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Using the records of the fluxes of solar neutrinos from the Homestake, GALLEX (GNO), and Super-Kamiokande experiments, their statistical analyses were performed to search for whether there existed a time variation of these fluxes. The results of the analysis for the three experiments indicate that these fluxes are varying quasi-biennially. This means that both efficiencies of the initial p-p and the pp-III reactions of the proton-proton chain are varying quasi-biennially together with a period of about 26 months. Since this time variation prospectively generated by these two reactions strongly suggests that the efficiency of the proton-proton chain as the main energy source of the Sun has a tendency to vary quasi-biennially due to some chaotic or non-linear process taking place inside the gravitationally stabilized solar fusion reactor. It should be, however, remarked that, at the present moment, we have no theoretical reasoning to resolve this mysterious result generally referred to as the quasi-biennial periodicity in the time variation of the fluxes of solar neutrinos. There is an urgent need to search for the reason why such a quasi-biennial periodicity is caused through some physical process as related to nuclear fusion deep inside the Sun.
Super-Kamiokande(SK) is a real-time detector capable of measuring the exact time of solar neutrino events. This, combined with a relatively high yield of these events of roughly 15 per day, allows a search for short-time variations in the observed fl
A search for day-night variations in the solar neutrino flux resulting from neutrino oscillations has been carried out using the 504 day sample of solar neutrino data obtained at Super-Kamiokande. The absence of a significant day-night variation has
We present a real-time supernova neutrino burst monitor at Super-Kamiokande (SK). Detecting supernova explosions by neutrinos in real time is crucial for giving a clear picture of the explosion mechanism. Since the neutrinos are expected to come earl
The results of the third phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first and second phase results. With improved detector calibrations, a full detector simulation, and improved analysis methods, the sy
Upgraded electronics, improved water system dynamics, better calibration and analysis techniques allowed Super-Kamiokande-IV to clearly observe very low-energy 8B solar neutrino interactions, with recoil electron kinetic energies as low as 3.49 MeV.