TIME VARIATION OF SOLAR NEUTRINO FLUX

Abstract

Considering the solar neutrino data during the period from June, 1989 to April, 1992 within first sunspot maximum (it coincides with the maximum of the sunspot (Wolf numbers) and second sunspot maximum (usually appears 2–3 years after the first sunspot maximum) from the four solar neutrino experiments (37 Cl radiochemical, SAGE I & II, Gallex, Kamiokande II & III) we see that the average solar neutrino flux is much higher at the second sunspot maximum (May, 1991 to April, 1992) than at the first sunspot maximum (June, 1989 to April, 1991). This type of observation is already observed in the previous two solar activity cycles in 37 Cl solar neutrino experiment. It has been known for many years that first sunspot maximum and second sunspot maximum are essential features of the solar activity cycle. The above observation suggests that the solar neutrino flux data from the solar neutrino experiments appear to be varying with the solar activity cycle which suggests that the solar activity cycle is due to the pulsating character of the nuclear energy generation inside the core of the Sun.