The theory of Feynman and Gell-Mann1 of weak interactions predicts an electron-neutrino interaction (ē ve) (v2 e) with the same coupling constant as that measured in β-decays. Owing to the lack of experimental verification of this prediction, a number of investigators have searched for possible astrophysical tests of the theory. The interaction cross-section of neutrinos with matter is very low and cosmic neutrinos are extremely difficult to detect directly. For this reason, however, they will escape unimpeded from stars and if produced in large quantities in stellar interiors, can have a marked effect on the total energy budget of some stars and consequently on their evolutionary time-scales. Ruderman2 and Chiu3 have discussed various aspects of this problem. Stothers4 has reviewed the relevant astrophysical data and concluded that so far all evidence confirms the existence of the interaction. He further concluded that g2=g2β × 10°±2, where gβ is the β-decay coupling constant.