Astrophysical relevance of the low-energy dipole strength of 206Pb
Abstract not provided
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
Engineering topics
Goriely, S
Publications and source records attributed to Goriely, S.
Determination of radiative neutron capture cross sections for unstable nuclei by the {gamma}-ray strength function method
An indirect method referred to as the {gamma}-ray strength function method has been devised to determine radiative neutron capture cross sections for unstable nuclei along the valley of {beta}-stability. This method is based on the {gamma}-ray strength function which interconnects radiative neutron capture and photoneutron emission within the statistical model. The method was applied to several unstable nuclei such as {sup 93,95}Zr, {sup 107}Pd, and 121,123Sn. This method offers a versatile application extended to unstable nuclei far from the stability when combined with Coulomb dissociation experiments at RIKEN-RIBF and GSI.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
Physical conditions for the r-process
Recent works show that the r-process can proceed by competition between neutron capture and {beta}-decay in low temperature environments (< 5 Multiplication-Sign 10{sup 8} K; cold r-process) where photo-disintegration plays no role. This is in contrast to the traditional picture of the r-process in high temperature environments ({approx} 1 Multiplication-Sign 10{sup 9} K; hot r-process) where the (n, {gamma})-({gamma}, n) equilibrium holds. In this study, we explore nucleosynthesis calculations based on a site-independent model to elucidate the physical conditions leading to cold and hot r-processes.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
The r-process nucleosynthesis: Nuclear physics challenges
About half of the nuclei heavier than iron observed in nature are produced by the socalled rapid neutron capture process, or r-process, of nucleosynthesis. The identification of the astrophysics site and the specific conditions in which the r-process takes place remains, however, one of the still-unsolved mysteries of modern astrophysics. Another underlying difficulty associated with our understanding of the r-process concerns the uncertainties in the predictions of nuclear properties for the few thousands exotic neutron-rich nuclei involved and for which essentially no experimental data exist. The present contribution emphasizes some important future challenges faced by nuclear physics in this problem, particularly in the determination of the nuclear structure properties of exotic neutron-rich nuclei as well as their radiative neutron capture rates and their fission probabilities. These quantities are particularly relevant to determine the composition of the matter resulting from the r-process. Their impact on the r-abundance distribution resulting from the decompression of neutron star matter is discussed.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
The r-process nucleosynthesis during the decompression of neutronised matter
The rapid neutron-capture process, or r-process, is known to be of fundamental importance for explaining the origin of approximately half of the A>60 stable nuclei observed in nature. In recent years nuclear astrophysicists have developed more and more sophisticated r-process models, eagerly trying to add new astrophysical or nuclear physics ingredients to explain the solar system composition in a satisfactory way.We show here that the decompression of the neutron star matter may provide suitable conditions for a robust r-processing. After decompression, the inner crust material gives rise to an abundance distribution for A>130 nuclei similar to the one observed in the solar system. Similarly, the outer crust if heated at a temperature of about 8 10{sup 9} K before decompression is made of exotic neutron-rich nuclei with a mass distribution close to the 80{<=}A{<=}130 solar one. During the decompression, the free neutrons (initially liberated by the high temperatures) are re-captured leading to a final pattern similar to the solar system distribution.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
Nuclear ingredients for cross section calculation of exotic nuclei
The increasing need for cross sections far from the valley of stability, especially for applications such as nuclear astrophysics, poses a challenge for nuclear reaction models. So far, predictions of cross sections have relied on more or less phenomenological approaches, depending on parameters adjusted to available experimental data or deduced from systematic relations. While such predictions are expected to be reliable for nuclei not too far from the experimentally known regions, it is clearly preferable to use more fundamental approaches, based on sound physical bases, when dealing with very exotic nuclei. Thanks to the high computer power available today, all major ingredients required to model a nuclear reaction can now be (and have been) microscopically (or semi-microscopically) determined starting from the information provided by a nucleon-nucleon effective interaction. We have implemented all these microscopic ingredients in the latest version of the TALYS nuclear reaction code, and we are now able to perform fully microscopic cross section calculations.We will discuss both the quality of these ingredients and the impact of using them instead of the usually adopted phenomenological parameters. We will also discuss the foreseen evolutions of the models and of the ingredients on which they rely.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
Gamma-ray strength functions and their relation to astrophysics
The nuclear {gamma}-ray strength function is one of the indispensable inputs needed for reaction-rate calculations, and is particularly important for the neutron-capture cross section. The nuclear physics group at the Oslo Cyclotron Laboratory has developed a method to extract simultaneously nuclear level density and {gamma}-ray strength function from particle-{gamma} coincidence measurements. Data on the strength functions of Sn nuclei as well as for lighter elements are presented. The Sn isotopes all display a resonance-like structure close to the neutron threshold, that could possibly be due to the neutron-skin oscillation mode. This so-called pygmy dipole resonance greatly influences the neutron-capture rates. In the lighter nuclei, an enhancement of the strength function at low {gamma} energies is observed. The possible impact of this increase on Maxwellian-averaged reaction rates has been investigated.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
THE {gamma}SF METHOD
The {gamma}-ray strength function ({gamma}SF) interconnects radiative neutron capture and photoneutron emission as a common ingredient in the statistical model. Outlined here is an indirect method of determining radiative neutron-capture cross sections for unstable nuclei based on the {gamma}-ray strength function. Application examples of the {gamma}SF method are demonstrated.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
Improved Relativistic QRPA calculations of the {gamma}-ray strength
Continuum Random Phase Approximation (CRPA) for relativistic point coupling models with density dependent coupling constants is applied to investigate collective excitations in spherical nuclei. In particular we study the impact of the exact continuum on the Giant Dipole Resonance of several Tin isotopes as well as the nuclear ({gamma},n) reaction rates which are important in astrophysical calculations.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
Gogny HFB prediction of nuclear structure properties
Large scale mean field calculations from proton to neutron drip lines have been performed using the Hartree-Fock-Bogoliubov method based on the Gogny nucleon-nucleon effective interaction. This extensive study has shown the ability of the method to reproduce bulk nuclear structure data available experimentally. This includes nuclear masses, radii, matter densities, deformations, moment of inertia as well as collective mode (low energy and giant resonances). In particular, the first mass table based on a Gogny-Hartree-Fock-Bogolyubov calculation including an explicit and coherent account of all the quadrupole correlation energies is presented. The rms deviation with respect to essentially all the available mass data is 798 keV. Nearly 8000 nuclei have been studied under the axial symmetry hypothesis and going beyond the mean-field approach.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
Latest development of the combinatorial model of nuclear level densities
The combinatorial model of nuclear level densities has now reached a level of accuracy comparable to that of the best global analytical expressions. We have recently improved the treatment using simultaneously the single particle levels and collective properties predicted by the newly derived D1M Gogny interaction. In addition for deformed nuclei, the transition to sphericity is coherently taken into account on the basis of a temperature-dependent Hartree-Fock calculation which provides at each temperature the structure properties needed to build the level densities. This new method is described and shown to give good results with respect to available experimental data.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
Striking behavior of photoneutron cross sections for {sup 90}Zr near threshold
Photoneutron cross sections for {sup 90}Zr near neutron threshold were examined with a photon difference technique using laser Compton scattering {gamma}-ray beams. The cross section decreasing in the vicinity of neutron threshold exhibited a steep rise within 150 keV above the threshold. We draw attention to a possible relation of this striking behavior to the 3P valence neutron resonance known in neutron capture in the mass region A{approx_equal}90.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
Application of the {gamma}SF method to palladium
Photoneutron cross sections were measured for {sup 108}Pd, {sup 106}Pd, and {sup 105}Pd with laser-Compton scattering {gamma}-ray beams in an application of the {gamma}SF method to a radioactive nucleus {sup 107}Pd. We present radiative neutron cross sections for {sup 107}Pd[6.5x10{sup 6} y] obtained with the {gamma}SF method.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗