an R-matrix analysis of the differential cross-sections. A doublet structure around 7.10 MeV has been identified and thought to be one state at 7.05 MeV (2⁺) and another one at 7.12 MeV (4⁺). The presently calculated total reaction rates of ¹⁴O (α, p) ¹⁷F are, at least, a factor of 1.2 ∝ 1.9 larger than the previous ones in a temperature region of 1.7 ∝ 3.0 GK mainly owing to the contribution from the 7.05 MeV (2⁺) state. This result implies that this breakout reaction may play a more important role than previously expected. (orig.)