The LIT method has allowed ab initio calculations of electroweak cross sections in light nuclear systems. This review presents a description of the method from both a general and a more technical point of view, as well as a summary of the results obtained by its application. The remarkable features of the LIT approach, which make it particularly efficient in dealing with a general reaction involving continuum states, are underlined. Emphasis is given on the results obtained for electroweak cross sections of few--nucleon systems. Their implications for the present understanding of microscopic nuclear dynamics are discussed.
The LIT approach is tested for the calculation of astrophysical S-factors. As an example the S-factor of the reaction 2H(p,gamma)3He is considered. It is discussed that a sufficiently high density of LIT states at low energies is necessary for a precise determination of S-factors. In particular it is shown that the hyperspherical basis is not very well suited for such a calculation and that a different basis system is much more advantageous. A comparison of LIT results with calculations, where continuum wave functions are explicitly used, shows that the LIT approach leads to reliable results. …
The maximum entropy method is examined as a new tool for solving the ill-posed inversion problem involved in the Lorentz integral transformation (LIT) method. As an example, we apply the method to the spin-dipole strength function of 4He. We show that the method can be successfully used for inversion of LIT, provided the LIT function is available with a sufficient accuracy.
Theoretical study of the ${}^{4}\rm{He}(γ,p)^3\rm{H}$ and ${}^{4}\rm{He}(γ,n)^3\rm{He}$ reactions
本文采用最新的核力，对反应$^{4}\rm{He}(γ,p)^3\rm{H}$和$^{4}\rm{He}(γ,n)^3\rm{He}$的总截面进行了{ \it Ab initio}计算。洛伦兹积分变换（LIT）的方法，它允许精确处理的最终状态相互作用（FSI）。采用有效相互作用超球谐函数（EIHH）方法求解动力学方程。在截面的计算中，除了在FSI跃迁矩阵元的LIT方程中的源项外，完全考虑了三核子力。
The accuracy of reconstruction of a response function from its Lorentz integral transform is studied in an exactly solvable model. An inversion procedure is elaborated in detail and features of the procedure are studied. Unlike results in the literature pertaining to the same model, the response function is reconstructed from its Lorentz integral transform with rather high accuracy.
The theoretical cross section calculations for the astrophysical $p$ process are needed because the most of the related reactions are technically very difficult to be measured in the laboratory. Even if the reaction was measured, most of the measured reactions have been carried out at the higher energy range from the astrophysical energies. Therefore, almost all cross sections needed for $p$ process simulation has to be theoretically calculated or extrapolated to the astrophysical energies. The $^{112}$Sn($α$,$γ$)$^{116}$Te is an important reaction for the $p$ process nucleosynthesis. The theo…
