The basic nuclear reaction in the core of the Sun is the fusion of two protons, giving a deuterium, a positron and an electron-neutrino ν e. The final result has been published in 19 98. At the end of the 70’s, the solar neutrino deficit was better quantified: (0.39± 0.06) 37Ar were produced per day translated into 2.1☐.3 solar neutrino units and compared to 7.8☑.5 expected from solar models.
This is the start of the solar neutrino problem, which will be solved only in 2001. His first results, in 1968, were a big surprise: Davis observed less than 0.2 37Ar produced per day, much less than the prediction. Such a detector would observe few 37Cl to 37Ar conversion per day.
#Solar neutrino problem install
He proposed to install 390 000 liters of perchlorethylene (C 2Cl 4) in the Homestake Gold mine (South Dakota), deep underground to avoid cosmic rays interaction. Simultaneously, Ray Davis revived his chlorine-argon detector. In 1964, John Bahcall developed his first solar model and calculated that the chlorine-argon reaction would be the most promising method to observe solar neutrinos. This process is accompanied by the emission of neutrinos, which are the only witnesses of the phenomenon. Since the pioneering work of Bethe and others, it was anticipated that the energy of the Sun was produced in its core by the fusion of hydrogen into helium.
Nuclear Power Plants : Neutrinos or Anti-Neutrinos ?ĭavis neutrino detector at Homestake 1970.Energy non-conservation hypothesis for the beta decay spectrum.
0 kommentar(er)
