Solar model predictions of B and p-p neutrinos agree with the experimentally-determined fluxes (including oscillations): φ(pp)measured = (1.02±0.02±0.01)φ(pp)theory, and φ( B)measured = (0.88± 0.04±0.23)φ(B)theory, 1σ experimental and theoretical uncertainties, respectively. We use improved input data for nuclear fusion reactions, the equation of state, and the chemical composition of the Sun. ...

Nuclear reaction rates are a fundamental yet uncertain ingredient in stellar evolution models. The astrophysical S-factor pertaining to the initial proton-proton chain is at 1% level, which contributes systematic but generally unpropagated error of similar order theoretical ages stars. In this work, we study prospect improving measurement and other pp CNO cycle using helioseismology solar neutr...

The magnetic field dependence of CIDNP is presented for two reaction products of independently generated alkyl radicals. It is shown that nuclear spin relaxation of the products influences the intensity distributions within multiplets, and how this relaxation can be included in the calculation of CIDNP effects from the radical pair theory. Analysis of the experimental results supports the recen...

The states with triangular and linear chain configurations of three a-clusters in C12 are treated by the reaction matrix theory on the basis of a realistic nuclear force. Clustering dependence of G-matrix is found to be essential for clusterization. It also ·brings on a change of effective interaction between the two configurations, which has a role in reducing the excitation energy of the line...