Abstract:The excitation functions of the yield of protons emitted in the D(d,p)T reaction in Ti, Fe, Pd, PdO and Au were measured for bombarding energies between 2.5 and 10 keV. It was found that the reaction rate at lower energies varies greatly with the host materials. The most strongly enhanced DD reaction occurs in PdO. At E d ¼ 2:5 keV, it is enhanced by factor of fifty from the bare deuteron rate and the screening energy deduced from the excitation function amounts to 600 eV. An enhancement of this size cannot be… Show more
“…The electron screening in d(d,p)t was studied previously for deuterated metals, insulators, and semiconductors, i.e. 58 samples in total [2,3] (see also [4,5]). As compared to measurements performed with a gaseous D 2 target (U e = 25 eV [6]), a large screening was observed in the metals (of order U e = 300 eV), a e-mail: raiola@ep3.rub.de; for the LUNA Collaboration.…”
“…The electron screening in d(d,p)t was studied previously for deuterated metals, insulators, and semiconductors, i.e. 58 samples in total [2,3] (see also [4,5]). As compared to measurements performed with a gaseous D 2 target (U e = 25 eV [6]), a large screening was observed in the metals (of order U e = 300 eV), a e-mail: raiola@ep3.rub.de; for the LUNA Collaboration.…”
“…The measured values are however not compatible with the adiabatic estimate [8,9,10,11,12]. Dynamical calculations have been performed, but they obviously cannot explain the discrepancy as they include atomic excitations and ionizations which reduce the energy available for fusion.…”
Section: Nuclear Reactionsmentioning
confidence: 87%
“…This case has been studied in great detail experimentally, as one can control different charge states of the projectile+target system in the laboratory [8,9,10,11,12]. The experimental findings disagree systematically by a factor of two or more with theory.…”
We observe photons and neutrinos from stars. Based on these observations, complemented by measurements of cosmic rays energies and composition, we have been able to constrain several models for the Big Bang and for stellar evolution. But that is not enough. We also need to help this effort with laboratory experiments. We are still far from being able to reproduce stellar environments in a terrestrial laboratory. But in many cases we can obtain accurate nuclear reaction rates needed for modeling primordial nucleosynthesis and hydrostatic burning in stars. The relevant reactions are difficult to measure directly in the laboratory at the small astrophysical energies. In recent years indirect reaction methods have been developed and applied to extract low-energy astrophysical S-factors. These methods require a combination of new experimental techniques and theoretical efforts, which are the subject of this short review.
Abstract. Nuclear fusion cross-sections considerably higher than corresponding theoretical predictions are observed in low-energy experiments with metal matrix targets and accelerated deuteron beams. The cross-section increment is significantly higher for liquid than for solid targets. We propose that the same two-body correlation entropy used in evaluating the metal melting entropy explains the large liquid-solid difference of the effective screening potential that parameterizes the cross-section increment. This approach is applied to the specific case of the 6 Li(d, α) 4 He reaction, whose measured screening potential liquid-solid difference is (235 ± 63) eV. Cross sections in the two metals with the highest two-body correlation entropy (In and Hg) has not been measured yet: increments of the cross sections in liquid relative to the ones in solid metals are estimated with the same procedure.
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