which, due to the charged-current contribution to scattering, has a relative sensitivity to s and heavy-flavor neutrinos of ~7:1. Since the direction of the recoil electron is constrained to be very forward, the direction of the neutrinos are kept in the direction of recoil electrons. Here, is provided where is the angle between the direction of recoil electrons and the Sun's position. This shows that the solar neutrino flux can be calculated to be . Comparing to the SSM, the ratio is . The result clearly indicates the deficit of solar neutrinos.
which, due to the charged-current contribution to scattering, has a relative sensitivity to s and heavy-flavor neutrinos of ~7:1. Since the direction of the recoil electron is constrained to be very forward, the direction of the neutrinos are kept in the direction of recoil electrons. Here, is provided where is the angle between the direction of recoil electrons and the Sun's position. This shows that the solar neutrino flux can be calculated to be . Comparing to the SSM, th.e ratio is . The result clearly indicates the deficit of solar neutrinos