Nuclear theory and science of the facility for rare isotope beams

Balantekin, A. B.; Carlson, J.; Dean, D. J.; Fuller, George M.; Furnstahl, R. J.; Hjorth‐Jensen, M.; Janssens, R. V. F.; Li, Bao-An; Nazarewicz, W.; Nunes, F. M.; Ormand, W. E.; Reddy, Sanjay; Sherrill, B. M.

doi:10.1142/s0217732314300109

Cited by 69 publications

(61 citation statements)

References 55 publications

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“…Alternatively, charge equilibration has also been studied with deep inelastic collisions at lower energies, but with large isospin asymmetry in the entrance channel [14][15][16]. To reveal possible systematic trends requires both theoretical and experimental studies with a wide variety of projectile and target combinations which are expected to become available at current and future radioactive ion-beam (RIB) facilities [17]. In addition, much greater degree of isospin asymmetry available with RIBs will allow timescale and degree of isospin equilibration to be studied in detail.…”

Section: Introductionmentioning

confidence: 99%

Transport properties of isospin asymmetric nuclear matter using the time-dependent Hartree-Fock method

Umar

Simenel

2017

Phys. Rev. C

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Background: The study of deep-inelastic reactions of nuclei provide a vehicle to investigate nuclear transport phenomena for a full range of equilibration dynamics. These inquires provide us the ingredients to model such phenomena and help answer important questions about the nuclear Equation of State (EOS) and its evolution as a function of neutron-to-proton (N/Z) ratio.Purpose: The motivation is to examine the real-time dynamics of nuclear transport phenomena and its dependence on (N/Z) asymmetry from a microscopic point of view to avoid any pre-conceived assumptions about the involved processes.Method: Time-dependent Hartree-Fock (TDHF) method in full 3D is employed to calculate deep-inelastic reactions of 78 Kr+ 208 Pb and 92 Kr+ 208 Pb systems at 8.5 MeV/A. The impact parameter and energy-loss dependence of relevant observables are calculated. In addition, density constrained TDHF method is used to compute excitation energies of the primary fragments. The statistical deexcitation code GEMINI is utilized to examine the final reaction products.Results: The kinetic energy loss and sticking times as a function of impact parameter are calculated. Final properties of the fragments (charge, mass, scattering angle, kinetic energy) are computed. Their evolution as a function of energy loss is studied and various intra-relations are investigated. The fragment excitation energy sharing is computed. Conclusions:We find a smooth dependence of the energy loss, E loss , on the impact parameter for both systems. On the other hand the transfer properties for low E loss values are very different for the two systems but become similar in the higher E loss regime. The mean life time of the charge equilibration process, obtained from the final (N − Z)/A value of the fragments, is shown to be ∼ 0.5 zs. This value is slightly larger (but of the same order) than the value obtained from reactions at Fermi energies.

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Section: Introductionmentioning

confidence: 99%

Transport properties of isospin asymmetric nuclear matter using the time-dependent Hartree-Fock method

Umar

Simenel

2017

Phys. Rev. C

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“…New-generation radioactive ion beam facilities [22][23][24] will be able to reach a range of nuclei never possible before, including the neutron-rich frontier of the nuclear landscape. Theoretically, there have been major advances in both nuclear modelling and astrophysical simulations, greatly facilitated by high-performance computing [25][26][27][28][29][30][31][32][33][34]. When it comes to the nuclear input for the r-process, one relies on global predictions of nuclear properties [35][36][37][38].…”

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confidence: 99%

Impact of Nuclear Mass Uncertainties on therProcess

et al. 2016

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Nuclear masses play a fundamental role in understanding how the heaviest elements in the Universe are created in the r-process. We predict r-process nucleosynthesis yields using neutron capture and photodissociation rates that are based on nuclear density functional theory. Using six Skyrme energy density functionals based on different optimization protocols, we determine for the first time systematic uncertainty bands -related to mass modelling -for r-process abundances in realistic astrophysical scenarios. We find that features of the underlying microphysics make an imprint on abundances especially in the vicinity of neutron shell closures: abundance peaks and troughs are reflected in trends of neutron separation energy. Further advances in nuclear theory and experiments, when linked to observations, will help in the understanding of astrophysical conditions in extreme r-process sites. Introduction -Understanding the origin of elements in nature is one of the outstanding questions in science. Here, the synthesis of the heavy elements represents a difficult interdisciplinary challenge. Half of the heavy elements up to bismuth and all of the thorium and uranium in the Universe are produced by the rapid capture of neutrons in the r-process [1]. This process requires high neutron densities and involves extreme neutron-rich nuclei not yet produced in the laboratory.In recent years, much progress has been made toward this problem in both astrophysics and nuclear physics. In astrophysics, multidimensional hydrodynamic simulations including improved microphysics indicate that (i) neutrino-driven winds following core-collapse supernovae are not neutron-rich enough to produce heavy elements as suggested in [2] (see Ref.[3] for a review); (ii) a rare kind of core-collapse supernova triggered by magnetic fields leads to neutron-rich jets where the r-process can occur [4][5][6]; and (iii) neutron star mergers (as suggested in [7] and preliminarily studied in [8]) -are excellent candidates for the synthesis of heavy elements [9][10][11] even if their contribution to the early galaxy is still under discussion. Some studies show that neutron star mergers provide an important contribution to the solar system rprocess, but this is not enough to explain the abundances in the oldest observed stars, see e.g., [12][13][14]. In contrast, other models can explain the r-process abundances at all metallicities solely based on the neutron star merger scenario [15].Experimentally, there has been impressive progress in approaching r-process nuclei, see [16][17][18][19][20][21] and references quoted therein. New-generation radioactive ion beam facilities [22][23][24] will be able to reach a range of nuclei

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“…The experimental research in this frontier relies heavily on the range and intensity of radioactive ion beams (RIBs) available in the laboratory, which has provided the impetus for worldwide construction of RIB facilities dedicated to providing beams of short-lived nuclei for fundamental and applied research. A number of reviews summarize the recent progress in upgrading the capabilities of existing RIB facilities and constructing next-generation RIB facilities throughout the world [3][4][5][6].…”

Section: Introductionmentioning

confidence: 99%

Production of negatively charged radioactive ion beams

2017

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Beams of short-lived radioactive nuclei are needed for frontier experimental research in nuclear structure, reactions, and astrophysics. Negatively charged radioactive ion beams have unique advantages and allow for the use of a tandem accelerator for post-acceleration, which can provide the highest beam quality and continuously variable energies. Negative ion beams can be obtained with high intensity and some unique beam purification techniques based on differences in electronegativity and chemical reactivity can be used to provide beams with high purity. This article describes the production of negative radioactive ion beams at the former holifield radioactive ion beam facility at Oak Ridge National Laboratory and at the CERN ISOLDE facility with emphasis on the development of the negative ion sources employed at these two facilities.

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Nuclear theory and science of the facility for rare isotope beams

Cited by 69 publications

References 55 publications

Transport properties of isospin asymmetric nuclear matter using the time-dependent Hartree-Fock method

Transport properties of isospin asymmetric nuclear matter using the time-dependent Hartree-Fock method

Impact of Nuclear Mass Uncertainties on therProcess

Production of negatively charged radioactive ion beams

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