PROTON-PROTON CYCLE

also called Proton-proton Reaction, chain of thermonuclear reactions that is the chief source of the energy radiated by the Sun and other cool main-sequence stars. Another sequence of thermonuclear reactions, called the carbon cycle, provides much of the energy released by hotter stars. In a proton-proton cycle, four hydrogen nuclei (protons) are combined to form one helium nucleus; 0.7 percent of the original mass is lost mainly by conversion into heat energy, but some energy escapes in the form of neutrinos (n). First, two hydrogen nuclei (1H) combine to form a hydrogen-2 nucleus (2H, deuterium) with the emission of a positive electron (e+, positron) and a neutrino (n). The hydrogen-2 nucleus then rapidly captures another proton to form a helium-3 nucleus (3He), while emitting a gamma ray (g). In symbols: From this point the reaction chain may follow any of several paths, but it always results in one helium-4 nucleus, with the emission of two neutrinos in total. The energy of the neutrinos emitted is different for the different paths. In the most direct continuation, two helium-3 nuclei (produced as indicated above) form one helium-4 nucleus (4He, alpha particle) with the release of two protons, The path that produces the most energetic neutrinos uses a helium-4 nucleus as a catalyst and cycles through beryllium and boron isotopes at intermediate states. In symbols: The latter path occurs only at relatively high temperatures and is of interest because such energetic neutrinos have been detected in a large-scale experiment in a deep mine. The detection rate in this solar-neutrino experiment is smaller than theoretically predicted; the cause for the discrepancy is as yet undetermined. Compare carbon cycle.