Key points are not available for this paper at this time.
Field-theoretic calculations of the cross sections for the photoneutrino process, +e^-e^-++, and the pair annihilation process, e^++e^-+, are performed in order to obtain the neutrino luminosity of very hot stars (T₂510^8^K). The energy loss rate which is obtained for the latter process is sufficient to determine the rate of evolution of the stellar core when T₂210^9^K.
Chiu et al. (Mon,) studied this question.