Pairing and the structure of the pf-shell N ~ Z nuclei

The influence of the isoscalar and isovector L=0 pairing components of the effective nucleon-nucleon interaction is evaluated for several isobaric chains, in the framework of full pf shell model calculations. We show that the combined effect of both isospin channels of the pairing force is responsible for the appearance of T=1 ground states in N=Z odd-odd nuclei. However, no evidence is found relating them to the Wigner energy. We study the dependence of their contributions to the total energy on the rotational frecuency in the deformed nucleus 48Cr. Both decrease with increasing angular momentum and go to zero at the band termination. Below the backbending their net effect is a reduction of the moment of inertia, more than half of which comes from the proton-neutron channel.Comment: 5 pages, RevTeX, 5 figure

Shell Model Calculation of the β- and β+ Partial Half-Lives of 54Mn and Other Unique Second Forbidden β Decays

The nucleus 54Mn, observed in cosmic rays, decays there dominantly by the β- branch with an unknown rate. The branching ratio of its β+ decay was determined recently. We use the shell model with only a minimal truncation and calculate both β+ and β- decay rates. Good agreement for the β+ branch suggests that the calculated partial half-life of the β- decay, 4.94×10^5 yr, should be reliable. However, this half-life is noticeably shorter than the range 1–2×10^6 yr indicated by the fit based on the 54Mn abundance in cosmic rays. We also evaluate other known unique second forbidden β decays from the p and sd shells and show that the shell model can describe them with reasonable accuracy as well

Dynamical r-process studies within the neutrino-driven wind scenario and its sensitivity to the nuclear physics input

We use results from long-time core-collapse supernovae simulations to investigate the impact of the late time evolution of the ejecta and of the nuclear physics input on the calculated r-process abundances. Based on the latest hydrodynamical simulations, heavy r-process elements cannot be synthesized in the neutrino-driven winds that follow the supernova explosion. However, by artificially increasing the wind entropy, elements up to A=195 can be made. In this way one can reproduce the typical behavior of high-entropy ejecta where the r-process is expected to occur. We identify which nuclear physics input is more important depending on the dynamical evolution of the ejecta. When the evolution proceeds at high temperatures (hot r-process), an (n,g)-(g,n) equilibrium is reached. While at low temperature (cold r-process) there is a competition between neutron captures and beta decays. In the first phase of the r-process, while enough neutrons are available, the most relevant nuclear physics input are the nuclear masses for the hot r-process and the neutron capture and beta-decay rates for the cold r-process. At the end of this phase, the abundances follow a steady beta flow for the hot r-process and a steady flow of neutron captures and beta decays for the cold r-process. After neutrons are almost exhausted, matter decays to stability and our results show that in both cases neutron captures are key for determining the final abundances, the position of the r-process peaks, and the formation of the rare-earth peak. In all the cases studied, we find that the freeze out occurs in a timescale of several seconds.Comment: 20 pages, 12 figures, submitted to Phys. Rev. C (improved version