Search

The Dual Fluid Reactor, DFR, is a novel concept of a fast heterogeneous nuclear reactor. Its key feature is the employment of two separate liquid cycles, one for fuel and one for the coolant. As opposed to other liquid-fuel concepts like the Molten-Salt Fast Reactor (MSFR), both cycles in the DFR can be separately optimized for their respective purpose, leading to advantageous consequences: A very high power density resulting in remarkable cost savings, and a highly negative temperature feedback coefficient, enabling a self-regulation without any control rods or mechanical parts in the core. In the current reference design the fuel liquid is an undiluted actinide trichloride based on isotope-purified Cl-37, circulating at an operating temperature of 1000 °C. It can be processed on-line in a small internal processing unit utilizing fractional distillation or electro refining. Medical radioisotopes like Mo-99/Tc-99m are by-products and can be provided right away. In a more advanced design, an actinide metal alloy melt with an appropriately low solidus temperature is also possible which enables a reduction of the core size and allows a further increase in the operating temperature due to its high heat conductivity. For the reference design, pure Lead as coolant is the best choice. It yields a very hard neutron spectrum, fostering a very good neutron economy and therefore making the DFR a preferred thorium breeder but also a very effective waste incinerator and transmuter. With its high coolant temperature the DFR achieves the same ambitions as the Generation IV concept of the very high temperature reactor (VHTR), with all its advantages like electricity production with high efficiency and the synthesis of carbon-free fuels, but with overall production costs competitive with today’s refined oil. The specific combination of the liquids in the very high temperature regime requires structural materials withstanding corrosive attacks. Because of the small size of the reactor core the utilization of these expensive materials would have no significant impact on the overall energy (and also economic) efficiency, measured by the EROI (Energy Return on Investment), which is more than 20 times higher than for a light-water reactor (LWR). The DFR inherits the positive properties of the lead-cooled reactor (LFR) and of the MSFR, especially its outstanding passive safety features.

The enhanced electron screening effect in nuclear reactions taking place in dense astrophysical plasmas is extremely important for determination of stellar reaction rates in terrestrial laboratories as well as in prediction of cross sections enhancement in interiors of stars such as White and Brown Dwarfs or Giant Planets. This effect resulting in reduction of the nuclear Coulomb potential by the atomic electrons has been confirmed in many laboratory experiments. Unfortunately, experimental screening energies are much higher than the theoretical predictions and the reason for that remains unknown. Here, we present absorbing results of the experiment studying d + d nuclear reactions in different deuterized metallic targets under ultra high vacuum conditions. The total cross sections and angular distributions of the 2H(d,p)3H and 2H(d,n)3He reactions have been measured using a deuteron beam of energies between 8 and 30 keV provided by the electron cyclotron ion source. The atomic cleanness of the target surface has been secured by combining Ar sputtering of the target and Auger electrons spectroscopy. Due to application of an on-line analysis method, the homogeneity of the implanted deuteron densities could be continuously monitored. We will discuss probable causes of the large discrepancy between theoretical and experimental data.

The energy returned on invested, EROI, has been evaluated for typical power plants representing wind energy, photovoltaics, solar thermal, hydro, natural gas, biogas, coal and nuclear power. The strict exergy concept with no “primary energy weighting”, updated material databases, and updated technical procedures make it possible to directly compare the overall efficiency of those power plants on a uniform mathematical and physical basis. Pump storage systems, needed for solar and wind energy, have been included in the EROI so that the efficiency can be compared with an “unbuffered” scenario. The results show that nuclear, hydro, coal, and natural gas power systems (in this order) are one order of magnitude more effective than photovoltaics and wind power.

Angular distributions and the neutron-proton branching ratio of the mirror reactions 2H(d, p)3H and 2H(d, n)3He have been investigated using different self-implanted deuterized metallic targets at projectile energies between 5 and 60 keV. Whereas the experimental results obtained for the transition metals Zr, Pd, Ta and also Al do not differ from those known from gas-target experiments, an enhancement of the angular anisotropy in the neutron channel and an attenuation of the neutron-proton branching ratio have been observed for the (earth)alkaline metals Li, Sr and Na at deuteron energies below 20 keV. Experimental results are discussed with consideration of the special problems arising from the properties of these chemically very reactive target materials. A first theoretical effort explaining simultaneously both n/p asymmetry effects based on an induced polarization of the reacting deuterons within the crystal lattice is presented.

The study of the 2H(d, p)3H reaction at very low energies in deuterized metallic targets provides a unique possibility to test models of the electron screening developed for dense astrophysical plasmas. Here, we compare the experimental screening energies obtained by our group as well as by other authors for different target materials with theoretical predictions based on an improved dielectric function theory. The calculations are performed within the self-consistent regime and include polarization of both quasifree and bound electrons. Additionally, the cohesion screening, arising from different binding energies of deuterons and α-particles in crystal lattices, is taken into account. The proposed theory predicts only a weak material dependence of the screening energy in agreement with our experimental results but fails in the absolute strength of the effect by a factor of 2. The projectile-velocity dependence of the screening energy corresponding to the transition from the weak-screening regime to the strong-screening limit is discussed.

The reaction threshold for deuteron induced reactions on 10 B amounts to 25.2 MeV, which enables an excitation of the giant resonances (GR) in the compound nucleus 12 C even at very low projectile energies. In our recent experimental and theoretical investigations of the 10 B(d,p) 11 B reaction, we have found a strong reaction contribution arising from the giant dipole resonance (GDR) excitation. This kind of transition is only possible due to a significant isospin impurity of the GDR in 12 C. In the present work, we study an influence of the GDR as well as of the giant quadrupole (GQR) excitation on the 10 B(d,p) 11 B reaction cross section for transitions to the ground as well as the first three excited states at astrophysically relevant deuteron energies below 3 MeV. Based on our new measurement of angular distributions and absolute cross sections as well as on experimental results of other authors we have determined the total astrophysical S-factor of the 10 B(d,p) 11 B reaction down to deuteron energies close to zero. Additionally, the importance of the interference between resonant and direct reaction amplitudes is discussed.

Based on our experimental studies of the electron screening effect in the 2H(d,p)3H reaction for five deuteron-implanted solid targets (C,Al,Zr,Pd,Ta), theoretical calculations have been performed within an improved dielectric function theory. The theory describes correctly the observed target material dependence of the screening energies, underestimating, however, the absolute values by about a factor of 2. Applying an effective screening energy approach, the theoretical cross-sections, thick-target yields as well as nuclear reaction rates have been calculated down to the energies corresponding to the conditions of so-called cold-fusion experiments. This allows for a comparison of the experimental results at higher energies with those achieved in the heavy-water electrolysis experiments.

To study the electron screening of nuclear reactions in metallic environments, angular distributions and thick target yields of the fusion reactions 2H(d,p)3H and 2H(d,n)3He have been measured on deuterons implanted in three different metal targets (Al, Zr and Ta) for beam energies ranging from 5 to 60 keV. The experimentally determined values of the screening energy are about one order of magnitude larger than the value achieved in a gas target experiment and significantly larger than the theoretical predictions. A clear target material dependence of the screening energy has been established.

By means of recoil nuclei spectroscopy the 6 Li(d,p 0 ) 7 Li and 6 Li(d,n 0 ) 7 Be mirror reactions have been measured for deuteron energies between 65 and 135 keV. The results have been compared with theoretical calculations including effects of the isospin mixed subthreshold resonance state in 8 Be.

The total cross section of the ${}^{6}$Li$(d,\ensuremath{\alpha}{)}^{4}$He reaction has been measured for deuteron energies between 50 and 180 keV. From a detailed distorted-wave Born approximation analysis of the angular distributions and the excitation function up to 1 MeV it was possible to determine the strength of a subthreshold resonance that dominates the cross section at sub-Coulomb energies and contributes significantly to the increase of the astrophysical $S$ factor at low energies. Consequently the electron screening energy we have determined for the ${}^{6}$Li(d,$\ensuremath{\alpha}{)}^{4}$He reaction is considerably smaller than the value given in previous works which overestimate the theoretical predictions. In addition the stellar reaction rate has been calculated up to a temperature of ${T}_{9}$=3.

The reaction cross-section has been measured for deuteron energies below 25 keV in a deuterized Zr target under improved ultra-high-vacuum conditions and controlled target surface contamination. The increase of reaction enhancement factors towards lower energies is much weaker than that determined before and can result not only from the electron screening effect but also from a suggested 0+ threshold resonance in 4He. The cross-section calculations performed within the T-matrix approximation enable to estimate a coherent resonance contribution and explain the observed energy dependence of the enhancement factors. Additionally, indications for the increase of the screening energies due to impurities at the target surface could be found.

We have performed a heavy ion radiative capture reaction between two light heavy ions, $^{12}$C and $^{16}$O, leading to $^{28}$Si. The present experiment has been performed below Coulomb barrier energies in order to reduce the phase space and to try to shed light on structural effects. Obtained $\gamma$-spectra display a previously unobserved strong feeding of intermediate states around 11 MeV at these energies. This new decay branch is not fully reproduced by statistical nor semi-statistical decay scenarii and may imply structural effects. Radiative capture cross-sections are extracted from the data., Comment: 4 pages, 7 figures, to appear as proceedings of FUSION 2011 conference at St-Malo, France

The {beta}-delayed {alpha} decay of {sup 16}N has been used to restrict the E1 fraction of the ground state {gamma} transition in the astrophysically important {sup 12}C({alpha},{gamma}){sup 16}O reaction in several experiments. A review of the published measurements is given, and GEANT4 simulations and R-matrix calculations are presented to further clarify the observed {alpha} spectra. A clear response function, in the form of a low-energy tail from the scattering of {alpha} particles in the catcher foil, is observed in these simulations for any foil thickness. Contrary to claims in the literature, the simulations show that the TRIUMF measurement and those performed at Yale and Mainz originate from the same underlying spectrum. The simulations suggest that the discrepancies between the Yale and TRIUMF final results can be attributed to incorrect deconvolution methods applied in the former case. The simulations show in general that the form (width) of the spectrum is very sensitive to the catcher foil thickness. It is concluded that the TRIUMF measurement most likely represents the currently closest approximation to the true {beta}-delayed {alpha}-decay spectrum of {sup 16}N.

The deuteron-emission channel in the beta decay of the halo nucleus (11)Li was measured at the Isotope Separator and Accelerator facility at TRIUMF by implanting postaccelerated (11)Li ions into a segmented silicon detector. The events of interest were identified by correlating the decays of (11)Li with those of the daughter nuclei. This method allowed the energy spectrum of the emitted deuterons to be extracted, free from contributions from other channels, and a precise value for the branching ratio B(d)=1.30(13)x10(-4) to be deduced for E(c.m.)>200 keV. The results provide the first unambiguous experimental evidence that the decay takes place essentially in the halo of (11)Li and that it proceeds mainly to the (9)Li+d continuum, opening up a new means to study the halo wave function of (11)Li.

Recent measurements of the reaction d(d,p)t in metallic environments at very low energies performed by different experimental groups point to an enhanced electron screening effect. However, the resulting screening energies differ strongly for divers host metals and different experiments. Here, we present new experimental results and investigations of interfering processes in the irradiated targets. These measurements inside metals set special challenges and pitfalls which make them and the data analysis particularly error-prone. There are multi-parameter collateral effects which are crucial for the correct interpretation of the observed experimental yields. They mainly originate from target surface contaminations due to residual gases in the vacuum as well as from inhomogeneities and instabilities in the deuteron density distribution in the targets. In order to address these problems an improved differential analysis method beyond the standard procedures has been implemented. Profound scrutiny of the other experiments demonstrates that the observed unusual changes in the reaction yields are mainly due to deuteron density dynamics simulating the alleged screening energy values. The experimental results are compared with different theoretical models of the electron screening in metals. The Debye-H\"{u}ckel model that has been previously proposed to explain the influence of the electron screening on both nuclear reactions and radioactive decays could be clearly excluded., Comment: 22 pages, 12 figures, REVTeX4, 2-column format. Submitted to Phys. Rev. C; accepted

The p({sup 11}Li,{sup 9}Li)t reaction has been studied for the first time at an incident energy of 3A MeV at the new ISAC-2 facility at TRIUMF. An active target detector MAYA, built at GANIL, was used for the measurement. The differential cross sections have been determined for transitions to the {sup 9}Li ground and first excited states in a wide range of scattering angles. Multistep transfer calculations using different {sup 11}Li model wave functions show that wave functions with strong correlations between the halo neutrons are the most successful in reproducing the observation.

The p((11)Li, (9)Li)t reaction has been studied for the first time at an incident energy of 3A MeV at the new ISAC-2 facility at TRIUMF. An active target detector MAYA, built at GANIL, was used for the measurement. The differential cross sections have been determined for transitions to the (9)Li ground and first excited states in a wide range of scattering angles. Multistep transfer calculations using different (11)Li model wave functions show that wave functions with strong correlations between the halo neutrons are the most successful in reproducing the observation.

The heavy-ion radiative capture reaction, {sup 12}C({sup 12}C,{gamma}), has been investigated at energies both on- and off-resonance, with a particular focus on known resonances at E{sub c.m.}=6.0, 6.8, 7.5, and 8.0 MeV. Gamma rays detected in a BGO scintillator array were recorded in coincidence with {sup 24}Mg residues at the focal plane of the DRAGON recoil separator at TRIUMF. In this manner, the relative strength of all decay pathways through excited states up to the particle threshold could be examined for the first time. Isovector M1 transitions are found to be a important component of the radiative capture from the E{sub c.m.}=6.0 and 6.8 MeV resonances. Comparison with Monte Carlo simulations suggests that these resonances may have either J=0 or 2, with a preference for J=2. The higher energy resonances at E{sub c.m.}=7.5 and 8.0 MeV have a rather different decay pattern. The former is a clear candidate for a J=4 resonance, whereas the latter has a dominant J=4 character superposed on a J=2 resonant component underneath. The relationship between these resonances and the well-known quasimolecular resonances as well as resonances in breakup and electrofission of {sup 24}Mg into two {sup 12}C nuclei are discussed.

The short-lived nuclide {sup 44}Ti is an important nuclide for the understanding of explosive nucleosynthesis. The main production reaction, {sup 40}Ca({alpha},{gamma}){sup 44}Ti, has been studied in inverse kinematics with the recoil mass spectrometer DRAGON located at the TRIUMF-ISAC facility in Vancouver, Canada. The temperature range relevant for {alpha}-rich freeze-out during a core-collapse supernova has been covered entirely with a {sup 40}Ca beam of 0.60 to 1.15 MeV/nucleon. All relevant quantities for the calculation of the astrophysical reaction rate have been measured directly. Because of many previously undiscovered resonances, the reaction rate derived from the energy dependent {sup 44}Ti yield is higher than the one based on previous prompt {gamma}-ray studies commonly used in supernova models. The presented new rate results in an increased {sup 44}Ti production in supernovae.

We measured the β‐decay of the halo‐nucleus 11Li, with particular attention to the deuteron‐ and triton‐emission channels. We employed a post‐accelerated beam of 11Li ions, and the implantation technique in a finely‐segmented silicon detector. The channels of interest were identified through the time and space correlations between the implantation events and the parent and daughter decays. We obtained the branching ratios, as well as the spectra of the emitted ions.

Radiative {alpha}-particle capture into the first excited, J{sup {pi}}=0{sup +} state of {sup 16}O at 6.049 MeV excitation energy has rarely been discussed as contributing to the {sup 12}C({alpha},{gamma}){sup 16}O reaction cross section due to experimental difficulties in observing this transition. We report here measurements of this radiative capture in {sup 12}C({alpha},{gamma}){sup 16}O for center-of-mass energies of E=2.22 MeV to 5.42 MeV at the DRAGON recoil separator. To determine cross sections, the acceptance of the recoil separator has been simulated in GEANT as well as measured directly. The transition strength between resonances has been identified in R-matrix fits as resulting both from E2 contributions as well as E1 radiative capture. Details of the extrapolation of the total cross section to low energies are then discussed [S{sub 6.0}(300)=25{sub -15}{sup +16} keV b] showing that this transition is likely the most important cascade contribution for {sup 12}C({alpha},{gamma}){sup 16}O.

The strength of the Ec.m.=184 keV resonance in the 26gAl(p,gamma)27Si reaction has been measured in inverse kinematics using the DRAGON recoil separator at TRIUMF's ISAC facility. We measure a value of omegagamma=35±7 µeV and a resonance energy of Ec.m.=184±1 keV, consistent with p-wave proton capture into the 7652(3) keV state in 27Si, and discuss the implications of these values for 26gAl nucleosynthesis in typical oxygen-neon white-dwarf novae.

Radiative alpha-particle capture into the first excited, J(pi)=0+ state of 16O at 6.049 MeV excitation energy has rarely been discussed as contributing to the 12C(alpha,gamma)16O reaction cross section due to experimental difficulties in observing this transition. We report here measurements of this radiative capture in 12C(alpha,gamma)16O for center-of-mass energies of E=2.22 MeV to 5.42 MeV at the DRAGON recoil separator. To determine cross sections, the acceptance of the recoil separator has been simulated in GEANT as well as measured directly. The transition strength between resonances has been identified in R-matrix fits as resulting both from E2 contributions as well as E1 radiative capture. Details of the extrapolation of the total cross section to low energies are then discussed [S6.0(300)=25(-15)(+16) keV b] showing that this transition is likely the most important cascade contribution for 12C(alpha,gamma)16O.

The strength of the Ec.m. = 184 keV resonance in the 26gAl(p, gamma)27 reaction has been measured in inverse kinematics using the DRAGON recoil separator at TRIUMF's ISAC facility. We measure a value of omega gamma = 35 +/- 7 microeV and a resonance energy of Ec.m. = 184 +/- 1 keV, consistent with p-wave proton capture into the 7652(3) keV state in 27Si, and discuss the implications of these values for 26GAl nucleosynthesis in typical oxygen-neon white-dwarf novae.

The angular distribution of the reaction $^{6}\mathrm{Li}(d,\ensuremath{\alpha})^{4}\mathrm{He}$ at deuteron energies below $100\phantom{\rule{0.3em}{0ex}}\mathrm{keV}$ and the total cross section as well as the angular distribution of the reaction $^{10}\mathrm{B}(d,{p}_{0})^{11}\mathrm{B}$ at energies below $350\phantom{\rule{0.3em}{0ex}}\mathrm{keV}$ have been measured. Based on our experimental results and data of other authors, the reaction mechanism has been studied in a wide energy range, relevant for astrophysical applications. It has been found that in both cases broad resonances in the compound nuclei play the key role for the description of the excitation functions. The long-standing problems of describing the angular distributions could be solved for both reactions by assuming a coherent superposition between resonant and direct reaction amplitudes. A theoretical approach allowing for coherent calculations has been developed. Some astrophysical implications are discussed.

The reaction 6Li(d,α)4He has been measured for deuteron energies between 50 and 180 keV. In addition to the direct reaction component, which was calculated in the frame of the DWBA formalism, a significant contribution of a broad 2+ subthreshold resonance in the compound nucleus 8Be to the reaction cross section was identified. The results of the present analysis are compared with those obtained for the 6Li(d,p)7Li and 6Li(d,n)7Be reactions. Implications on the astrophysical S‐factor value at zero deuteron energy and on the electron screening potential are discussed.

The nuclide 44Ti is predicted to be produced in significant quantities in core-collapse supernovae, and indeed it has been observed in the supernova remnant Cassiopeia-A by space-based γ-ray telescopes. The main production of 44Ti takes place in the α-rich freeze-out phase deep inside the supernova. The key reactions governing the 44Ti abundance have been identified in an earlier sensitivity study. Using the recoil mass spectrometer DRAGON at the TRIUMF-ISAC facility in Vancouver, Canada, we measured the main production reaction 40Ca(α,γ)44Ti, resulting in an increased reaction rate compared to the rate derived from previous prompt γ-ray studies, which is commonly used in supernova models. The uncertainty of the 44Ti production is now dominated by the rate of reactions with short-lived nuclides around 44Ti, namely 45V(p,γ)46Cr, 44Ti(α,p)47V and 44Ti(α,γ)48Cr. The sensitivity of these reactions on the 44Ti production has been revisited.

Ruprecht H.-G. « Weltliteratur » vue du Mexique en 1826. In: Bulletin Hispanique, tome 73, n°3-4, 1971. pp. 307-318.