Electro-weak reactions for astrophysics

The status of ''ab initio'' microscopic calculations of the 2H(p,γ)3He and 3He(p,e+νe)4He reactions is reviewed. The methods used to generate accurate nuclear ground- and scattering-state wave functions, and to construct realistic electro-weak transition operators are described. The uncertainties in the theoretical predictions, particularly those relevant to the p-3He weak capture, are discussed. For the dp radiative capture, the theoretical results are compared with the TUNL data in the energy range 0--100 keV