The reaction of a pulsed 18 O beam on a 164 Dy target was studied in the first experiment with the NuBall array at the IPN Orsay, France. Excited state half-lives were measured using the fast timing method with 20 LaBr 3 (Ce) detectors. The timing characteristics of the fully digital acquisition system is briefly discussed. A value for the previously unknown half-life of the first excited 4 + state in 178 W is presented.
We report on the measurement of lifetimes of excited states in the near-mid-shell nuclei 164,166 Dy using the gamma-ray coincidence fast-timing method. The nuclei of interest were populated using reactions between an 18 O beam and a gold-backed isotopically enriched 164 Dy target of thickness 6.3 mg/cm 2 at primary beam energies of 71, 76, and 80 MeV from the IPN-Orsay laboratory, France. Excited states were populated in 164 Dy, 166 Dy, and 178,179 W following Coulomb excitation, inelastic nuclear scattering, two-neutron transfer, and fusionevaporation reaction channels respectively. Gamma rays from excited states were measured using the ν-Ball high-purity germanium (HPGe)-LaBr 3 hybrid γ-ray spectrometer with the excited state lifetimes extracted using the fast-timing coincidence method using HPGe-gated LaBr 3-LaBr 3 triple coincident events. The lifetime of the first I π = 2 + excited state in 166 Dy was used to determine the transition quadrupole deformation of this neutron-rich nucleus for the first time. The experimental methodology was validated by showing consistency with previously determined excited state lifetimes in 164 Dy. The half-lives of the yrast 2 + states in 164 Dy and 166 Dy were 2.35(6) and 2.3(2) ns, respectively, corresponding to transition quadrupole moment values of Q 0 = 7.58(9) and 7.5(4) eb, respectively. The lifetime of the yrast 2 + state in 166 Dy is consistent with a quenching of nuclear quadrupole deformation at β ≈ 0.35 as the N = 104 mid-shell is approached.
We have performed the first direct measurement of the 83 Rbðp; γÞ radiative capture reaction cross section in inverse kinematics using a radioactive beam of 83 Rb at incident energies of 2.4 and 2.7A MeV. The measured cross section at an effective relative kinetic energy of E cm ¼ 2.393 MeV, which lies within the relevant energy window for core collapse supernovae, is smaller than the prediction of statistical model calculations. This leads to the abundance of 84 Sr produced in the astrophysical p process being higher than previously calculated. Moreover, the discrepancy of the present data with theoretical predictions indicates that further experimental investigation of p-process reactions involving unstable projectiles is clearly warranted.
The discovery of presolar grains in primitive meteorites has initiated a new era of research in the study of stellar nucleosynthesis. However, the accurate classification of presolar grains as being of specific stellar origins is particularly challenging. Recently, it has been suggested that sulfur isotopic abundances may hold the key to definitively identifying presolar grains with being of nova origins and, in this regard, the astrophysical 33 Clðp; γÞ 34 Ar reaction is expected to play a decisive role. As such, we have performed a detailed γ-ray spectroscopy study of 34 Ar. Excitation energies have been measured with high precision and spin-parity assignments for resonant states, located above the proton threshold in 34 Ar, have been made for the first time. Uncertainties in the 33 Clðp; γÞ reaction have been dramatically reduced and the results indicate that a newly identified l ¼ 0 resonance at E r ¼ 396.9ð13Þ keV dominates the entire rate for T ¼ 0.25-0.40 GK. Furthermore, nova hydrodynamic simulations based on the present work indicate an ejected 32 S= 33 S abundance ratio distinctive from type-II supernovae and potentially compatible with recent measurements of a presolar grain.
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